NASA/TP—2008–214171

Annular and Total Solar Eclipses of 2010

F. Espenak and J. Anderson

November 2008
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COVER CAPTION:

Map of annular and total solar eclipses of 2010.
National Aeronautics and 

Space Administration

Goddard Space Flight Center

Greenbelt, Maryland 20771

November 2008

NASA/TP—2008–214171

Annular and Total Solar Eclipses of 2010

F. Espenak

NASA Goddard Space Flight Center, Greenbelt, Maryland

J. Anderson

Royal Astronomical Society of Canada, Winnipeg, Manitoba
Available from:

NASA Center for AeroSpace Information National Technical Information Service

7115 Standard Drive 5285 Port Royal Road

Hanover, MD 21076-1320 Springfield, VA 22161
Reader's Note

While most NASA eclipse bulletins cover a single eclipse, this publication presents predictions for 

two solar eclipses during 2010. This has required a different organization of the material into the following sections.

Section 1—Eclipse Predictions: The section consists of a general discussion about the eclipse path 

maps, Besselian elements, shadow contacts, eclipse path tables, local circumstances tables, and the 

lunar limb profile.

Section 2—Annular Solar Eclipse of 2010 Jan 15: The section covers predictions and weather prospects 

for the annular eclipse.

Section 3—Total Solar Eclipse of 2010 Jul 11: The section covers predictions and weather prospects 

for the total eclipse.

Section 4—Observing Eclipses: The section provides information on eye safety, solar filters, eclipse 

photography, and making contact timings from the path limits.

Section 5—Eclipse Resources: The final section contains a number of resources including information 

on the IAU Working Group on Eclipses, the Solar Eclipse Mailing List, the NASA eclipse bulletins 

on the Internet, Web sites for the two 2010 eclipses, and a summary identifying the algorithms, ephemerides, and parameters used in the eclipse predictions.

Bold headers at the top of every page identify the section number and title for easy reference. This 

should help the reader to quickly navigate to any section.

Annular and Total Solar Eclipses of 2010 iii

Reader’s Note

Table of Contents

PREFACE. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .vii

1. ECLIPSE PREDICTIONS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1

1.1 Introduction. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1

1.2 Orthographic Projection Maps. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1

1.3 Equidistant Conic Projection Maps of the Eclipse Paths. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.4 Detailed Maps of the Eclipse Paths. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.5 Elements, Shadow Contacts, and Eclipse Path Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.6 Local Circumstances Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3

1.7 Mean Lunar Radius. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4

1.8 Lunar Limb Profile. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5

2. ANNULAR SOLAR ECLIPSE OF 2010 JAN 15. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7

2.1 Introduction. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7

2.2 Antumbral Path and Visibility. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7

2.3 Maps of the Annular Eclipse Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

2.4 Annular Eclipse Elements and Path Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

2.5 Annular Eclipse Local Circumstances Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

2.6 Annular Eclipse Lunar Limb Profile. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

2.7 Weather Prospects for the Annular Eclipse. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

3. TOTAL SOLAR ECLIPSE OF 2010 JUL 11. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43

3.1 Introduction. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43

3.2 Umbral Path and Visibility. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43

3.3 Maps of the Total Eclipse Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43

3.4 Total Eclipse Elements and Path Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44

3.5 Total Eclipse Local Circumstances Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44

3.6 Total Eclipse Lunar Limb Profile. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44

3.7 Weather Prospects for the Total Eclipse. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44

4. OBSERVING ECLIPSES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65

4.1 Eye Safety and Solar Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65

4.2 Sources for Solar Filters. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 67

4.3 Eclipse Photography. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 67

4.4 Contact Timings from the Path Limits. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68

4.5 Plotting Eclipse Paths on Maps. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 69

4.6 Eclipse Paths on Google Maps. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 69

5. ECLIPSE RESOURCES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.1 IAU Working Group on Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.2 IAU Solar Eclipse Education Committee. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.3 Solar Eclipse Mailing List. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.4 NASA Eclipse Bulletins on the Internet. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.5 Future Eclipse Paths on the Internet. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

5.6 NASA Web Site for 2010 Solar Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74

5.7 Predictions for Eclipse Experiments. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74

5.8 Algorithms, Ephemerides, and Parameters. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74

AUTHOR’S NOTE. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74

ACRONYMS and UNITS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 75

REFERENCES

Bibliography. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 75

Further Reading on Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 76

Further Reading on Eye Safety. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 77

Further Reading on Meteorology. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 77

Annular and Total Solar Eclipses of 2010 v

Table of Contents

Preface

This work is the thirteenth in a series of NASA publications containing detailed predictions, maps, and meteorological data for 

future total and annular solar eclipses of interest. Published as part of NASA’s Technical Publication (TP) series, the eclipse 

bulletins are prepared in cooperation with the Working Group on Eclipses of the International Astronomical Union and are 

provided as a public service to both the professional and lay communities, including educators and the media. In order to allow 

a reasonable lead time for planning purposes, eclipse bulletins are published 12 to 24 months before each event.

Single copies of the bulletins are available at no cost by sending a 9 × 12 inch self-addressed stamped envelope with postage 

for 12 oz. (340g). Detailed instructions and an order form can be found at the back of this publication.

The 2010 bulletin uses the World Data Bank II (WDBII) mapping database for the path figures. WDBII outline files were 

digitized from navigational charts to a scale of approximately 1:3,000,000. The database is available through the Global Relief 

Data CD-ROM from the National Geophysical Data Center. The highest detail eclipse maps are constructed from the Digital 

Chart of the World (DCW), a digital database of the world developed by the U.S. Defense Mapping Agency (DMA). The primary sources of information for the geographic database are the Operational Navigation Charts (ONC) and the Jet Navigation 

Charts (JNC). The eclipse path and DCW maps are plotted at a scale of 1:3,000,000 to 1:6,000,000 in order to show roads, cities, and villages, and lakes and rivers, making them suitable for eclipse expedition planning. Place names are from the World 

Gazetteer at <http://www.world-gazetteer.com/>.

The geographic coordinates database includes over 90,000 cities and locations. This permits the identification of many more 

cities within the umbral path and their subsequent inclusion in the local circumstances tables. Many of these locations are 

plotted in the path figures when the scale allows. The source of these coordinates is Rand McNally’s The New International 

Atlas. A subset of these coordinates is available in digital form, which has been augmented with population data.

The bulletins have undergone a great deal of change since their inception in 1993. The expansion of the mapping and geographic 

coordinates databases have improved the coverage and level of detail. This renders them suitable for the accuracy required 

by scientific eclipse expeditions. Some of these changes are the direct result of suggestions from the end user. Readers are 

encouraged to share comments and suggestions on how to improve the content and layout in subsequent editions. Although 

every effort is made to ensure that the bulletins are as accurate as possible, an error occasionally slips by. We would appreciate 

your assistance in reporting all errors, regardless of their magnitude.

We thank Dr. B. Ralph Chou for a comprehensive discussion on solar eclipse eye safety (Sect. 4.1). Dr. Chou is Professor of 

Optometry at the University of Waterloo with over 30 years of eclipse observing experience. As a leading authority on the 

subject, Dr. Chou’s contribution should help dispel much of the fear and misinformation about safe eclipse viewing.

The NASA Eclipse Web Site provides general information on every solar and lunar eclipse occurring during the period 1901 

through 2100. An online catalog also lists the date and basic characteristics of every solar and lunar eclipse from 2000 BCE 

through 3000 CE. The World Atlas of Solar Eclipses provides maps for every central solar eclipse path over the same fivemillennium period. The URL of the NASA Eclipse Web Site is <http://eclipse.gsfc.nasa.gov/>.

In addition to the synoptic data provided by the Web site above, special Web sites have been prepared for the annular and total 

solar eclipses of 2010. The URL of the annular eclipse Web site is <http://eclipse.gsfc.nasa.gov/SEmono/ASE2010/ASE2010.

html>. The URL of the total eclipse Web site is <http://eclipse.gsfc.nasa.gov/SEmono/TSE2010/TSE2010.html>. These Web 

sites include supplemental predictions, figures, and maps, which are not included in the present publication.

Because the eclipse bulletins have size limits, they cannot include everything needed by every scientific investigation. Some 

investigators may require exact contact times, which include lunar limb effects, or times for a specific observing site not listed in 

the bulletin. Other investigations may need customized predictions for an aerial rendezvous, or near the path limits for grazing 

eclipse experiments. We would like to assist such investigations by offering to calculate additional predictions for any professionals or large groups of amateurs. Please contact Fred Espenak with complete details and eclipse prediction requirements.

We would like to acknowledge the valued contributions of a number of individuals who were essential to the success of this 

publication. The format and content of the NASA eclipse bulletins has drawn heavily from over 40 years of eclipse Circulars

published by the U.S. Naval Observatory. We owe a debt of gratitude to past and present staff of that institution who performed 

this service for so many years. The numerous publications and algorithms of Dr. Jean Meeus have served to inspire a life-long 

interest in eclipse prediction. Prof. Jay M. Pasachoff reviewed the manuscript and offered many helpful suggestions. As Chair 

of the International Astronomical Union’s (IAU) Working Group on Eclipses, Prof. Pasachoff maintains a general Web site at 

Annular and Total Solar Eclipses of 2010 vii

Preface
<http://www.eclipses.info> that links to many eclipse related Web sites. Dr. David Dunham and Mr. Paul Maley reviewed and 

updated the information about eclipse contact timings. Ms. Elaine Firestone (Goddard Publications Senior Technical Editor) 

meticulously reviewed the manuscript. She was responsible for the editing, two-column page layout, and for ensuring that the 

bulletin conforms to NASA publication standards.

Permission is freely granted to reproduce any portion of this publication, including data, figures, maps, tables, and text. All 

uses and/or publication of this material should be accompanied by an appropriate acknowledgment (e.g., “Reprinted from 

NASA’s Annular and Total Solar Eclipses of 2010, Espenak and Anderson 2008”). We would appreciate receiving a copy of 

any publications where this material appears. 

The names and spellings of countries, cities, and other geopolitical regions are for identification purposes only. They are not 

authoritative, nor do they imply any official recognition in status by the United States Government. Corrections to names, 

geographic coordinates, and elevations are actively solicited in order to update the database for future bulletins. All calculations, diagrams, and opinions are those of the authors and they assume full responsibility for their accuracy.

Fred Espenak Jay Anderson

NASA Goddard Space Flight Center Royal Astronomical Society of Canada

Planetary Systems Laboratory, Code 693 189 Kingsway Ave.

Greenbelt, MD 20771 Winnipeg, MB 

USA CANADA R3M 0G4

E-mail: fred.espenak@nasa.gov E-mail: jander@cc.umanitoba.ca

 

NASA Solar Eclipse Bulletins

NASA Eclipse Bulletin RP # Publication Date

Annular Solar Eclipse of 1994 May 10 1301 April 1993

Total Solar Eclipse of 1994 November 3 1318 October 1993

Total Solar Eclipse of 1995 October 24 1344 July 1994

Total Solar Eclipse of 1997 March 9 1369 July 1995

Total Solar Eclipse of 1998 February 26 1383 April 1996

Total Solar Eclipse of 1999 August 11 1398 March 1997

NASA Eclipse Bulletin TP # Publication Date

Total Solar Eclipse of 2001 June 21 1999-209484 November 1999

Total Solar Eclipse of 2002 December 04 2001-209990 October 2001

Annular and Total Solar Eclipses of 2003 2002-211618 October 2002

Total Solar Eclipse of 2006 March 29 2004-212762 November 2004

Total Solar Eclipse of 2008 August 01 2007-214149 March 2007

Total Solar Eclipse of 2009 July 22 2008-214169 March 2008 

Annular and Total Solar Eclipses of 2010 2008-214171 November 2008

 viii Annular and Total Solar Eclipses of 2010

Preface
1. Eclipse Predictions

1.1 Introduction

During 2010, there are two major eclipses of the Sun. The 

first is an annular eclipse on January 15 (Section 2) and the 

second is a total eclipse on July 11 (Section 3). This section is 

a general description of the tables, maps, and figures appearing 

in the later sections for each eclipse.

For simplicity, the term “umbral” will be used when 

referring to either the “umbral” (total eclipse) or “antumbral” 

(annular eclipse) shadow or path. 

1.2 Orthographic Projection Maps

Figures 2.1 and 3.1 feature an orthographic projection map 

of Earth (adapted from Espenak 1987) for the annular (Jan 15) 

and total (Jul 11) eclipses, respectively. Each map shows the 

path of penumbral (partial eclipse) and umbral shadows (annular or total eclipse). The daylight terminator is plotted for 

the instant of greatest eclipse with north at the top. The map 

is centered over the point of greatest eclipse and is indicated 

with an asterisk symbol. The subsolar point (Sun in zenith) at 

that instant is also shown.

The limits of the Moon’s penumbral shadow define the 

region of visibility of the partial eclipse. This saddle-shaped 

region often covers more than half of Earth’s daylight hemisphere and consists of several distinct zones or limits. At 

the northern and/or southern boundaries lie the limits of the 

penumbra’s path. Partial eclipses have only one of these limits, 

as do umbral eclipses when the shadow axis falls no closer 

than about 0.45 radii from Earth’s center. Great loops at the 

western and eastern extremes of the penumbra’s path identify 

the areas where the eclipse begins and ends at sunrise and 

sunset, respectively. 

In the case of the 2010 annular eclipse (Figure 2.1), the 

penumbra has both a northern and southern limit, so that the 

rising and setting curves form two separate, closed loops. In 

comparison, the penumbral shadow of the 2010 total eclipse 

(Figures 3.1) has no southern limit; its southern edge falls off 

Earth so the southern penumbral path is bounded by Earth’s 

terminator.

Bisecting the “eclipse begins and ends at sunrise and sunset” loops is the curve of maximum eclipse at sunrise (western 

loop) and sunset (eastern loop). The exterior tangency points 

P1 and P4 mark the coordinates where the penumbral shadow 

first contacts (partial eclipse begins) and last contacts (partial 

eclipse ends) Earth’s surface. The path of the umbral shadow 

bisects the penumbral path from west to east.

A curve of maximum eclipse is the locus of all points 

where the eclipse is at maximum at a given time. They are 

plotted at each half hour in Universal Time, and generally run 

in a north-south direction. The outline of the umbral shadow 

is plotted every 15min in Universal Time. Curves of constant 

eclipse magnitude1 delineate the locus of all points where the 

1. Eclipse magnitude is defined as the fraction of the Sun’s diameter 

occulted by the Moon. It is strictly a ratio of diameters and should not 

magnitude at maximum eclipse is constant. These curves run 

exclusively between the curves of maximum eclipse at sunrise 

and sunset. Furthermore, they are quasi-parallel to the southern 

penumbral limit. This limit may be thought of as a curve of 

constant magnitude of 0.0, while the adjacent curves are for 

magnitudes of 0.2, 0.4, 0.6, and 0.8. The northern and southern limits of the path of total eclipse are curves of constant 

magnitude of 1.0.

At the top of Figures 2.1 and 3.1, the Universal Time of 

geocentric conjunction in ecliptic coordinates between the 

Moon and Sun is given (i.e., instant of New Moon) followed by 

the instant of greatest eclipse. The eclipse magnitude is given 

for greatest eclipse. It is equivalent to the topocentric ratio of 

diameters of the Moon and Sun. Gamma is the minimum distance of the Moon’s shadow axis from Earth’s center in units of 

equatorial Earth radii. Finally, the Saros series number of the 

eclipse is given along with its relative sequence in the series.

In the upper left and right corners are the geocentric coordinates of the Sun and Moon, respectively, at the instant of 

greatest eclipse. They are:

R.A.—Right Ascension

Dec.—Declination

S.D.—Apparent Semi-Diameter

H.P.—Horizontal Parallax

To the lower left are the exterior/interior contact times 

of the Moon’s penumbral shadow with Earth, which are defined:

P1—Instant of first exterior tangency of Penumbra with 

Earth’s limb. (Partial Eclipse Begins)

P2—Instant of first interior tangency of Penumbra with 

Earth’s limb.

P3—Instant of last interior tangency of Penumbra with 

Earth’s limb.

P4—Instant of last exterior tangency of Penumbra with 

Earth’s limb. (Partial Eclipse Ends)

Not all eclipses have P2 and P3 penumbral contacts. They 

are only present in cases where the penumbral shadow falls 

completely within Earth’s disk. For instance, the 2010 annular 

eclipse (Jan 15) has all four penumbral contacts, but the total 

eclipse (Jul 11) only has P1 and P4. The lower right corner lists 

exterior/interior contact times of the Moon’s umbral shadow 

with Earth’s limb which are defined as follows:

U1—Instant of first exterior tangency of Umbra with Earth’s 

limb. (Umbral [Total/Annular] Eclipse Begins)

U2—Instant of first interior tangency of Umbra with Earth’s 

limb.

U3—Instant of last interior tangency of Umbra with Earth’s 

limb.

U4—Instant of last exterior tangency of Umbra with Earth’s 

limb. (Umbral [Total/Annular] Eclipse Ends)

be confused with eclipse obscuration, which is a measure of the Sun’s 

surface area occulted by the Moon. Eclipse magnitude is usually expressed as a decimal fraction (e.g., 0.50 for 50%).

Annular and Total Solar Eclipses of 2010 1

Eclipse Predictions
At bottom center are the geographic coordinates of the 

position of greatest eclipse, along with the local circumstances 

at that location (i.e., Sun altitude, Sun azimuth, path width, 

and duration of totality/annularity). At bottom left are a list of 

parameters used in the eclipse predictions, while bottom right 

gives the Moon’s geocentric libration (optical + physical) at 

greatest eclipse.

1.3 Equidistant Conic Projection Maps of the 

Eclipse Paths

Figures 2.2 and 2.6 (Jan 15 annular) are maps that use an 

equidistant conic projection chosen to minimize distortion, 

and that isolate the land portions of the annular path. Curves 

of maximum eclipse are plotted and labeled at intervals of 

30min, while curves of constant eclipse magnitude appear 

at intervals of 0.1 magnitudes. A linear scale is included for 

estimating approximate distances (in kilometers). Within the 

northern and southern limits of the path of annularity, the outline of the antumbral shadow is plotted at intervals of 15min. 

The Universal Time, the duration of annularity (in minutes 

and seconds), and the Sun’s altitude are given at mid-eclipse 

for each shadow position.

1.4 Detailed Maps of the Eclipse Paths

The path of annularity or totality is plotted on a series of 

detailed maps appearing in Figures 2.3 to 2.5, 2.7 to 2.14 (Jan 15 

annular), and Figures 3.2 to 3.6 (Jul 11 total). The maps were 

chosen to isolate small regions of each eclipse path over the 

entire land portion of the tracks and to include ocean sections 

containing islands. Curves of maximum eclipse are plotted at 

5 min or shorter intervals along each path and labeled with 

the Universal Time, the central line duration of annularity or 

totality, and the Sun’s altitude. The maps are constructed from 

the Digital Chart of the World (DCW), a digital database of 

the world developed by the U.S. Defense Mapping Agency 

(DMA). The primary sources of information for the geographic 

database are the Operational Navigation Charts (ONC) and the 

Jet Navigation Charts (JNC) developed by the DMA.

The scale varies from map to map depending partly on 

the population density and accessibility. The scale is adequate 

for showing the roads, villages, and cities required for eclipse 

expedition planning. The DCW database used for the maps 

was developed in the 1980s and contains place names in use 

during that period. Whenever possible, the DCW place names 

have been replaced with current names in use from the World 

Gazetteer at <http://www.world-gazetteer.com/>.

While Tables 2.1 to 2.6 (Jan 15 annular) and Tables 3.1 to 

3.6 (Jul 11 total) deal with eclipse elements and specific characteristics of the path calculated at 5 min intervals, the northern 

and southern limits, as well as the central line of the path, are 

plotted using data generated at a higher cadence. These mapping data are available at the NASA Web sites for the 2010 annular eclipse <http://eclipse.gsfc.nasa.gov/SEmono/ASE2010/

ASE2010.html>, and the 2010 total eclipse <http://eclipse.gsfc.

nasa.gov/SEmono/TSE2010/TSE2010.html>.

Although no corrections have been made for center of 

figure or lunar limb profile, they have no observable effect 

at the scale of the maps. Atmospheric refraction has not been 

included, as it plays a significant role only at very low solar 

altitudes.. The primary effect of refraction is to shift the path 

opposite to that of the Sun’s local azimuth. This amounts to 

approximately 0.5° at the extreme ends, i.e., sunrise and sunset, 

of the umbral path. In any case, refraction corrections to the 

path are uncertain because they depend on the atmospheric 

temperature-pressure profile, which cannot be predicted 

in advance. A special feature of the maps are the curves of 

constant umbral (annular or total) eclipse duration which are 

plotted within the path at 1 or 2 min increments. These curves 

permit fast determination of approximate durations without 

consulting any tables.

Major highways are delineated in dark broad lines, but 

secondary and soft-surface roads are not distinguished, so 

caution should be used in this regard. If observations from the 

graze zones are planned, then the zones of grazing eclipse must 

be plotted on higher scale maps using graze path coordinates, 

which are available at the NASA Web sites for the 2010 annular eclipse <http://eclipse.gsfc.nasa.gov/SEmono/ASE2010/

ASE2010.html>, and the 2010 total eclipse <http://eclipse.gsfc.

nasa.gov/SEmono/TSE2010/TSE2010.html>. See Sect. 4.5 

“Plotting Eclipse Paths on Maps” for sources and more information. The paths also show the curves of maximum eclipse 

at 5min increments in Universal Time. The maps are also 

available at the NASA Web site for the 2010 solar eclipses.

1.5 Elements, Shadow Contacts, and Eclipse 

Path Tables

The geocentric ephemeris for the Sun and Moon, various 

parameters, constants, and the Besselian elements (polynomial 

form) are given in Tables 2.1 (Jan 15 annular) and 3.1 (Jul 11 

total). The eclipse elements and predictions were derived from 

the DE200 and LE200 ephemerides (solar and lunar, respectively) developed jointly by NASA’s Jet Propulsion Laboratory 

(JPL) and the U.S. Naval Observatory for use in the Astronomical Almanac beginning in 1984. Unless otherwise stated, all 

predictions are based on center of mass positions for the Moon 

and Sun with no corrections made for center of figure, lunar 

limb profile, or atmospheric refraction. The predictions depart 

from normal International Astronomical Union (IAU) convention through the use of a smaller constant for the mean lunar 

radius k for all umbral contacts (see Sect. 1.8 “Lunar Limb 

Profile”). Times are expressed in either Terrestrial Dynamical 

Time (TDT) or in Universal Time (UT), where the best value 

of ∆T (the difference between Terrestrial Dynamical Time and 

Universal Time) available at the time of preparation, is used.

The Besselian elements are used to predict all aspects 

and circumstances of a solar eclipse. The simplified geometry 

introduced by Bessel in 1824 transforms the orbital motions 

of the Sun and Moon into the position, motion, and size of 

the Moon’s penumbral and umbral shadows with respect to 

a plane passing through Earth. This fundamental plane is 

constructed in an x–y rectangular coordinate system with its 

 2 Annular and Total Solar Eclipses of 2010

Eclipse Predictions
origin at Earth’s center. The axes are oriented with north in 

the positive y direction and east in the positive x direction. The 

z-axis is perpendicular to the fundamental plane and parallel 

to the shadow axis. 

The x and y coordinates of the shadow axis are expressed 

in units of the equatorial radius of Earth. The radii of the 

penumbral and umbral shadows on the fundamental plane are 

l1 and l2 , respectively. The direction of the shadow axis on the 

celestial sphere is defined by its declination d and ephemeris 

hour angle μ. Finally, the angles that the penumbral and umbral 

shadow cones make with the shadow axis are expressed as f

1

and f2, respectively. The details of actual eclipse calculations 

can be found in the Explanatory Supplement (Her Majesty’s 

Nautical Almanac Office 1974) and Elements of Solar Eclipses 

(Meeus 1989).

From the polynomial form of the Besselian elements, any 

element can be evaluated for any time t1 (in decimal hours) 

during the eclipse via the equation

 a = a0 + a1 t + a2 t 

2

 + a3 t 

3 (1)

 (or a = ∑ [an t 

n

]; n = 0 to 3),

where a = x, y , d, l1 , l2 , or μ; and t = t1 – t0 (decimal hours) and t0

= 7.00 TDT (Jan 15 annular) or t0 = 20.00 TDT (Jul 11 total).

The polynomial Besselian elements were derived from 

a least-squares fit to elements rigorously calculated at five 

separate times over a 6 h period centered at t0.

Tables 2.2 (Jan 15 annular) and 3.2 (Jul 11 total) lists all external and internal contacts of penumbral and umbral shadows 

with Earth. They include TDT and geodetic coordinates with 

and without corrections for ∆T. The contacts are defined: 

P1—Instant of first external tangency of penumbral shadow 

cone with Earth’s limb (partial eclipse begins).

P2—Instant of first internal tangency of penumbral shadow 

cone with Earth’s limb.

P3—Instant of last internal tangency of penumbral shadow 

cone with Earth’s limb.

P4—Instant of last external tangency of penumbral shadow 

cone with Earth’s limb (partial eclipse ends).

U1—Instant of first external tangency of umbral shadow cone 

with Earth’s limb (annular or total eclipse begins).

U2—Instant of first internal tangency of umbral shadow cone 

with Earth’s limb.

U3—Instant of last internal tangency of umbral shadow cone 

with Earth’s limb.

U4—Instant of last external tangency of umbral shadow cone 

with Earth’s limb (annular or total eclipse ends).

Similarly, the northern and southern extremes of the penumbral and umbral paths, and extreme limits of the central line 

are given. The IAU longitude convention is used throughout 

this publication (i.e., for longitude, east is positive and west is 

negative; for latitude, north is positive and south is negative).

The path of the umbral shadow is delineated at 5min intervals (in Universal Time) in Tables 2.3 and 3.3. Coordinates 

of the northern limit, the southern limit, and the central line 

are listed to the nearest tenth of an arc minute (~185m at the 

equator). The Sun’s altitude, path width, and duration are calculated for the central line position. Tables 2.4 and 3.4 present 

a physical ephemeris for the umbral shadow at 5min intervals 

in Universal Time. The central line coordinates are followed 

by the topocentric ratio of the apparent diameters of the Moon 

and Sun, the eclipse obscuration (defined as the fraction of the 

Sun’s surface area occulted by the Moon), and the Sun’s altitude 

and azimuth at that instant. The umbral path width, the umbral 

shadow’s major and minor axes, and its instantaneous velocity 

with respect to Earth’s surface are included. Finally, the central 

line duration of the annular or total phase is given.

Local circumstances for each central line position, listed 

in Tables 2.3 and 3.3, are presented in Tables 2.5 and 3.5, 

respectively. The first three columns give the Universal Time 

of maximum eclipse, the central line duration of annularity or 

totality, and the altitude of the Sun at that instant. The following 

columns list each of the four eclipse contact times followed 

by their related contact position angles and the corresponding 

altitude of the Sun. The four contacts identify significant stages 

in the progress of the eclipse. They are defined as follows:

First Contact: Instant of first external tangency between the 

Moon and Sun (partial eclipse begins).

Second Contact: Instant of first internal tangency between 

the Moon and Sun (annular or total eclipse begins).

Third Contact: Instant of last internal tangency between the 

Moon and Sun (annular or total eclipse ends).

Fourth Contact: Instant of last external tangency between 

the Moon and Sun (partial eclipse ends).

The position angles P and V (where P is defined as the 

contact angle measured counterclockwise from the equatorial 

north point of the Sun’s disk, and V is defined as the contact 

angle measured counterclockwise from the local zenith point 

of the Sun’s disk) identify the point along the Sun’s disk where 

each contact occurs. Second and third contact altitudes are 

omitted because they are always within 1° of the altitude at 

maximum eclipse.

Tables 2.6 and 3.6 present topocentric values from the 

umbral path at maximum eclipse for the Moon’s horizontal 

parallax, semi-diameter, relative angular velocity with respect 

to the Sun, and libration in longitude. The altitude and azimuth 

of the Sun are given along with the azimuth of the umbral 

path. The northern limit position angle identifies the point on 

the lunar disk defining the umbral path’s northern limit. It is 

measured counterclockwise from the equatorial north point 

of the Moon. In addition, corrections to the path limits due 

to the lunar limb profile are listed (minutes of arc in latitude). 

The irregular profile of the Moon results in a zone of “grazing eclipse” at each limit, which is delineated by interior and 

exterior contacts of lunar features with the Sun’s limb. 

1.6 Local Circumstances Tables

Local circumstances for several hundred cities; metropolitan areas, and places are presented in Tables 2.7 to 2.15 (Jan 

15 annular), and Table 3.7 (Jul 11 total). The tables give the 

local circumstances at each contact and at maximum eclipse 

for every location. (For partial eclipses, maximum eclipse is 

Annular and Total Solar Eclipses of 2010 3

Eclipse Predictions
the instant when the greatest fraction of the Sun’s diameter is 

occulted. For annular and total eclipses, maximum eclipse is 

the instant of mid-annularity or mid-totality.) The coordinates 

are listed along with the location’s elevation (in meters) above 

sea level, if known. If the elevation is unknown (i.e., not in the 

database), then the local circumstances for that location are 

calculated at sea level. The elevation does not play a significant 

role in the predictions unless the location is near the umbral 

path limits or the Sun’s altitude is relatively small (<10°). 

The Universal Time of each contact is given to a tenth of a 

second, along with position angles P and V and the altitude of 

the Sun. The position angles identify the point along the Sun’s 

disk where each contact occurs and are measured counterclockwise (i.e., eastward) from the north and zenith points, respectively. Locations outside the umbral path miss the annular or 

total eclipse and only witness first and fourth contacts. The 

Universal Time of maximum eclipse (either partial or total) is 

listed to a tenth of a second. Next, the position angles P and V

of the Moon’s disk with respect to the Sun are given, followed 

by the altitude and azimuth of the Sun at maximum eclipse. 

Finally, the corresponding eclipse magnitude and obscuration 

are listed. For umbral eclipses (both annular and total), the 

eclipse magnitude is identical to the topocentric ratio of the 

Moon’s and Sun’s apparent diameters. 

Two additional columns are included if the location lies 

within the path of the Moon’s umbral shadow. The “umbral 

depth” is a relative measure of a location’s position with respect 

to the central line and path limits. It is a unit less parameter, 

which is defined as

 u = 1 – (2 x/W), (2)

where:

u is the umbral depth, 

x is the perpendicular distance from the central line in 

kilometers, and 

W is the width of the path in kilometers.

The umbral depth for a location varies from 0.0 to 1.0. A 

position at the path limits corresponds to a value of 0.0, while 

a position on the central line has a value of 1.0. The parameter 

can be used to quickly determine the corresponding central line 

duration; thus, it is a useful tool for evaluating the trade-off 

in duration of a location’s position relative to the central line. 

Using the location’s duration and umbral depth, the central 

line duration is calculated as 

 D = d /[1 – (1 – u)2]1/2, (3)

where:

D is the duration of annularity or totality on the central 

line (in seconds), 

d is the duration of annularity or totality at location (in 

seconds), and 

u is the umbral depth. 

The final column gives the duration of annularity or totality. The effects of refraction have not been included in these 

calculations, nor have there been any corrections for center of 

figure or the lunar limb profile. 

Locations were chosen based on general geographic distribution, population, and proximity to the path. The primary 

source for geographic coordinates is The New International Atlas (Rand McNally 1991). Elevations for major cities were taken 

from Climates of the World (U.S. Dept. of Commerce, 1972). 

In this rapidly changing political world, it is often difficult to 

ascertain the correct name or spelling for a given location; 

therefore, the information presented here is for location purposes only and is not meant to be authoritative. Furthermore, 

it does not imply recognition of status of any location by the 

United States Government. Corrections to names, spellings, 

coordinates, and elevations should be forwarded to the authors 

in order to update the geographic database for future eclipse 

predictions.

1.7 Mean Lunar Radius

A fundamental parameter used in eclipse predictions is 

the Moon’s radius k, expressed in units of Earth’s equatorial radius. The Moon’s actual radius varies as a function of 

position angle and libration because of the irregularity in the 

limb profile. From 1968 to 1980, the Nautical Almanac Office 

used two separate values for k in their predictions. The larger 

value (k=0.2724880), representing a mean over topographic 

features, was used for all penumbral (exterior) contacts and for 

annular eclipses. A smaller value (k=0.272281), representing 

a mean minimum radius, was reserved exclusively for umbral 

(interior) contact calculations of total eclipses (Explanatory 

Supplement, Her Majesty’s Nautical Almanac Office, 1974). 

Unfortunately, the use of two different values of k for umbral eclipses introduces a discontinuity in the case of hybrid

(annular-total) eclipses.

In 1982, the IAU General Assembly adopted a value of 

k=0.2725076 for the mean lunar radius. This value is now used 

by the Nautical Almanac Office for all solar eclipse predictions 

(Fiala and Lukac 1983) and is currently accepted as the best 

mean radius, averaging mountain peaks and low valleys along 

the Moon’s rugged limb. The adoption of one single value for k

eliminates the discontinuity in the case of hybrid eclipses and 

ends confusion arising from the use of two different values; 

however, the use of even the “best” mean value for the Moon’s 

radius introduces a problem in predicting the true character and 

duration of umbral eclipses, particularly total eclipses. 

During a total eclipse, the Sun’s disk is completely 

occulted by the Moon. This cannot occur so long as any 

photospheric rays are visible through deep valleys along the 

Moon’s limb (Meeus et al. 1966). The use of the IAU’s mean 

k, however, guarantees that some annular or hybrid eclipses 

will be misidentified as total. A case in point is the eclipse of 

1986 October 03. Using the IAU value for k, the Astronomical 

Almanac identified this event as a total eclipse of 3 s duration 

when it was, in fact, a beaded annular eclipse. Because a 

smaller value of k is more representative of the deeper lunar 

 4 Annular and Total Solar Eclipses of 2010

Eclipse Predictions
valleys and hence, the minimum solid disk radius, it helps 

ensure an eclipse’s correct classification.

Of primary interest to most observers are the times when 

an umbral eclipse begins and when it ends (second and third 

contacts, respectively), and the duration of the umbral phase. 

When the IAU’s value for k is used to calculate these times, they 

must be corrected to accommodate low valleys (total) or high 

mountains (annular) along the Moon’s limb. The calculation 

of these corrections is not trivial, but is necessary, especially 

if one plans to observe near the path limits (Herald 1983). For 

observers near the central line of a total eclipse, the limb corrections can be more closely approximated by using a smaller 

value of k, which accounts for the valleys along the profile.

This publication uses the IAU’s accepted value of 

k=0.2725076 for all penumbral (exterior) contacts. In order to 

avoid eclipse type misidentification and to predict umbral durations, which are closer to the actual durations at total eclipses, 

this document departs from IAU convention by adopting the 

smaller value of k=0.272281 for all umbral (interior) contacts. 

This is consistent with predictions in Fifty Year Canon of 

Solar Eclipses: 1986–2035 (Espenak 1987) and Five Millennium Canon of Solar Eclipses: –1999 to +3000 (Espenak and 

Meeus 2006). Consequently, the smaller k value produces 

shorter umbral durations and narrower paths for total eclipses 

when compared with calculations using the IAU value for k. 

Similarly, predictions using a smaller k value results in longer 

umbral durations and wider paths for annular eclipses than do 

predictions using the IAU’s k value.

1.8 Lunar Limb Profile

Eclipse contact times, magnitude, and duration of annularity or totality all depend on the angular diameters and 

relative velocities of the Moon and Sun. Unfortunately, these 

calculations are limited in accuracy by the departure of the 

Moon’s limb from a perfectly circular figure. The Moon’s 

surface exhibits a dramatic topography, which manifests itself 

as an irregular limb when seen in profile. Most eclipse calculations assume some mean radius that averages high mountain 

peaks and low valleys along the Moon’s rugged limb. Such an 

approximation is acceptable for many applications, but when 

higher accuracy is needed, the Moon’s actual limb profile must 

be considered. Fortunately, an extensive body of knowledge 

exists on this subject in the form of Watts’s limb charts (Watts 

1963). These data are the product of a photographic survey of 

the marginal zone of the Moon and give limb profile heights 

with respect to an adopted smooth reference surface (or

datum). 

Analyses of lunar occultations of stars by Van Flandern 

(1970) and Morrison (1979) showed that the average cross section of Watts’s datum is slightly elliptical rather than circular. 

Furthermore, the implicit center of the datum (i.e., the center 

of figure) is displaced from the Moon’s center of mass. 

In a follow-up analysis of 66,000 occultations, Morrison 

and Appleby (1981) found that the radius of the datum appears 

to vary with libration. These variations produce systematic errors in Watts’s original limb profile heights that attain 0.4arcsec 

at some position angles, thus, corrections to Watts’s limb data 

are necessary to ensure that the reference datum is a sphere 

with its center at the center of mass.

The Watts charts were digitized by Her Majesty’s Nautical 

Almanac Office (then in Herstmonceux, England), and transformed to grid-profile format at the U.S. Naval Observatory. 

In this computer readable form, the Watts limb charts lend 

themselves to the generation of limb profiles for any lunar 

libration. Ellipticity and libration corrections may be applied 

to refer the profile to the Moon’s center of mass. Such a profile 

can then be used to correct eclipse predictions, which have 

been generated using a mean lunar limb.

Figures 2.15 and 3.7 give the limb profiles for the 2010 

annular and total eclipses, respectively, for single location and 

time. The radial scale of the limb profiles (at bottom of each 

figure) is greatly exaggerated so that the true limb’s departure 

from the mean lunar limb is readily apparent. The mean limb 

with respect to the center of figure of Watts’s original data is 

shown (dashed curve) along with the mean limb with respect 

to the center of mass (solid curve). Note that all the predictions 

presented in this publication are calculated with respect to the 

latter limb unless otherwise noted. Position angles of various 

lunar features can be read using the protractor marks along 

the Moon’s mean limb (center of mass). The position angles of 

second and third contact are clearly marked, as are the north 

pole of the Moon’s axis of rotation and the observer’s zenith 

at mid-totality. The dashed line with arrows at either end 

identifies the contact points on the limb corresponding to the 

northern and southern limits of the path. To the upper left of 

the profile, are the Sun’s topocentric coordinates at maximum 

eclipse. They include the right ascension (R.A.), declination 

(Dec.), semi-diameter (S.D.), and horizontal parallax (H.P.) The 

corresponding topocentric coordinates for the Moon are to the 

upper right. Below and left of the profile are the geographic 

coordinates of the central line at selected locations, while the 

times of the four eclipse contacts at each location appear to 

the lower right. The limb-corrected times of second and third 

contacts are listed with the applied correction to the center of 

mass prediction.

Directly below the limb profile are the local circumstances 

at maximum eclipse. They include the Sun’s altitude and azimuth, the path width, and umbral duration. The position angle 

of the path’s northern-to-southern limit axis is PA(N.Limit)

and the angular velocity of the Moon with respect to the Sun 

is A.Vel.(M:S). At the bottom left are a number of parameters 

used in the predictions, and the topocentric lunar librations 

appear at the lower right.

In investigations where accurate contact times are needed, 

the lunar limb profile can be used to correct the nominal or 

mean limb predictions. For any given position angle, there will 

be a high mountain (annular eclipses) or a low valley (total 

eclipses) in the vicinity that ultimately determines the true 

instant of contact. The difference, in time, between the Sun’s 

position when tangent to the contact point on the mean limb 

and tangent to the highest mountain (annular) or lowest valley 

(total) at actual contact is the desired correction to the predicted 

contact time. On the exaggerated radial scale of Figures 2.15 

Annular and Total Solar Eclipses of 2010 5

Eclipse Predictions
and 3.7, the Sun’s limb can be represented as an epicyclic curve 

that is tangent to the mean lunar limb at the point of contact 

and departs from the limb by h through

 h = S (m–1) (1–cos[C]), (9)

where: 

h is the departure of Sun’s limb from mean lunar limb, 

S is the Sun’s semi-diameter, 

m is the eclipse magnitude, and 

C is the angle from the point of contact.

Herald (1983) takes advantage of this geometry in developing a graphic procedure for estimating correction times over a 

range of position angles. Briefly, a displacement curve of the 

Sun’s limb is constructed on a transparent overlay by way of 

equation (9). For a given position angle, the solar limb overlay 

is moved radially from the mean lunar limb contact point until 

it is tangent to the lowest lunar profile feature in the vicinity. 

The solar limb’s distance d (in arc seconds) from the mean 

lunar limb is then converted to a time correction δ by

 δ = d/v cos[X – C], (10)

where: 

δ is the correction to contact time (in seconds), 

d is the distance of solar limb from Moon’s mean limb (in 

arc seconds), 

v is the angular velocity of the Moon with respect to the 

Sun (arc seconds per second), 

X is the central line position angle of the contact, and 

C is the angle from the point of contact.

This operation may be used for predicting the formation and 

location of Baily’s beads. When calculations are performed 

over a large range of position angles, a contact time correction 

curve can then be constructed.

Because the limb profile data are available in digital 

form, an analytical solution to the problem is possible that is 

quite straightforward and robust. Curves of corrections to the 

times of second and third contact for most position angles have 

been computer generated and are plotted in Figures 2.15 and 

3.7. The circular protractor scale at the center represents the 

nominal contact time using a mean lunar limb. The departure 

of the contact correction curves from this scale graphically 

illustrates the time correction to the mean predictions for any 

position angle as a result of the Moon’s true limb profile. Time 

corrections external to the circular scale are added to the mean 

contact time; time corrections internal to the protractor are 

subtracted from the mean contact time. The magnitude of the 

time correction at a given position angle is measured using any 

of the four radial scales plotted at each cardinal point.

 6 Annular and Total Solar Eclipses of 2010

Eclipse Predictions
2. Annular Solar Eclipse of 2010 Jan 15

2.1 Introduction

On Friday, 2010 January 15, an annular eclipse of the Sun 

is visible from within a 300 km wide track that traverses half 

of Earth. The path of the Moon’s antumbral shadow begins in 

Africa and passes through Chad, Central African Republic, 

Democratic Republic of the Congo, Uganda, Kenya, and Somalia. After leaving Africa, the path crosses the Indian Ocean 

where the maximum duration of annularity reaches 11 min 

08 s (Espenak 1987). The central path then continues into Asia 

through Bangladesh, India, Burma (Myanmar), and China. 

A partial eclipse is seen within the much broader path of the 

Moon’s penumbral shadow, which includes eastern Europe, 

most of Africa, Asia, and Indonesia (Figure 2.1).

2.2 Antumbral Path and Visibility

Earth reaches perihelion on Jan 03, just 12 days before 

the annular eclipse, so the Sun is nearly at its maximum apparent diameter. The Moon passes through apogee on Jan 17 

(01:41 UT) so it is close to its minimum apparent diameter 

during the eclipse. The combination of these factors results 

in an unusually wide path of annularity.

The track of the Moon’s shadow begins in western-most 

Central African Republic (Figure 2.2) at 05:14 UT. The eclipse 

path is 371 km wide at its start as the antumbra quickly travels 

east-southeast.

The northern edge of the path begins in southern Chad 

(Figure 2.3), but quickly crosses into the Central African 

Republic (CAR). Bangui, the capital of, and the largest city 

in, the CAR, lies 150 km south of the central line. Its 500,000 

inhabitants witness a 4 min 0 s annular eclipse with the Sun 

just 4° above the eastern horizon at 05:17 UT. To the north, 

the duration on the central line is 7 min 18 s. At this instant, 

the enormous antumbral shadow is racing across the African 

continent with a velocity exceeding 10 km/s, but its speed is 

dropping fast. 

When the central line crosses into the Democratic Republic of the Congo (DRC) at 05:19 UT, the duration hits 

7 min 30 s and the Sun’s altitude is 8°. DRC’s capital city, 

Kisangani, is 115 km south of the southern limit (Figure 2.4). 

Its population of more than 7 million must be content with a 

partial eclipse of 0.88.

Continuing eastward, the shadow enters Uganda and 

engulfs Lake Albert and Kabarega National Park (05:23 UT). 

The central line duration now tops 8 min, the Sun stands 17° 

above the horizon, and the antumbral velocity is 2.3 km/s. 

Uganda’s capital, Kampala, with a population of 1.2 million, 

is 60 km south of the central line but still deep in the annular 

path. The central phase of the eclipse lasts 7 min 36 s in Kampala, while the central line duration is 8 min 12 s. The northern 

half of Lake Victoria, Africa’s largest lake, also extends into 

the antumbral track.

At 05:27 UT, the central line exits Uganda and enters Kenya (Figure 2.5). Many of Kenya’s national parks and wildlife 

reserves fall within the annular path including Mt. Elgon, Keno 

Valley, Samburu, Mt. Kenya, Lake Nakuru, Meru, Kora, and 

Tsavo East. The southern edge of the path bisects Masai Mara 

Game Reserve. Nairobi, Kenya’s capital of 2.9 million people, 

stands within 100 km of the central line and experiences 6 min 

54 s of annularity. Due north of Nairobi on the central line, 

the duration is 8 min 32 s, the Sun is 25° above the horizon, 

and the antumbral velocity is 1.5 km/s (05:30 UT). The long 

duration implies that the Moon appears considerably smaller 

than the Sun. Indeed, the lunar diameter is only 0.912 of the 

Sun’s disk, obscuring just 0.832 of the Sun’s surface area. 

Most people will not even be aware of any local darkening at 

maximum eclipse unless it is pointed out.

The Moon’s shadow continues through Kenya as its northern half briefly enters southernmost Somalia. As the central 

line exits Kenya and heads across the Indian Ocean (05:37 UT), 

its annular duration is 1 s shy of 9 min. For the next 2 h, the 

antumbra crosses the Indian Ocean, its course slowly curving 

from east-southeast to northeast. The Seychelles lie just outside 

of the track and get a deep partial eclipse of magnitude 0.907 

at 06:09 UT.

The instant of greatest eclipse occurs at 07:06:33 UT 

(latitude 01° 37′N, longitude 69° 17′E) when the axis of the 

Moon’s shadow passes closest to the center of Earth (gamma1 = 

+0.40016). The maximum duration of annularity here is 11 min 

08 s, the Sun’s altitude is 66°, the path width is 333 km, and the 

antumbra’s velocity is 0.46 km/s. Although the Moon’s relative diameter to the Sun (0.919) is slightly larger than it was in 

Kenya, its relative motion is considerably smaller due in larger 

part to Earth’s rotation along with the antumbral, making the 

central duration several minutes longer. This is, in fact, the 

longest annular eclipse of the 3rd Millennium—its duration 

will not be exceeded until the year 3043.

Although the eclipse is half over, it must now traverse 

southern Asia before reaching its terminus (Figure 2.6). The 

next landfall occurs at about 07:26 UT when the shadow sweeps 

over the Maldive Islands (Figure 2.7). The capital city of Malé is 

just 22 km from the central line so it experiences a long annular 

duration of 10 min 45 s. This is the longest duration of any city 

having an international airport in the eclipse track.

The path finally reaches Asia as the central line passes 

directly between the southern tip of India and northern Sri 

Lanka. Both regions lie within the path (Figure 2.8) although 

Sri Lanka’s capital city Colombo (pop. 640,000) is outside 

the southern limit and receives a partial eclipse of magnitude 

0.902 at 07:49 UT.

Leaving the Indian subcontinent, the antumbra crosses 

the Bay of Bengal before its central axis reaches the southwest 

coast of Burma (Myanmar) at 08:33 UT (Figure 2.9). The central line duration is 08 m 47 s, the solar altitude is 34°, the path 

width is 834 km, and the velocity is 1.1 km/s. The northern 

edge of the shadow briefly enters Bangladesh and southeastern 

1 Gamma is the perpendicular distance of the Moon’s shadow axis 

from Earth’s center in units of equatorial Earth radii. It is measured 

when the distance to the geocenter reaches a minimum (i.e., instant of 

greatest eclipse).

Annular and Total Solar Eclipses of 2010 7

 Annular Solar Eclipse of 2010 January 15
India before returning completely into Burma. Mandalay is 

75 km south of the central line where its 0.9 million inhabitants 

experience a 7 min 35 s annular phase centered at 08:38 UT.

At 08:41 UT, the antumbra’s central line enters China, the 

largest and final country in the track. The shadow crosses the 

southern foot of the Himalayas through Yunnan and Sichuan 

provinces (Figures 2.10 and 2.11). Chongqing (urban population 2.2 million) is the largest and most populous of China’s 

four provincial-level municipalities. It lies directly on the 

central line where the duration is 7 min 50 s and the Sun’s 

altitude is 15°. 

As the curvature of Earth brings the planet’s surface farther from the Moon and at an increasingly oblique angle, the 

duration of annularity and the Sun’s altitude decrease, while 

the antumbra’s ground velocity increases. Racing through parts 

of Shaanxi, and Hubei provinces (Figures 2.12 and 2.13), the 

northern antumbra engulfs Zhenzhou, the capital city of Henan 

province. The Sun is 7° during a 4 min 30 s annular phase. On 

the central line 145 km to the southeast, the duration is still 

7 min 27 s while the shadow’s velocity is 6.6 km/s.

In its final moments, the antumbra enters Shandong province and the lower reaches of the Yellow River (Figure 2.14). 

The track travels down the Shandong Peninsula where it ends 

as the Moon’s shadow lifts off Earth (08:59 UT). During the 

course of its 3 h 45 min trajectory, the antumbra’s track is approximately 12,900 km long, which covers 0.87% of Earth’s 

surface area. It will be 29 months before the next annular solar 

eclipse occurs on 2012 May 20.

2.3 Maps of the Annular Eclipse Path

Maps of the Jan 15 annular eclipse path are given in Figures 2.1 through 2.14. Figure 2.1 is an orthographic projection 

map of Earth showing the path of penumbral (partial) and antumbral (annular) eclipse. The limits of the Moon’s penumbral 

shadow define the region of visibility of the partial eclipse. 

The much narrower path of the antumbral shadow defines the 

zone where the annular eclipse is visible. For a more detailed 

description of Figure 3.1, see Section 1.2.

Figures 2.2 through 2.14 offer more detailed maps of the 

entire land portion of the path of annularity, as well as ocean 

sections of the track containing islands. A complete description 

of these figures can be found in Sections 1.3 and 1.4.

2.4 Annular Eclipse Elements and Path Tables

Tables 2.1 through 2.7 give elements for the eclipse, as 

well as basic characteristics of the annular path. The geocentric ephemeris for the Sun and Moon, various parameters, 

constants, and the Besselian elements (polynomial form) are 

found in Table 2.1. All external and internal contacts of penumbral and antumbral shadows with Earth are listed in Table 

2.2. They include TDT and geodetic coordinates with and 

without corrections for ∆T.

The path of the antumbral shadow is delineated at 5 min 

intervals (in Universal Time) in Table 2.3. Coordinates of the 

northern limit, the southern limit, and the central line are listed 

along with the Sun’s altitude, path width, and central line duration of annularity. Table 2.4 presents a physical ephemeris for 

the antumbral shadow and includes the topocentric ratio of the 

Moon’s and Sun’s apparent diameters, the eclipse obscuration, 

the path width, the dimensions of the antumbral shadow, and 

its ground velocity.

Table 2.5 gives the local circumstances for each central 

line position listed in Tables 2.3 and 2.4. Table 2.6 presents 

topocentric values from the central path for the Moon’s horizontal parallax, semi-diameter, relative angular velocity with 

respect to the Sun, and libration in longitude. In addition, 

corrections to the path limits due to the lunar limb profile are 

listed. A detailed description of these tables can be found in 

Section 1.5.

2.5 Annular Eclipse Local Circumstances Tables

Local circumstances for many cities, metropolitan areas, 

and places in Africa, Europe, the Middle East, and Asia are 

presented in Tables 2.7 to 2.15. The tables give the local circumstances at each contact and at maximum eclipse for every 

location. The coordinates are listed along with the location’s 

elevation (in meters) above sea level. The Universal Time of 

each contact is given to a tenth of a second, along with position angles P and V and the altitude of the Sun. Two additional 

columns are included if the location lies within the path of the 

Moon’s antumbral shadow. The “umbral depth” is a relative 

measure of a location’s position with respect to the central line 

and path limits. The last column gives the duration of annularity. For more information about these tables, see Section 1.6.

2.6 Annular Eclipse Lunar Limb Profile

Along the 2010 annular eclipse path, the Moon’s topocentric libration (physical plus optical) in longitude ranges from 

l = +2.4° to l = +0.6°; thus, a limb profile with the appropriate 

libration is required in any detailed analysis of contact times, 

central durations, etc. A profile with an intermediate value, 

however, is useful for planning purposes and may even be 

adequate for most applications. The lunar limb profile presented in Figure 2.15 includes corrections for center of mass 

and ellipticity (Morrison and Appleby 1981). It is generated 

for 7:00 UT, which corresponds to the integral hour nearest 

greatest eclipse. The antumbral shadow is then located in the 

Indian Ocean at latitude 00° 49.9′N and longitude 67° 52.1′E. 

The Moon’s topocentric libration is l=+1.58°, and the topocentric semi-diameters of the Sun and Moon are 975.6 and 

896.6 arcsec, respectively. The Moon’s angular velocity with 

respect to the Sun is 0.236 arcsec/s. 

The times of the four eclipse contacts from this location 

appear to the lower right in Figure 2.15. The limb-corrected 

times of second and third contacts are listed with the applied 

correction to the center of mass prediction. The time correction curves can be used for estimating corrections to the 

times of second and third contacts as a function of the position angle of the contact. More information on this topic and 

 8 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
a detailed description of the limb profile figure can be found 

in Section 1.8.

2.7 Weather Prospects for the Annular Eclipse

2.7.1 Introduction

During the annular eclipse of 2010, Earth intercepts the 

Moon’s shadow during the dry monsoons of January. In many 

places along the path, the weather prospects are almost guaranteed to be excellent. Alas, the political and social climates are 

major concerns, and these factors will have to be considered 

when selecting an observing site. 

In January, the Sun is far to the south and winter is in its 

depths over the Northern Hemisphere. Over tropical regions 

of Africa and Southeast Asia, winds turn to the northwest, 

tapping the warm dry air of the Sahara in Africa, or the dry 

cool air descending from the Himalayas in India and Burma. 

Sunshine dominates in most regions, interrupted only where 

high terrain or nearby moisture sources provide the forcing 

necessary to produce clouds or where the path makes a feint 

toward the tropical rain forests of Africa. While moisture is 

abundant over the Indian Ocean, the strong inversions created 

by air subsiding aloft suppresses the development of clouds and 

precipitation. On the north side of the Himalayas, the eclipse 

track encounters China’s winter season, with air masses too 

cold to support extensive cloudiness. 

2.7.2 Africa

Between the arid Sahara Desert and the equatorial rain 

forest, lies a climatic region known as the wet and dry tropics 

and it is through this zone that the Moon’s antumbral shadow 

makes its sunrise contact and early passage across the globe. 

Earth’s weather equator or Intertropical Convergence Zone 

(ITCZ) has migrated southward to its winter latitudes, permitting the drier continental air from the Sahara to spread toward 

the eclipse path. It is not a complete victory for the desert air, 

as the track skips along the boundary between the dry and wet 

zones and even dips into a nose of moist air over the Democratic 

Republic of the Congo (DRC) and Uganda before crossing back 

into the sunnier climate of Kenya (Figure 2.2). 

At Bangui in the Central African Republic, average January precipitation amounts to only 25 mm and measurable rains 

fall on only three days of the month. Sunshine is an encouraging 59% of the maximum possible at Bangui, and probably 

as much as 10% higher at the beginning of the track over the 

northwestern part of the country. Farther along, where the path 

dips into the DRC, the closer proximity of the ITCZ increases 

average cloudiness to 65% to 75% (Kisangani: Table 2.16) and 

a sunshine frequency of only 50%. 

As the lunar shadow’s path reaches the DRC–Uganda border (Figure 2.4), the terrain changes dramatically, rising from 

the flat sierra of the DRC to the elevated plateau of Uganda 

and western Kenya. It is a region of complex terrain, with a 

highly variable climatology that depends on elevation, airflow, 

and moisture supply, all of which change in small scale. In the 

eastern DRC, the Mitumba Mountains and their northward 

extension are a volcanic chain that rises above 5000 m at Mount 

Stanley and at Margherita Peak and brings a heavier cloudiness than the lower plains. Immediately east of the mountains, 

along the DRC–Uganda border, the Western Rift Valley carves 

a deep trench in the terrain to hold Lake Edward and Lake 

Albert. Once past the Rift Valley, the terrain becomes more 

sedate, and the eclipse path transits the flat uplands of Uganda 

where moisture is readily available because of the swampy 

terrain and the presence of Lake Victoria, the largest lake in 

Africa. Cloudiness is highly variable (Table 2.16), with average 

amounts ranging from 54% to 77% depending on the proximity 

of Lake Victoria. Masindi, in central Uganda and well removed 

from Lake Victoria, seems to offer the best weather with an 

average cloudiness of 54% and perhaps a 70% probability 

of sunny weather on eclipse day. Entebbe Airport, along the 

shores of Lake Victoria, records a much higher cloudiness, but 

its 62% frequency of sunshine is also promising. 

Leaving Uganda, the eclipse path moves back into the 

rougher terrain that dominates western Kenya (Figure 2.5). 

This is a region of tall volcanoes, framed by Mount Elgon 

(4321 m) in the west and Mount Kenya (5199 m) in the east, and 

cut down the middle by the Eastern Rift Valley. The position 

of the ITCZ lies well to the south of Kenya in January and the 

country offers the best prospects for sunshine in Africa, in spite 

of its rugged topography. Average cloudiness is below 50% at 

Eldoret and Kitale, and under 60% in the rest of the western 

highlands. The percent of maximum possible sunshine rises 

to a surprising 76% at Nairobi and is probably even higher at 

Eldoret. Without doubt, there will be some eclipse-watchers 

ensconced on Mount Kenya, though there are many other sites 

with high sunshine probabilities. The secret is to select a site 

in a valley behind one of the many mountains, so that the prevailing easterly winds (that is, winds blowing toward the west) 

must flow downhill to an eclipse-watcher’s encampment. A 

quick look at a topographic map will identify suitable locations 

including Nairobi, Nakuru, Kisumu, Eldoret, and Kitale. 

East of Nairobi, the eclipse moves onto the coastal plains 

of Kenya and southern Somalia. The north limit is considerably 

drier than the south, but the plains are only a little cloudier 

than the Kenyan highlands. The explanation lies in the pattern 

of the wind flow and the cool ocean currents, which together 

conspire to reduce the production of convective clouds in 

the region. Temperatures and humidity are uncomfortable 

through the lowlands, with daytime highs climbing into the 

mid-30s (°C), over 85° F, and overnight lows only falling to 

the mid-20s (°C). 

Falling temperatures during the eclipse may cause the 

formation of fog and low clouds in the high humidity of lowland 

regions, though these types of clouds are usually rare in other 

circumstances. Eclipse sites should avoid rising terrain where 

the winds blow upslope. This is easier said than done, as the 

winds across Africa are typically light in the season, and the 

winds themselves may change with the eclipse cooling. 

2.7.3 India and Sri Lanka

The eclipse path continues to head slowly southward as it 

leaves the African coast, leaving its northward turn until about 

Annular and Total Solar Eclipses of 2010 9

 Annular Solar Eclipse of 2010 January 15
halfway to India. This trend keeps the track on the northern 

margins of the ITCZ where the highest frequency of convective cloudiness occurs. At its most southerly extent, near the 

Seychelles Islands, the path encounters the most unfavorable 

climatology, with a mean cloud cover of more than 70% and a 

sunshine frequency of only 40%. By the time the track reaches 

the Maldives (Figure 2.7) and its capital Malé (23 km south of 

the central line), cloudiness has dropped to only 55% and the 

daily sunshine averages 2/3 of the amount possible. 

A little farther along, past Minicoy, the antumbral path 

reaches the southern tip of India and the states of Kerala and 

Tamil Nadu (Figure 2.8). Landfall is near Thiruvananthapuram 

(Trivandrum), where the amount of sunshine climbs to 72%. 

The dry winter season over southern India is not as cloud-free 

as farther north, but the general conditions here are slightly 

more favorable than in Kenya. The path through Kerala and 

Tamil Nadu gives a high probability of sunshine on eclipse 

day. India might be the best location from which to observe 

at the north limit, where beading phenomena are at their best. 

Climate statistics for Madurai and Cuddalore in Tamil Nadu 

(Table 2.16) characterize the north limit of the shadow track; 

there is no climate information near the north limit in Kerala, 

but Thiruvananthapuram is probably an accurate reflection of 

the area. From the cloud statistics, the east coast seems more 

suitable than the west. As in Africa, the formation of fog is 

a possibility as the ground cools during the approach of the 

shadow, but this seems unlikely if winds are light or not blowing in an upslope direction.

Sri Lanka also offers favorable weather prospects, but 

the political situation makes it all but impossible to observe 

from the island. 

2.7.4 Burma and Bangladesh

North-central Burma is a low landscape lying between 

two mountain chains, the Arakan Yoma inland from the coast 

of the Bay of Bengal, and the Shan Plateau in the west, which 

blends gradually into the Himalayan Mountains to the north. 

During January, the northeast monsoon is entrenched across 

the region, and the flow of air into the lowlands, though much 

modified by its passage southward across the subtropical 

landscape, retains the dry and stable character of its source 

region in Mongolia. Because of the Himalayas, cold Siberian 

air cannot reach Burma directly, but must first run through 

southern China and across Vietnam and Laos where the terrain 

is lower and where heat and moisture are added to the lower 

layers of the atmosphere. The region of the eclipse track, being 

rather well protected by the eastern mountains, enjoys a nearly 

rain-free climatology and abundant sunshine. Burma has the 

best weather prospects of any eclipse site along the path of the 

Moon’s antumbral shadow. 

Mandalay, in the Burma lowlands along the Irrawaddy 

River and south of the central line, offers more than 80% of 

the sunshine amount possible on a January day. The average 

cloud amount is a minuscule 15%—equal to the Sahara on its 

best days. January rainfall, though not completely absent, is 

only a few millimeters. Satellite observations of cloud cover 

(Figure 2.16) place the area around Mandalay among the sunniest parts of the globe in January. 

The dry northeast monsoon brings favorable weather to all 

of Burma, even in the humid air along the Bay of Bengal coast 

where Sittwe has nearly the same cloud and sunshine characteristics as Mandalay. Mountains still have an influence, however, 

as Mindat, in the Arakan Yoma, and Lashio in the midst of 

the Shan Plateau, have a higher, though still-excellent, average cloudiness of around 30%. Bad weather, when it comes, 

is usually formed on the weak front that develops between the 

modified polar air from the north and intrusion of maritime 

tropical air from the equator. The frontal zone typically lies 

north of the eclipse track, but makes occasional excursions 

southward whenever a fresh surge of Mongolian air reaches 

the region. January is well outside the cyclone season. 

In Burma, a location north (for the central line) or south 

(for the beaded zone) of Mandalay offers some of the best 

prospects. Highway 1, from Rangoon to Mandalay and beyond, 

provides convenient access to the width of the track. 

The northern side of the eclipse path can also be reached 

at Cox’s Bazarre in Bangladesh (Figure 2.9). One of the mostvisited tourist locations in Bangladesh, it lies 27 km inside 

the north limit and boasts the same sunny character as Sittwe to the south. Its average cloud amount is even lower than 

Mandalay.

2.7.5 China

The accelerating shadow makes its last dash across Earth 

in China, moving steadily northeastward to its sunset ending in 

the Yellow Sea southeast of Beijing (Figure 2.6). The first part 

of the trek is across the rough terrain of Yunnan and Sichuan 

provinces, crossing the southern foot of the Himalayas until 

finally reaching the flat plains of central China (Figure 2.10). In 

January, the Siberian high is at its strongest and coldest, bringing steady northeast winds to the country. This is the season of 

the winter monsoon, with frequent southward-moving surges 

of cold air. These frontal outbreaks occur at a frequency of 

about one per week and typically involve the development of 

a low-pressure system along the front that brings extensive 

cloudiness and precipitation—a pattern that will be familiar 

to North American and European visitors. The cold air is relatively shallow and does not penetrate readily into the high terrain in Yunnan, which retains the sunny character of Burma. 

The climate statistics in Table 2.16 show a steady decline 

in the percent of possible sunshine along the path, from 74% 

in Tengchong to 50% at Zengzhou. Central China, between 

Chongqing and Zengzhou, has the cloudiest weather according 

to the satellite observations (Figure 2.16). Farther northeast, 

where the dry, cold Siberian air has more influence, the weather 

prospects actually improve modestly as the eclipse track 

reaches its sunset terminus (Figure 2.14). This is a region that 

has the unique distinction of being visited by three eclipses 

in three years—two totals and now an annular. A fortunate 

observer at Xiangfan would have to travel no more than 100 km 

to see all three. 

Temperatures decline along with the weather prospects 

across China, but it is only northeast of Chongqing that freezing 

weather becomes a serious possibility, and then mostly at night. 

 10 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Along with the colder weather comes the possibility of snow, 

but most travelers from the Northern Hemisphere will find that 

the weather in China is less severe than that at home. 

2.7.6 Summary

Thanks to the dry winter season, good weather can be 

found across much of Africa, the Indian Ocean, India, Burma, 

and southwest China. Mountains should be avoided, but the 

moist air of the Indian Ocean is not inclined to make clouds 

Annular and Total Solar Eclipses of 2010 11

 Annular Solar Eclipse of 2010 January 15

and so, only the humidity will interfere with observations of the 

eclipse. Southern India is attractive and central Burma offers 

the best weather of all. Winds are generally light, fog is rare 

(though it may form during the eclipse), and temperatures on 

the plateaus are tolerable while those near sea level are hot. 

No region is without its cloudy days, however, and quick 

movement to a sunnier location is not easily done in rugged 

terrain or where roads are limited, so the best advice is to pick 

carefully at the start and hope for “climatological” weather on 

eclipse day.
 12 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15

TABLE 2.1

ELEMENTS OF THE ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

Equatorial Conjunction: 07:21:27.24 TDT J.D. = 2455211.806565

(Sun & Moon in R.A.) (=07:20:21.20 UT)

Ecliptic Conjunction: 07:12:28.46 TDT J.D. = 2455211.800329

(Sun & Moon in Ec. Lo.) (=07:11:22.41 UT)

Instant of 07:07:39.03 TDT J.D. = 2455211.796980

Greatest Eclipse: (=07:06:32.99 UT)

Geocentric Coordinates of Sun & Moon at Greatest Eclipse (JPL DE200/LE200):

Sun: R.A. = 19h47m51.053s Moon: R.A. = 19h47m25.329s

Dec. =-21°07'38.69" Dec. =-20°46'54.79"

Semi-Diameter = 16'15.54" Semi-Diameter = 14'44.35"

Eq.Hor.Par. = 08.94" Eq.Hor.Par. = 0°54'05.35"

∆ R.A. = 10.744s/h ∆ R.A. = 122.609s/h

∆ Dec. = 27.56"/h ∆ Dec. = 480.39"/h

Lunar Radius k1 = 0.2725076 (Penumbra) Shift in ∆b = 0.00"

Constants: k2 = 0.2722810 (Umbra) Lunar Position: ∆l = 0.00"

Geocentric Libration: l = 1.5° Brown Lun. No. = 1077

(Optical + Physical) b = -0.5° Saros Series = 141 (23/70)

c = -8.8° nDot = -26.00 "/cy**2

Eclipse Magnitude = 0.91903 Gamma = 0.40016 ∆T = 66.0 s

Polynomial Besselian Elements for: 2010 Jan 15 07:00:00 TDT (=t0)

n x y d l1 l2 μ

0 -0.1732440 0.3664046-21.1292992 0.5746956 0.0283960 282.671112

1 0.4845213 0.1404923 0.0073072 0.0000372 0.0000370 14.997591

2 -0.0000371 0.0001170 0.0000056 -0.0000099 -0.0000099 0.000002

3 -0.0000054 -0.0000017 0.0000000 0.0000000 0.0000000 0.000000

Tan ƒ1 = 0.0047545 Tan ƒ2 = 0.0047308

At time t1 (decimal hours), each Besselian element is evaluated by:

a = a0 + a1*t + a2*t2 + a3*t3 (or a = ∑ [an*tn]; n = 0 to 3)

where: a = x, y, d, l1, l2, or μ

t = t1 - t0 (decimal hours) and t0 = 7.00 TDT

The Besselian elements were derived from a least-squares fit to elements

calculated at five uniformly spaced times over a 6-hour period centered at

t0. Thus, they are valid over the period 4.00 ≤ t1 ≤ 10.00 TDT.

All times are expressed in Terrestrial Dynamical Time (TDT).

Saros Series 141: Member 23 of 70 eclipses in series.
Annular and Total Solar Eclipses of 2010 13

 Annular Solar Eclipse of 2010 January 15

TABLE 2.2

SHADOW CONTACTS AND CIRCUMSTANCES

ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

∆T = 66.0 s

=000°16'33.3"

Terrestrial

Dynamical Ephemeris True

Time Latitude Longitude† Longitude*

h m s

External/Internal

Contacts of Penumbra: P1 04:06:33.5 01°19.3'S 030°10.3'E 030°26.8'E

P2 06:51:12.8 49°46.0'N 016°42.4'E 016°58.9'E

P3 07:23:43.6 68°44.1'N 078°14.4'E 078°31.0'E

P4 10:08:41.1 28°48.1'N 107°54.8'E 108°11.4'E

Extreme

North/South Limits

of Penumbral Path: N1 06:38:30.2 55°02.1'N 026°15.4'E 026°31.9'E

S1 05:22:22.9 23°58.0'S 001°49.9'E 002°06.4'E

N2 07:36:14.0 68°32.5'N 057°41.0'E 057°57.6'E

S2 08:53:00.5 06°14.6'N 136°39.6'E 136°56.2'E

External/Internal

Contacts of Umbra: U1 05:15:00.9 06°20.1'N 016°01.9'E 016°18.4'E

U2 05:22:21.8 07°39.7'N 014°43.0'E 014°59.5'E

U3 08:52:46.3 37°29.1'N 121°54.8'E 122°11.4'E

U4 09:00:09.7 36°12.5'N 120°52.3'E 121°08.8'E

Extreme

North/South Limits

of Umbral Path: N1 05:19:34.2 08°37.1'N 015°47.6'E 016°04.1'E

S1 05:17:54.1 05°21.4'N 014°55.6'E 015°12.2'E

N2 08:55:34.1 38°24.0'N 120°37.1'E 120°53.7'E

S2 08:57:16.1 35°16.0'N 122°10.1'E 122°26.7'E

Extreme Limits

of Central Line: C1 05:18:40.7 06°58.7'N 015°22.1'E 015°38.6'E

C2 08:56:28.6 36°49.6'N 121°24.3'E 121°40.9'E

Instant of

Greatest Eclipse: G0 07:07:39.0 01°37.4'N 069°00.9'E 069°17.4'E

Circumstances at

Greatest Eclipse: Sun’s Altitude = 66.4° Path Width = 333.1 km

Sun’s Azimuth = 164.9° Central Duration = 11m07.8s

_____________________________________________________________________________

† Ephemeris Longitude is the terrestrial dynamical longitude assuming a

uniformly rotating Earth.

* True Longitude is calculated by correcting the Ephemeris Longitude for

the non-uniform rotation of Earth.

(T.L. = E.L. + 1.002738*∆T/240, where ∆T(in seconds) = TDT - UT)

Note: Longitude is measured positive to the East.

Because ∆T is not known in advance, the value used in the predictions is an

extrapolation based on pre-2009 measurements. The actual value is expected

to fall within ±0.3 seconds of the estimated ∆T used here.
 14 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15

TABLE 2.3

PATH OF THE ANTUMBRAL SHADOW

ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

∆T = 66.0 s

Universal Northern Limit Southern Limit Central Line Sun Path Central

Time Latitude Longitude Latitude Longitude Latitude Longitude Alt Width Durat.

° km

Limits 08°37.1'N 016°04.1'E 05°21.4'N 015°12.2'E 06°58.7'N 015°38.6'E 0 371 07m09.4s

05:20 05°36.1'N 023°55.2'E 01°10.3'N 026°38.3'E 03°16.3'N 025°32.1'E 11 360 07m41.3s

05:25 02°54.0'N 031°38.9'E 00°51.6'S 032°56.7'E 00°58.9'N 032°22.3'E 19 354 08m09.8s

05:30 01°29.3'N 036°16.1'E 02°03.8'S 037°14.5'E 00°18.8'S 036°48.0'E 25 351 08m31.7s

05:35 00°33.2'N 039°47.9'E 02°52.9'S 040°39.0'E 01°11.1'S 040°15.3'E 30 349 08m50.8s

05:40 00°06.2'S 042°43.2'E 03°27.5'S 043°31.7'E 01°48.0'S 043°08.9'E 34 347 09m08.1s

05:45 00°34.2'S 045°14.8'E 03°51.7'S 046°02.8'E 02°14.0'S 045°39.9'E 37 347 09m24.0s

05:50 00°53.5'S 047°29.2'E 04°07.8'S 048°18.0'E 02°31.6'S 047°54.5'E 41 346 09m38.7s

05:55 01°05.8'S 049°30.6'E 04°17.4'S 050°21.0'E 02°42.5'S 049°56.6'E 44 346 09m52.3s

06:00 01°12.4'S 051°21.8'E 04°21.4'S 052°14.2'E 02°47.8'S 051°48.6'E 47 346 10m04.9s

06:05 01°14.0'S 053°04.7'E 04°20.6'S 053°59.4'E 02°48.2'S 053°32.5'E 49 346 10m16.4s

06:10 01°11.3'S 054°40.7'E 04°15.5'S 055°37.9'E 02°44.2'S 055°09.7'E 52 345 10m26.9s

06:15 01°04.6'S 056°11.0'E 04°06.6'S 057°10.8'E 02°36.4'S 056°41.2'E 54 345 10m36.3s

06:20 00°54.4'S 057°36.4'E 03°54.1'S 058°38.8'E 02°25.1'S 058°07.9'E 56 345 10m44.5s

06:25 00°40.9'S 058°57.6'E 03°38.4'S 060°02.7'E 02°10.5'S 059°30.4'E 58 344 10m51.7s

06:30 00°24.4'S 060°15.3'E 03°19.6'S 061°23.0'E 01°52.8'S 060°49.3'E 60 344 10m57.7s

06:35 00°04.9'S 061°30.0'E 02°58.0'S 062°40.2'E 01°32.3'S 062°05.2'E 61 343 11m02.5s

06:40 00°17.3'N 062°42.0'E 02°33.6'S 063°54.7'E 01°09.0'S 063°18.4'E 63 341 11m06.2s

06:45 00°42.2'N 063°51.8'E 02°06.6'S 065°06.9'E 00°43.1'S 064°29.4'E 64 340 11m08.8s

06:50 01°09.6'N 064°59.8'E 01°37.0'S 066°17.2'E 00°14.6'S 065°38.4'E 65 339 11m10.3s

06:55 01°39.6'N 066°06.2'E 01°04.9'S 067°25.8'E 00°16.4'N 066°45.9'E 66 337 11m10.8s

07:00 02°12.0'N 067°11.4'E 00°30.5'S 068°33.0'E 00°49.9'N 067°52.1'E 66 335 11m10.1s

07:05 02°47.0'N 068°15.7'E 00°06.4'N 069°39.2'E 01°25.8'N 068°57.3'E 66 334 11m08.5s

07:10 03°24.4'N 069°19.4'E 00°45.6'N 070°44.6'E 02°04.1'N 070°01.9'E 66 332 11m06.0s

07:15 04°04.3'N 070°22.7'E 01°27.2'N 071°49.6'E 02°44.9'N 071°06.0'E 66 330 11m02.5s

07:20 04°46.7'N 071°25.9'E 02°11.2'N 072°54.4'E 03°28.1'N 072°10.0'E 65 329 10m58.2s

07:25 05°31.7'N 072°29.5'E 02°57.7'N 073°59.3'E 04°13.8'N 073°14.2'E 65 327 10m53.2s

07:30 06°19.4'N 073°33.6'E 03°46.6'N 075°04.7'E 05°02.1'N 074°18.9'E 63 326 10m47.4s

07:35 07°09.9'N 074°38.6'E 04°38.1'N 076°10.9'E 05°53.1'N 075°24.5'E 62 325 10m40.9s

07:40 08°03.2'N 075°45.0'E 05°32.3'N 077°18.3'E 06°46.9'N 076°31.4'E 61 324 10m33.8s

07:45 08°59.6'N 076°53.2'E 06°29.2'N 078°27.3'E 07°43.5'N 077°40.0'E 59 323 10m26.1s

07:50 09°59.3'N 078°03.6'E 07°29.2'N 079°38.4'E 08°43.3'N 078°50.7'E 57 323 10m17.8s

07:55 11°02.4'N 079°17.0'E 08°32.3'N 080°52.2'E 09°46.4'N 080°04.3'E 55 323 10m09.1s

08:00 12°09.3'N 080°33.9'E 09°38.9'N 082°09.4'E 10°53.2'N 081°21.3'E 53 323 09m59.9s

08:05 13°20.4'N 081°55.2'E 10°49.3'N 083°30.8'E 12°03.9'N 082°42.6'E 51 324 09m50.2s

08:10 14°36.2'N 083°22.0'E 12°03.9'N 084°57.4'E 13°19.1'N 084°09.3'E 48 325 09m40.1s

08:15 15°57.4'N 084°55.7'E 13°23.2'N 086°30.4'E 14°39.3'N 085°42.6'E 45 326 09m29.5s

08:20 17°24.7'N 086°38.2'E 14°48.1'N 088°11.6'E 16°05.3'N 087°24.3'E 43 327 09m18.4s

08:25 18°59.4'N 088°31.9'E 16°19.5'N 090°03.3'E 17°38.3'N 089°16.9'E 39 329 09m06.7s

08:30 20°43.2'N 090°40.6'E 17°58.9'N 092°08.6'E 19°19.7'N 091°23.7'E 36 332 08m54.5s

08:35 22°38.9'N 093°10.1'E 19°48.4'N 094°32.7'E 21°12.1'N 093°50.2'E 32 335 08m41.4s

08:40 24°50.8'N 096°10.2'E 21°51.7'N 097°23.6'E 23°19.4'N 096°45.2'E 28 339 08m27.3s

08:45 27°28.1'N 100°00.9'E 24°15.2'N 100°56.9'E 25°49.1'N 100°26.1'E 23 344 08m11.5s

08:50 30°54.8'N 105°37.0'E 27°14.3'N 105°49.4'E 29°00.1'N 105°36.9'E 17 351 07m52.7s

08:55 - - 31°58.7'N 114°52.1'E 34°49.6'N 116°59.7'E 4 367 07m21.4s

Limits 38°24.0'N 120°53.7'E 35°16.0'N 122°26.7'E 36°49.6'N 121°40.9'E 0 373 07m11.5s
Annular and Total Solar Eclipses of 2010 15

 Annular Solar Eclipse of 2010 January 15

TABLE 2.4

PHYSICAL EPHEMERIS OF THE ANTUMBRAL SHADOW

ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

∆T = 66.0 s

Universal Central Line Diameter Eclipse Sun Sun Path Major Minor Umbra Central

Time Latitude Longitude Ratio Obscur. Alt Azm Width Axis Axis Veloc. Durat.

° ° km km km km/s

05:17.6 06°58.7'N 015°38.6'E 0.9061 0.8210 0.0 111.3 370.7 - 361.0 - 07m09.4s

05:20 03°16.3'N 025°32.1'E 0.9088 0.8260 11.1 112.3 360.4 1817.1 349.5 3.820 07m41.3s

05:25 00°58.9'N 032°22.3'E 0.9108 0.8296 19.4 112.9 354.2 1025.7 341.1 2.017 08m09.8s

05:30 00°18.8'S 036°48.0'E 0.9121 0.8320 25.2 113.3 350.8 789.6 335.6 1.476 08m31.7s

05:35 01°11.1'S 040°15.3'E 0.9132 0.8339 29.8 113.8 348.8 666.5 331.3 1.193 08m50.8s

05:40 01°48.0'S 043°08.9'E 0.9140 0.8354 33.8 114.4 347.4 588.6 327.8 1.013 09m08.1s

05:45 02°14.0'S 045°39.9'E 0.9147 0.8367 37.4 115.1 346.6 534.2 324.8 0.888 09m24.0s

05:50 02°31.6'S 047°54.5'E 0.9154 0.8379 40.7 116.0 346.1 493.9 322.2 0.794 09m38.7s

05:55 02°42.5'S 049°56.6'E 0.9159 0.8389 43.7 117.0 345.8 462.7 319.9 0.723 09m52.3s

06:00 02°47.8'S 051°48.6'E 0.9164 0.8398 46.5 118.2 345.7 438.0 317.8 0.666 10m04.9s

06:05 02°48.2'S 053°32.5'E 0.9168 0.8406 49.1 119.7 345.6 417.9 316.1 0.620 10m16.4s

06:10 02°44.2'S 055°09.7'E 0.9172 0.8413 51.6 121.4 345.5 401.4 314.5 0.583 10m26.9s

06:15 02°36.4'S 056°41.2'E 0.9176 0.8419 53.9 123.3 345.2 387.8 313.1 0.553 10m36.3s

06:20 02°25.1'S 058°07.9'E 0.9178 0.8424 56.0 125.6 344.8 376.4 311.9 0.528 10m44.5s

06:25 02°10.5'S 059°30.4'E 0.9181 0.8429 57.9 128.2 344.3 366.8 310.8 0.508 10m51.7s

06:30 01°52.8'S 060°49.3'E 0.9183 0.8433 59.7 131.2 343.6 358.9 309.9 0.492 10m57.7s

06:35 01°32.3'S 062°05.2'E 0.9185 0.8437 61.3 134.6 342.6 352.4 309.1 0.480 11m02.5s

06:40 01°09.0'S 063°18.4'E 0.9187 0.8440 62.7 138.4 341.5 347.0 308.4 0.470 11m06.2s

06:45 00°43.1'S 064°29.4'E 0.9188 0.8442 63.9 142.7 340.2 342.7 307.9 0.464 11m08.8s

06:50 00°14.6'S 065°38.4'E 0.9189 0.8444 64.9 147.3 338.7 339.5 307.5 0.460 11m10.3s

06:55 00°16.4'N 066°45.9'E 0.9190 0.8445 65.7 152.4 337.1 337.1 307.2 0.458 11m10.8s

07:00 00°49.9'N 067°52.1'E 0.9190 0.8446 66.2 157.7 335.4 335.6 307.0 0.458 11m10.1s

07:05 01°25.8'N 068°57.3'E 0.9190 0.8446 66.4 163.2 333.7 335.0 307.0 0.461 11m08.5s

07:10 02°04.1'N 070°01.9'E 0.9190 0.8446 66.3 168.8 332.0 335.2 307.0 0.466 11m06.0s

07:15 02°44.9'N 071°06.0'E 0.9190 0.8445 66.0 174.3 330.3 336.2 307.2 0.472 11m02.5s

07:20 03°28.1'N 072°10.0'E 0.9189 0.8444 65.4 179.6 328.7 338.1 307.5 0.480 10m58.2s

07:25 04°13.8'N 073°14.2'E 0.9188 0.8442 64.6 184.7 327.3 340.9 307.9 0.491 10m53.2s

07:30 05°02.1'N 074°18.9'E 0.9187 0.8440 63.5 189.4 326.0 344.6 308.4 0.504 10m47.4s

07:35 05°53.1'N 075°24.5'E 0.9185 0.8437 62.2 193.7 324.9 349.4 309.1 0.519 10m40.9s

07:40 06°46.9'N 076°31.4'E 0.9183 0.8433 60.7 197.7 324.1 355.3 309.9 0.536 10m33.8s

07:45 07°43.5'N 077°40.0'E 0.9181 0.8429 59.0 201.3 323.4 362.4 310.8 0.556 10m26.1s

07:50 08°43.3'N 078°50.7'E 0.9179 0.8425 57.1 204.6 323.1 371.1 311.8 0.580 10m17.8s

07:55 09°46.4'N 080°04.3'E 0.9176 0.8419 55.1 207.6 323.0 381.4 313.0 0.607 10m09.1s

08:00 10°53.2'N 081°21.3'E 0.9172 0.8413 52.9 210.3 323.2 393.7 314.4 0.639 09m59.9s

08:05 12°03.9'N 082°42.6'E 0.9169 0.8406 50.6 212.8 323.7 408.6 315.9 0.676 09m50.2s

08:10 13°19.1'N 084°09.3'E 0.9164 0.8399 48.1 215.1 324.5 426.5 317.7 0.720 09m40.1s

08:15 14°39.3'N 085°42.6'E 0.9160 0.8390 45.4 217.3 325.7 448.4 319.6 0.773 09m29.5s

08:20 16°05.3'N 087°24.3'E 0.9155 0.8380 42.5 219.4 327.3 475.6 321.8 0.838 09m18.4s

08:25 17°38.3'N 089°16.9'E 0.9149 0.8370 39.4 221.4 329.3 510.2 324.3 0.919 09m06.7s

08:30 19°19.7'N 091°23.7'E 0.9142 0.8357 36.0 223.4 331.8 555.6 327.1 1.025 08m54.5s

08:35 21°12.1'N 093°50.2'E 0.9134 0.8343 32.2 225.4 334.9 618.1 330.4 1.170 08m41.4s

08:40 23°19.4'N 096°45.2'E 0.9125 0.8326 28.0 227.7 338.8 710.6 334.3 1.382 08m27.3s

08:45 25°49.1'N 100°26.1'E 0.9113 0.8305 23.0 230.2 343.8 866.2 339.0 1.738 08m11.5s

08:50 29°00.1'N 105°36.9'E 0.9098 0.8277 16.5 233.6 351.0 1209.8 345.4 2.519 07m52.7s

08:55 34°49.6'N 116°59.7'E 0.9068 0.8223 4.4 240.5 366.6 4618.8 358.0 10.219 07m21.4s

08:55.4 36°49.6'N 121°40.9'E 0.9058 0.8204 0.0 243.2 372.7 - 362.6 - 07m11.5s
 16 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15

TABLE 2.5

LOCAL CIRCUMSTANCES ON THE CENTRAL LINE

ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

∆T = 66.0 s

Central Line

Maximum Eclipse First Contact Second Contact Third Contact Fourth Contact .

U.T. Durat. Alt U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt

05:18 07m09.5s 1 - - - - - - - 05:21:10 84 167 06:37:27 83 158 18

05:20 07m41.3s 11 - - - - 05:16:10 264 346 05:23:51 83 165 06:50:06 82 154 32

05:25 08m09.8s 19 04:05:54 264 352 1 05:20:56 262 344 05:29:06 82 163 07:04:02 80 148 42

05:30 08m31.7s 25 04:06:42 263 351 6 05:25:45 261 342 05:34:17 81 161 07:15:34 78 142 49

05:35 08m50.8s 30 04:08:00 262 350 10 05:30:35 260 340 05:39:26 80 158 07:25:55 76 136 54

05:40 09m08.1s 34 04:09:37 262 349 13 05:35:27 259 337 05:44:35 79 156 07:35:23 74 129 59

05:45 09m24.0s 37 04:11:26 261 347 16 05:40:19 258 335 05:49:43 78 153 07:44:08 73 122 62

05:50 09m38.7s 41 04:13:25 260 346 19 05:45:12 257 332 05:54:50 77 150 07:52:15 71 114 66

05:55 09m52.3s 44 04:15:31 260 344 21 05:50:05 256 329 05:59:57 75 147 07:59:47 69 104 68

06:00 10m04.9s 47 04:17:45 259 343 23 05:54:59 255 326 06:05:03 74 144 08:06:47 68 94 70

06:05 10m16.4s 49 04:20:05 258 341 25 05:59:53 254 323 06:10:09 73 141 08:13:19 66 83 71

06:10 10m26.9s 52 04:22:31 257 339 27 06:04:47 252 320 06:15:14 72 137 08:19:26 65 72 71

06:15 10m36.3s 54 04:25:03 256 337 29 06:09:43 251 316 06:20:19 71 133 08:25:10 64 62 71

06:20 10m44.5s 56 04:27:41 256 335 31 06:14:38 250 312 06:25:23 69 129 08:30:34 63 52 71

06:25 10m51.7s 58 04:30:26 255 333 33 06:19:35 249 308 06:30:26 68 124 08:35:40 62 44 70

06:30 10m57.7s 60 04:33:18 254 331 35 06:24:32 248 303 06:35:29 67 119 08:40:30 61 36 69

06:35 11m02.5s 61 04:36:16 253 328 36 06:29:29 247 298 06:40:32 66 114 08:45:06 60 30 68

06:40 11m06.2s 63 04:39:22 252 326 38 06:34:27 245 293 06:45:33 65 108 08:49:29 59 24 66

06:45 11m08.8s 64 04:42:36 251 323 40 06:39:26 244 287 06:50:34 64 102 08:53:42 58 20 65

06:50 11m10.3s 65 04:45:59 250 321 41 06:44:25 243 281 06:55:35 63 95 08:57:44 58 16 63

06:55 11m10.8s 66 04:49:31 249 318 43 06:49:25 242 275 07:00:35 62 88 09:01:39 57 12 61

07:00 11m10.1s 66 04:53:13 248 315 44 06:54:25 241 268 07:05:35 61 82 09:05:26 56 9 59

07:05 11m08.5s 66 04:57:06 247 312 46 06:59:25 240 262 07:10:34 60 75 09:09:06 56 7 58

07:10 11m06.0s 66 05:01:09 246 308 47 07:04:27 240 255 07:15:32 59 68 09:12:40 56 5 56

07:15 11m02.5s 66 05:05:25 245 304 48 07:09:28 239 248 07:20:31 58 61 09:16:08 55 3 54

07:20 10m58.2s 65 05:09:54 244 301 50 07:14:30 238 242 07:25:28 58 55 09:19:32 55 2 52

07:25 10m53.2s 65 05:14:36 243 297 51 07:19:33 237 236 07:30:26 57 49 09:22:51 55 0 50

07:30 10m47.4s 63 05:19:32 242 292 52 07:24:36 237 230 07:35:23 56 43 09:26:07 55 359 48

07:35 10m40.9s 62 05:24:44 242 287 53 07:29:39 236 224 07:40:20 56 39 09:29:18 54 358 46

07:40 10m33.8s 61 05:30:11 241 282 54 07:34:42 236 219 07:45:16 56 34 09:32:26 54 358 44

07:45 10m26.1s 59 05:35:53 240 277 55 07:39:46 235 215 07:50:12 55 30 09:35:31 54 357 42

07:50 10m17.8s 57 05:41:53 239 272 55 07:44:50 235 211 07:55:08 55 27 09:38:32 54 357 40

07:55 10m09.1s 55 05:48:09 238 266 56 07:49:55 235 208 08:00:04 55 24 09:41:30 55 356 38

08:00 09m59.9s 53 05:54:43 238 260 56 07:54:59 235 204 08:04:59 55 21 09:44:25 55 356 35

08:05 09m50.2s 51 06:01:34 237 253 56 08:00:04 235 202 08:09:54 55 18 09:47:16 55 356 33

08:10 09m40.1s 48 06:08:42 237 247 55 08:05:09 235 199 08:14:49 55 16 09:50:03 55 356 31

08:15 09m29.5s 45 06:16:09 236 241 54 08:10:14 235 197 08:19:44 55 15 09:52:46 56 356 28

08:20 09m18.4s 43 06:23:53 236 234 53 08:15:20 235 195 08:24:38 55 13 09:55:25 56 357 25

08:25 09m06.7s 39 06:31:57 236 228 51 08:20:26 235 194 08:29:33 55 12 09:57:57 57 357 23

08:30 08m54.5s 36 06:40:21 236 223 49 08:25:32 236 193 08:34:27 56 11 10:00:22 57 358 19

08:35 08m41.4s 32 06:49:08 236 218 46 08:30:39 236 192 08:39:20 56 10 10:02:38 58 359 16

08:40 08m27.3s 28 06:58:22 237 213 42 08:35:46 237 191 08:44:13 57 10 10:04:41 59 360 12

08:45 08m11.5s 23 07:08:14 237 208 37 08:40:54 238 191 08:49:05 58 10 10:06:23 60 1 8

08:50 07m52.7s 17 07:19:10 238 205 31 08:46:03 239 191 08:53:56 60 10 10:07:25 61 3 2

08:55 07m21.4s 5 07:34:09 241 201 18 08:51:19 242 192 08:58:40 62 12 - - - -
Annular and Total Solar Eclipses of 2010 17

 Annular Solar Eclipse of 2010 January 15

TABLE 2.6

TOPOCENTRIC DATA AND PATH CORRECTIONS DUE TO LUNAR LIMB PROFILE

ANNULAR SOLAR ECLIPSE OF 2010 JANUARY 15

∆T = 66.0 s

North South

Moon Moon Moon Topo North Limit Limit Central

Universal Topo Topo Rel. Lib. Sun Sun Path Limit —————————— —————————— Durat.

Time H.P. S.D. Ang.V Long Alt. Az. Az. P.A. Int. Ext. Int. Ext. Corr.

" " "/s ° ° ° ° ° ' ' ' ' s

05:20 3256.0 886.6 0.386 2.42 11.1 112.3 109.6 173.5 -2.9 2.9 0.9 -4.2 -8.5

05:25 3263.1 888.6 0.355 2.38 19.4 112.9 107.3 172.4 -2.4 3.3 0.9 -3.6 -10.1

05:30 3267.9 889.9 0.335 2.34 25.2 113.3 105.2 171.3 -2.3 3.2 0.8 -3.3 -11.4

05:35 3271.6 890.9 0.319 2.30 29.8 113.8 103.0 170.2 -2.3 3.5 0.7 -3.4 -12.6

05:40 3274.6 891.7 0.306 2.26 33.8 114.4 100.9 169.1 -1.8 3.0 0.4 -2.9 -13.5

05:45 3277.2 892.4 0.295 2.21 37.4 115.1 98.6 168.0 -1.7 2.5 0.3 -2.9 -14.6

05:50 3279.5 893.0 0.285 2.17 40.7 116.0 96.3 166.9 -2.4 2.1 0.7 -3.3 -15.5

05:55 3281.5 893.5 0.277 2.13 43.7 117.0 93.9 165.7 -2.8 1.7 0.8 -2.8 -16.3

06:00 3283.3 894.0 0.270 2.09 46.5 118.2 91.4 164.5 -2.8 1.6 0.8 -2.8 -17.4

06:05 3284.9 894.4 0.263 2.04 49.1 119.7 88.9 163.3 -2.4 1.9 0.6 -2.8 -17.8

06:10 3286.2 894.8 0.258 2.00 51.6 121.4 86.4 162.2 -1.5 2.2 0.5 -3.0 -18.0

06:15 3287.5 895.1 0.253 1.96 53.9 123.3 83.8 161.0 -1.5 2.8 0.9 -4.1 -17.8

06:20 3288.5 895.4 0.249 1.92 56.0 125.6 81.2 159.8 -2.2 2.9 1.0 -4.5 -17.7

06:25 3289.5 895.7 0.245 1.87 57.9 128.2 78.7 158.6 -2.7 2.0 0.6 -4.9 -17.4

06:30 3290.3 895.9 0.242 1.83 59.7 131.2 76.1 157.4 -2.9 2.5 0.7 -5.2 -17.1

06:35 3291.0 896.1 0.240 1.79 61.3 134.6 73.6 156.3 -3.0 3.0 1.1 -4.9 -16.7

06:40 3291.6 896.2 0.238 1.75 62.7 138.4 71.1 155.2 -2.7 3.1 1.0 -4.4 -16.2

06:45 3292.0 896.4 0.237 1.70 63.9 142.7 68.7 154.1 -2.5 3.6 1.0 -4.2 -16.0

06:50 3292.4 896.5 0.236 1.66 64.9 147.3 66.4 153.0 -3.4 4.1 1.4 -4.7 -15.9

06:55 3292.6 896.5 0.236 1.62 65.7 152.4 64.2 152.0 -3.9 4.6 1.5 -4.2 -15.7

07:00 3292.8 896.6 0.236 1.58 66.2 157.7 62.2 151.1 -4.1 3.5 1.2 -3.9 -15.4

07:05 3292.8 896.6 0.236 1.53 66.4 163.2 60.2 150.2 -4.6 4.0 1.1 -4.2 -15.0

07:10 3292.8 896.6 0.237 1.49 66.3 168.8 58.4 149.3 -4.7 3.7 1.1 -4.5 -14.3

07:15 3292.6 896.5 0.239 1.45 66.0 174.3 56.7 148.5 -4.7 4.1 1.2 -4.8 -13.8

07:20 3292.4 896.5 0.240 1.41 65.4 179.6 55.2 147.8 -4.4 4.5 1.3 -4.5 -13.3

07:25 3292.0 896.4 0.243 1.36 64.6 184.7 53.8 147.2 -4.1 4.9 1.2 -4.3 -12.8

07:30 3291.5 896.2 0.245 1.32 63.5 189.4 52.6 146.6 -3.7 5.2 1.2 -4.2 -12.4

07:35 3291.0 896.1 0.248 1.28 62.2 193.7 51.5 146.1 -3.7 5.7 1.3 -4.1 -12.2

07:40 3290.3 895.9 0.251 1.24 60.7 197.7 50.6 145.7 -4.1 5.6 1.2 -4.0 -12.0

07:45 3289.5 895.7 0.255 1.19 59.0 201.3 49.8 145.3 -4.3 4.9 1.1 -3.9 -11.7

07:50 3288.5 895.4 0.259 1.15 57.1 204.6 49.2 145.0 -4.4 4.5 1.0 -3.7 -11.4

07:55 3287.5 895.2 0.264 1.11 55.1 207.6 48.8 144.8 -4.5 4.6 0.9 -3.8 -11.1

08:00 3286.3 894.8 0.269 1.07 52.9 210.3 48.5 144.7 -4.5 4.7 0.9 -3.9 -10.7

08:05 3284.9 894.5 0.275 1.02 50.6 212.8 48.4 144.6 -4.5 4.8 0.9 -3.9 -10.5

08:10 3283.4 894.1 0.281 0.98 48.1 215.1 48.4 144.7 -4.5 4.7 0.9 -3.9 -10.3

08:15 3281.7 893.6 0.288 0.94 45.4 217.3 48.6 144.8 -4.4 4.7 1.0 -3.9 -10.1

08:20 3279.8 893.1 0.295 0.90 42.5 219.4 48.9 145.1 -4.3 5.3 1.1 -4.0 -9.8

08:25 3277.6 892.5 0.304 0.86 39.4 221.4 49.5 145.4 -4.2 5.5 1.2 -4.2 -9.7

08:30 3275.1 891.8 0.313 0.81 36.0 223.4 50.2 145.8 -3.9 6.0 1.3 -4.4 -9.5

08:35 3272.3 891.1 0.324 0.77 32.2 225.4 51.2 146.4 -3.4 5.7 1.3 -4.7 -9.3

08:40 3268.9 890.2 0.337 0.73 28.0 227.7 52.5 147.2 -3.9 5.2 1.1 -5.0 -9.1

08:45 3264.8 889.0 0.352 0.69 23.0 230.2 54.1 148.2 -4.4 4.6 1.2 -5.5 -9.2

08:50 3259.3 887.6 0.372 0.64 16.5 233.6 56.5 149.5 -4.5 3.9 1.1 -4.7 -9.4

08:55 3248.7 884.7 0.412 0.60 4.4 240.5 61.3 152.3 -3.8 4.6 1.3 -4.9 -9.0
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

ANGOLALuanda 08°48'S 013°14'E 59 — — — 06:21:43.1 56 148 18 05:14:47.9 355 93 3 111 0.508 0.387BENINCotonou 06°21'N 002°26'E — — — — 06:26:55.3 75 157 4 06:07 Rise — — 0 111 0.253 0.142Porto-Novo 06°29'N 002°37'E — — — — 06:27:06.8 76 157 4 06:07 Rise — — 0 111 0.262 0.150BOTSWANAGaborone 24°45'S 025°55'E — 04:38:01.5 315 67 11 — — 06:14:32.5 29 135 33 05:23:58.0 352 102 21 104 0.198 0.100BURUNDIBujumbura 03°23'S 029°22'E — 04:05:43.7 273 6 0 — — 06:53:40.7 72 149 39 05:21:02.1 353 80 17 111 0.812 0.732CAMEROONDouala 04°03'N 009°42'E — — — — 06:29:48.1 76 157 12 05:34 Rise — — 0 111 0.668 0.565Yaoundé 03°52'N 011°31'E 770 — — — 06:31:14.1 76 157 14 05:27 Rise — — 0 111 0.760 0.671CENTRAL AFRICAN REPUBLICBangui 04°22'N 018°35'E 387 — 05:15:09.1 321 45 05:19:10.6 28 111 06:39:30.5 81 156 23 05:17:10.1 354 78 4 112 0.907 0.823 0.167 04m02sBouar 05°57'N 015°36'E — — 05:14:13.0 300 24 05:20:01.2 49 132 06:36:47.3 82 158 19 05:17:07.0 354 78 1 111 0.906 0.821 0.417 05m48sCHADMoundou 08°34'N 016°05'E — — 05:17:38.4 187 268 05:19:15.2 161 242 06:38:49.7 86 159 18 05:18:27.2 174 255 1 111 0.906 0.821 0.025 01m37sNdjamena 12°07'N 015°03'E 295 — — — 06:39:33.4 91 161 16 05:26 Rise — — 0 112 0.809 0.726CONGOBrazzaville 04°16'S 015°17'E 318 — — — 06:28:47.8 65 152 20 05:14:45.0 354 88 3 111 0.651 0.545Pointe-Noire 04°48'S 011°51'E 50 — — — 06:24:22.5 62 151 16 05:14:34.7 355 90 1 111 0.601 0.489DEM. REP. CONGOBeni 00°30'N 029°28'E — — 05:19:51.1 320 43 05:24:10.2 26 109 06:56:41.7 78 150 38 05:22:00.9 353 76 16 112 0.910 0.828 0.161 04m19sBunia 01°34'N 030°15'E — — 05:19:05.9 266 348 05:27:05.4 80 161 06:59:09.9 80 150 39 05:23:05.0 353 74 17 113 0.910 0.828 0.944 08m00sButembo 00°09'N 029°17'E — — — — 06:56:03.1 78 150 38 05:21:45.1 353 76 16 112 0.906 0.827Isiro 02°47'N 027°37'E — — 05:17:25.8 255 337 05:25:10.8 91 172 06:53:59.9 82 152 35 05:21:17.7 173 255 14 113 0.909 0.827 0.861 07m45sKananga 05°54'S 022°25'E — — — — 06:37:46.5 66 150 30 05:16:35.7 354 86 11 110 0.679 0.578Kinshasa 04°18'S 015°18'E — — — — 06:28:47.6 65 152 20 05:14:45.4 354 88 3 111 0.650 0.545Kisangani 00°30'S 025°12'E — — — — 06:47:07.6 76 152 32 05:18:37.6 354 79 12 112 0.851 0.775Kolwezi 10°43'S 025°28'E — 04:11:06.8 287 29 1 — — 06:38:21.8 58 147 34 05:18:26.1 353 89 16 109 0.577 0.463Lubumbashi 11°40'S 027°28'E — 04:11:24.9 288 29 3 — — 06:41:13.8 57 146 37 05:19:47.1 353 89 18 109 0.569 0.454Mbuji-Mayi 06°09'S 023°38'E — — — — 06:39:40.8 66 150 31 05:17:08.5 354 86 12 110 0.684 0.584DJIBOUTIDjibouti 11°36'N 043°09'E 7 04:22:23.3 240 313 11 — — 07:42:18.3 94 132 50 05:50:30.2 168 230 30 123 0.616 0.507EGYPTCairo 30°03'N 031°15'E 116 — — — 07:04:33.6 122 164 23 05:53:45.1 170 222 11 122 0.289 0.173EQUATORIAL GUINEAMalabo, Bioko 03°45'N 008°47'E — — — — 06:28:50.7 75 156 11 05:38 Rise — — 0 111 0.620 0.510ERITREAAsmera 15°20'N 038°53'E 2325 04:24:26.1 237 308 6 — — 07:27:05.1 101 144 42 05:45:31.2 170 231 23 122 0.549 0.433ETHIOPIAAddis Ababa 09°02'N 038°42'E 2450 04:14:29.2 247 325 6 — — 07:25:58.8 92 141 46 05:38:44.9 170 239 25 118 0.701 0.605GABONLibreville 00°23'N 009°27'E 35 — — — 06:26:43.6 70 154 13 05:30 Rise — — 0 111 0.642 0.535GHANAAccra 05°33'N 000°13'W 27 — — — 06:25:09.1 72 156 2 06:16 Rise — — 0 111 0.112 0.043KENYAEldoret 00°31'N 035°17'E — 04:06:25.4 263 351 4 05:24:12.6 248 328 05:32:21.7 96 175 07:11:40.0 79 145 46 05:28:16.5 172 252 23 113 0.912 0.831 0.756 08m09sKisumu 00°06'S 034°45'E — 04:06:07.7 264 353 4 05:23:18.4 275 356 05:31:27.0 69 149 07:09:44.4 78 145 46 05:27:22.0 352 73 23 113 0.912 0.831 0.779 08m09sMachakos 01°31'S 037°16'E — 04:06:38.1 265 354 7 05:27:01.1 302 24 05:33:26.3 40 120 07:16:04.9 76 141 50 05:30:13.6 351 72 26 113 0.912 0.832 0.339 06m25sMeru 00°03'N 037°39'E — 04:07:07.0 262 349 7 05:27:21.9 240 320 05:35:24.4 102 181 07:18:26.0 78 141 50 05:31:22.6 171 250 26 114 0.912 0.832 0.642 08m03sMombasa 04°03'S 039°40'E 16 04:07:28.5 267 358 10 — — 07:21:21.8 72 137 54 05:33:02.3 350 73 30 112 0.875 0.804Nairobi 01°17'S 036°49'E 1820 04:06:28.6 265 354 6 05:26:11.6 297 18 05:33:05.0 45 126 07:14:52.2 76 142 49 05:29:38.0 351 72 25 113 0.912 0.832 0.412 06m53sNakuru 00°17'S 036°04'E — 04:06:27.5 263 352 5 05:24:48.5 268 348 05:33:13.4 75 155 07:13:24.2 78 143 48 05:29:00.2 351 72 24 113 0.912 0.832 0.894 08m25sLESOTHOMaseru 29°28'S 027°30'E — 04:56:04.4 328 83 18 — — 06:01:21.1 15 127 32 05:27:48.1 352 105 25 101 0.084 0.028LIBYABanghazi 32°07'N 020°04'E 25 — — — 06:50:09.3 122 170 12 05:45:13.7 172 227 1 115 0.328 0.208Tripoli 32°54'N 013°11'E 22 — — — 06:45:58.6 120 171 6 06:12 Rise — — 0 115 0.268 0.155

 18 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

MADAGASCARAntananarivo 18°55'S 047°31'E — 04:23:50.7 288 30 26 — — 07:20:54.8 44 133 67 05:44:53.3 347 83 44 101 0.497 0.377Fianarantsoa 21°26'S 047°05'E — 04:28:19.9 294 37 27 — — 07:13:07.1 40 135 65 05:44:23.3 347 87 44 99 0.423 0.300MALAWIBlantyre 15°47'S 035°00'E — 04:15:13.8 290 33 12 — — 06:52:44.4 52 142 48 05:26:58.0 351 88 28 106 0.517 0.398Lilongwe 13°59'S 033°44'E — 04:12:53.0 288 29 9 — — 06:52:23.3 55 143 46 05:25:17.9 352 87 26 107 0.558 0.442MAYOTTEDzaoudzi 12°47'S 045°17'E — 04:14:29.4 279 15 20 — — 07:27:23.7 56 131 65 05:41:02.5 348 77 40 107 0.664 0.562MOZAMBIQUEBeira 19°49'S 034°52'E 9 04:22:07.5 298 44 14 — — 06:45:03.4 44 140 47 05:28:03.9 351 93 29 104 0.403 0.280Maputo 25°58'S 032°35'E 59 04:38:25.6 313 64 18 — — 06:25:05.3 29 135 41 05:28:57.0 351 100 29 101 0.216 0.114NAMIBIAWindhoek 22°34'S 017°06'E 1728 04:38:53.9 318 71 3 — — 06:04:07.6 29 135 22 05:19:45.1 353 103 12 108 0.179 0.086NIGERNiamey 13°31'N 002°07'E 216 — 06:19:44.1 06:19:44.1 06:32:00.6 86 161 2 06:20 Rise — — 0 112 0.156 0.070NIGERIAIbadan 07°17'N 003°30'E — — — — 06:28:09.3 77 158 5 06:04 Rise — — 0 111 0.303 0.186Kano 12°00'N 008°30'E — — — — 06:34:10.8 87 161 9 05:52 Rise — — 0 112 0.521 0.402Lagos 06°27'N 003°24'E 3 — — — 06:27:28.1 76 157 5 06:03 Rise — — 0 111 0.306 0.188Ogbomosho 08°08'N 004°15'E — — — — 06:29:09.8 79 158 6 06:03 Rise — — 0 111 0.337 0.216RWANDAKigali 01°57'S 030°04'E — 04:05:29.0 270 2 0 — — 06:56:23.8 75 149 39 05:21:53.7 353 78 18 112 0.857 0.783SOMALIAKismaayo 00°22'S 042°32'E — 04:09:38.6 260 345 12 05:36:51.6 205 282 05:42:09.2 134 210 07:34:28.5 77 131 57 05:39:30.6 169 245 33 115 0.914 0.835 0.187 05m18sMoqadisho 02°04'N 045°22'E 12 04:13:17.9 254 336 15 — — 07:46:58.4 79 122 60 05:47:00.8 168 239 36 118 0.845 0.771SOUTH AFRICABloemfontein 29°12'S 026°07'E — 04:56:07.4 329 84 17 — — 05:59:22.8 15 127 30 05:26:54.1 352 105 23 102 0.080 0.026Durban 29°55'S 030°56'E 5 04:55:22.8 326 81 21 — — 06:07:15.8 16 128 36 05:30:11.9 351 104 28 99 0.096 0.034Johannesburg 26°15'S 028°00'E — 04:41:42.8 317 70 14 — — 06:14:27.2 26 134 35 05:25:59.6 352 102 24 103 0.174 0.083Pretoria 25°45'S 028°10'E 1369 04:39:50.7 316 68 14 — — 06:16:15.6 27 135 35 05:25:45.9 352 101 24 103 0.189 0.093SUDANKhartoum 15°36'N 032°32'E 390 — — — 07:09:06.7 102 154 34 05:35:30.8 171 238 16 118 0.585 0.472SWAZILANDMbabane 26°18'S 031°06'E — 04:40:09.6 315 67 17 — — 06:20:52.4 27 135 39 05:28:01.9 351 101 27 101 0.196 0.099TANZANIADar-es-Salaam 06°48'S 039°17'E 14 04:07:54.9 272 5 11 — — 07:17:11.9 67 138 54 05:31:51.0 351 76 30 111 0.798 0.717Mwanza 02°31'S 032°54'E — 04:05:37.9 269 1 3 — — 07:02:57.9 74 146 44 05:24:31.7 352 77 21 112 0.866 0.793TOGOLome 06°08'N 001°13'E 22 — — — 06:26:12.5 74 156 3 06:12 Rise — — 0 111 0.187 0.092TUNISIATunis 36°48'N 010°11'E 66 — — — 06:46:12.9 123 172 2 06:33 Rise — — 0 116 0.111 0.042UGANDAJinja 00°26'N 033°12'E — 04:05:54.6 264 353 2 05:21:40.9 272 354 05:29:46.6 72 153 07:05:51.4 79 147 43 05:25:43.1 352 73 21 113 0.911 0.830 0.823 08m06sKampala 00°19'N 032°25'E 1312 04:05:44.0 265 354 2 05:21:02.1 285 7 05:28:33.2 59 141 07:03:42.6 79 148 42 05:24:47.1 352 74 20 113 0.911 0.830 0.612 07m31sMasaka 00°20'S 031°44'E — 04:05:34.7 266 356 1 05:22:10.2 327 50 05:25:36.0 17 100 07:01:34.3 77 148 41 05:23:53.5 353 75 19 112 0.911 0.829 0.094 03m26sMbale 01°05'N 034°10'E — 04:06:17.5 262 350 3 05:23:16.4 239 320 05:30:56.4 105 184 07:08:53.0 80 146 44 05:27:05.9 172 252 22 113 0.911 0.830 0.612 07m40sVENDAThohoyandou 23°00'S 030°29'E — 04:30:29.5 307 57 13 — — 06:28:17.7 35 138 40 05:25:47.2 352 98 25 103 0.282 0.168ZAMBIAKitwe 12°49'S 028°13'E — 04:12:29.5 289 31 4 — — 06:41:20.4 56 145 38 05:20:30.2 353 89 19 108 0.544 0.427Lusaka 15°25'S 028°17'E 1277 04:15:56.6 294 38 6 — — 06:37:49.0 51 144 38 05:21:10.7 353 92 20 107 0.473 0.351Ndola 12°58'S 028°38'E — 04:12:33.0 289 31 4 — — 06:42:01.7 55 145 39 05:20:49.3 353 89 20 108 0.544 0.427ZIMBABWEBulawayo 20°09'S 028°36'E 1343 04:24:25.0 303 51 9 — — 06:30:23.7 41 141 38 05:23:07.7 352 96 22 105 0.346 0.225Harare 17°50'S 031°03'E 1472 04:19:03.3 296 42 10 — — 06:39:54.0 47 142 42 05:23:58.0 352 93 24 106 0.429 0.306

Annular and Total Solar Eclipses of 2010 19

 Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

ALBANIATiranë 41°20'N 019°50'E 7 — — — 06:50:35.6 134 175 7 06:06 Rise — — 0 118 0.171 0.080AUSTRIAVienna 48°13'N 016°20'E 202 — — — 06:49:59.4 142 179 1 06:43 Rise — — 0 122 0.035 0.008BOSNIA &

HERZEGOWINA

Sarajevo 43°52'N 018°25'E — — — — 06:50:06.2 137 177 4 06:19 Rise — — 0 119 0.129 0.053BULGARIASofija 42°41'N 023°19'E 550 — — — 06:52:22.2 138 176 8 06:07:33.3 169 212 2 121 0.133 0.055CROATIAZagreb 45°48'N 015°58'E — — — — 06:49:41.8 139 178 2 06:35 Rise — — 0 120 0.072 0.022CZECH REPUBLICOstrava 49°50'N 018°17'E — — — — 06:50:06.7 146 180 1 06:41 Rise — — 0 123 0.035 0.007GREECEAthens 37°58'N 023°43'E 107 — — — 06:53:16.8 131 173 11 05:58:41.2 170 218 3 119 0.200 0.101HUNGARYBudapest 47°30'N 019°05'E 120 — — — 06:50:17.0 143 179 3 06:29 Rise — — 0 122 0.078 0.025ITALYNaples 40°51'N 014°17'E 25 — — — 06:48:26.8 131 175 3 06:27 Rise — — 0 118 0.133 0.056Rome 41°54'N 012°29'E 115 — — — 06:48:17.8 131 175 2 06:37 Rise — — 0 118 0.075 0.024MACEDONIASkopje 41°59'N 021°26'E 240 — — — 06:51:23.4 136 176 7 06:04:17.4 170 214 0 119 0.153 0.069MOLDOVAKisin'ov 47°00'N 028°50'E — 05:53:36.6 188 226 1 — — 06:54:12.5 147 179 8 06:23:17.1 168 203 5 128 0.057 0.016POLANDKrakow 50°03'N 019°58'E 220 — — — 06:50:06.9 147 181 2 06:35 Rise — — 0 123 0.047 0.012Warsaw 52°15'N 021°00'E 90 — — — 06:49:28.7 151 183 1 06:41 Rise — — 0 125 0.023 0.004ROMANIABucharest 44°26'N 026°06'E 82 — — — 06:53:42.7 142 177 9 06:14:19.5 169 208 3 124 0.096 0.035RUSSIABarnaul 53°22'N 083°45'E — 07:14:50.2 195 189 15 — — 09:12:37.6 114 91 8 08:15:27.6 154 139 12 204 0.227 0.122Chelyabinsk 55°10'N 061°24'E — 07:09:25.3 175 183 13 — — 08:05:41.2 141 141 14 07:37:37.4 158 162 14 174 0.040 0.009Irkutsk 52°16'N 104°20'E 467 07:25:17.1 211 191 11 — — — 08:36:10.0 154 126 4 227 0.439 0.316Kemerovo 55°20'N 086°05'E — 07:17:43.7 195 188 13 — — 09:12:08.1 114 92 6 08:16:31.5 155 139 10 206 0.225 0.120Krasnojarsk 56°01'N 092°50'E 152 07:21:06.2 200 188 11 — — 09:20:51.2 110 84 2 08:22:52.5 155 135 7 214 0.275 0.161Novokuzneck 53°45'N 087°06'E — 07:16:56.0 197 189 14 — — 09:17:44.1 111 87 6 08:19:15.2 154 137 11 208 0.253 0.143Novosibirsk 55°02'N 082°55'E — 07:16:03.3 193 187 13 — — 09:06:58.0 117 96 8 08:12:55.3 155 141 11 203 0.200 0.102Omsk 55°00'N 073°24'E 85 07:12:04.1 186 186 14 — — 08:44:46.5 126 113 12 07:59:06.8 156 149 13 190 0.122 0.049Tomsk 56°30'N 084°58'E — 07:18:10.7 194 187 12 — — 09:07:15.3 117 96 6 08:14:04.0 155 141 9 205 0.202 0.103Ufa 54°44'N 055°56'E 174 07:08:59.0 170 181 12 — — 07:44:20.4 149 155 14 07:26:40.6 159 168 13 166 0.015 0.002Vladivostok 43°10'N 131°56'E 29 07:40:17.5 240 199 3 — — — 08:00 Set — — 0 241 0.250 0.140Volgograd 48°44'N 044°25'E — 06:35:30.3 175 200 12 — — 07:14:34.3 151 171 15 06:54:57.6 163 185 14 147 0.018 0.003SERBIA AND MONTENEGROBeograd 44°50'N 020°30'E 138 — — — 06:50:48.0 140 178 5 06:14 Rise — — 0 120 0.119 0.047SLOVAKIABratislava 48°09'N 017°07'E — — — — 06:50:02.9 143 179 1 06:39 Rise — — 0 122 0.048 0.012SLOVENIALjubljana 46°03'N 014°31'E — — — — 06:49:33.1 138 177 1 06:42 Rise — — 0 121 0.041 0.010UKRAINEKiev 50°26'N 030°31'E — 06:14:32.8 179 212 2 — — 06:51:29.6 154 183 7 06:32:53.8 167 198 4 131 0.020 0.003Odessa 46°28'N 030°44'E 65 05:54:59.7 188 226 2 — — 06:56:02.1 147 178 10 06:24:53.2 167 202 6 129 0.055 0.015

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U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

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JAPANFukuoka 33°35'N 130°24'E — 07:45:30.8 253 204 8 — — — 08:31 Set — — 0 245 0.560 0.444Hiroshima 34°24'N 132°27'E — 07:46:09.3 253 204 6 — — — 08:21 Set — — 0 245 0.437 0.313Kitakyushu 33°53'N 130°50'E — 07:45:34.8 253 204 7 — — — 08:29 Set — — 0 245 0.533 0.414Kobe 34°41'N 135°10'E — 07:47:18.9 255 204 4 — — — 08:10 Set — — 0 244 0.282 0.167Kyoto 35°00'N 135°45'E — 07:47:19.9 255 204 3 — — — 08:07 Set — — 0 244 0.244 0.135Osaka 34°40'N 135°30'E 15 07:47:28.8 255 204 3 — — — 08:08 Set — — 0 244 0.263 0.151

 20 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

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ARMENIAJerevan 40°11'N 044°30'E — 05:54:55.2 191 228 14 — — 07:28:46.8 136 157 24 06:40:26.6 164 193 19 143 0.097 0.035AZERBAIJANBaku 40°23'N 049°51'E — 06:06:42.1 190 221 18 — — 07:47:06.3 132 146 27 06:55:48.3 161 184 23 151 0.103 0.038BAHRAINAl-Manamah 26°13'N 050°35'E — 05:12:54.2 212 263 20 — — 08:07:36.9 111 122 42 06:34:46.9 162 198 33 143 0.304 0.187GEORGIATbilisi 41°43'N 044°49'E — 06:02:23.4 188 223 14 — — 07:27:44.1 138 159 23 06:44:00.4 163 191 19 144 0.081 0.026IRANEsfahan 32°40'N 051°38'E 1597 05:39:09.2 202 242 21 — — 08:05:07.9 119 129 35 06:49:21.6 161 188 30 149 0.205 0.105Qom 34°39'N 050°54'E — 05:45:20.1 199 237 20 — — 07:59:29.3 123 134 33 06:50:04.7 161 188 28 149 0.175 0.084Shiraz 29°37'N 052°33'E — 05:29:33.1 206 250 22 — — 08:12:51.3 114 121 39 06:47:39.6 160 189 33 149 0.254 0.144Tehran 35°40'N 051°26'E 1200 05:50:36.0 197 233 20 — — 08:00:17.1 124 134 32 06:53:28.4 160 186 28 151 0.163 0.075IRAQBasra 30°30'N 047°47'E — 05:22:20.5 206 253 17 — — 07:51:38.7 119 137 36 06:32:42.8 163 198 28 141 0.230 0.125Mosul 36°20'N 043°08'E 223 05:35:35.3 199 241 12 — — 07:29:00.3 131 155 27 06:29:44.8 165 200 20 139 0.146 0.064Baghdad 33°21'N 044°25'E 34 05:26:13.3 203 249 14 — — 07:36:13.3 125 149 31 06:27:42.7 164 201 23 138 0.187 0.092ISRAELJerusalem 31°46'N 035°14'E 809 05:03:35.2 211 265 4 — — 07:11:49.2 125 162 25 06:03:22.8 168 216 15 127 0.237 0.130JORDAN'Amman 31°57'N 035°56'E 776 05:05:18.9 211 264 5 — — 07:13:17.2 125 161 26 06:05:02.3 168 215 15 128 0.231 0.125KUWAITKuwait City 29°20'N 047°59'E 5 05:18:26.0 208 257 17 — — 07:53:37.7 117 135 37 06:31:18.2 163 199 29 141 0.249 0.140LEBANONBeirut 33°53'N 035°30'E — 05:11:29.9 207 259 5 — — 07:11:18.6 128 163 24 06:07:47.9 168 213 14 128 0.202 0.103O

MAN

Masqat 23°37'N 058°35'E — 05:22:39.2 215 260 29 — — 08:45:23.6 98 88 45 07:01:46.4 156 179 42 157 0.386 0.264SAUDI ARABIAMecca 21°27'N 039°49'E — 04:39:09.7 226 290 7 — — 07:28:52.3 110 146 38 05:55:39.1 168 223 23 126 0.411 0.288Riyadh 24°38'N 046°43'E 591 04:59:39.5 217 272 15 — — 07:52:26.8 111 133 41 06:19:04.4 165 208 29 136 0.330 0.210SYRIADamascus 33°30'N 036°18'E 720 05:11:26.5 208 259 5 — — 07:13:14.6 128 162 25 06:08:37.1 168 212 15 129 0.204 0.105TURKEYAnkara 39°56'N 032°52'E 861 05:30:26.7 198 243 3 — — 07:03:00.1 137 171 17 06:14:50.1 168 208 10 129 0.124 0.050Bursa 40°11'N 029°04'E — — — — 06:57:58.6 137 173 14 06:09:29.6 169 211 7 125 0.137 0.058Istanbul 41°01'N 028°58'E 18 — — — 06:57:31.6 138 174 13 06:11:02.0 169 210 6 125 0.126 0.052Izmir 38°25'N 027°09'E 28 — — — 06:56:27.5 133 172 14 06:03:27.1 169 215 5 122 0.173 0.082UNITED ARAB EMIRATESAbu Dhabi 24°28'N 054°22'E — 05:15:24.8 214 263 24 — — 08:26:04.9 104 106 44 06:46:05.4 159 190 38 148 0.346 0.225YEMENSana 15°23'N 044°12'E — 04:30:50.2 233 302 12 — — 07:46:17.3 99 131 48 05:57:41.7 167 224 30 126 0.524 0.406

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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

KAZAKHSTANAlma-Ata 43°15'N 076°57'E 775 06:54:49.2 199 200 26 — — 09:20:06.1 106 80 18 08:10:27.2 152 138 24 198 0.288 0.173KYRGYZSTANBishkek 42°54'N 074°36'E — 06:51:24.1 197 201 26 — — 09:14:46.0 108 84 20 08:05:46.9 152 141 25 194 0.266 0.154MONGOLIAUlaanbaatar 47°55'N 106°53'E 1307 07:26:01.7 218 193 14 — — — 08:42:12.0 153 120 5 230 0.547 0.429TAJIKISTANDusanbe 38°35'N 068°48'E — 06:33:06.6 198 211 29 — — 09:05:31.4 108 88 27 07:51:42.8 152 148 30 185 0.259 0.148TURKMENISTANAschabad 37°57'N 058°23'E — 06:13:24.0 194 220 24 — — 08:26:34.2 120 117 31 07:19:44.9 157 169 30 165 0.171 0.081UZBEKISTANTaskent 41°20'N 069°18'E — 06:41:09.1 195 206 26 — — 09:02:05.5 111 93 24 07:53:38.0 153 148 27 186 0.229 0.123

Annular and Total Solar Eclipses of 2010 21

 Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

AFGHANISTANKabul 34°31'N 069°12'E 1815 06:22:24.6 203 220 32 — — 09:13:24.3 101 77 29 07:51:13.4 151 147 34 185 0.322 0.203BANGLADESHChittagong 22°20'N 091°50'E — 06:45:36.1 233 218 45 — — 10:01:47.9 61 4 17 08:32:53.2 146 104 33 223 0.898 0.825Dacca 23°43'N 090°25'E — 06:44:06.7 230 218 44 — — 10:00:58.7 64 9 18 08:31:36.9 147 107 33 221 0.844 0.770Khulna 22°48'N 089°33'E — 06:40:38.1 230 220 45 — — 10:00:10.2 64 9 19 08:29:41.6 146 107 35 220 0.850 0.776Rajshahi 24°22'N 088°36'E — 06:40:46.9 228 219 44 — — 09:59:24.9 67 14 19 08:29:08.2 147 109 34 218 0.800 0.720BHUTANThimbu 27°28'N 089°39'E — 06:47:54.3 225 214 41 — — 09:59:53.2 71 19 16 08:32:14.3 147 111 31 219 0.751 0.663INDIAAhmadabad 23°02'N 072°37'E 55 05:57:16.2 218 243 42 — — 09:33:32.6 81 42 35 07:52:21.6 148 137 45 191 0.564 0.450Ambasamudram 08°42'N 077°28'E — 05:37:05.7 238 275 54 07:41:56.6 199 178 07:50:19.7 92 68 09:36:28.8 56 360 41 07:46:08.7 145 123 58 201 0.918 0.843 0.406 08m23sAruppukkottai 09°31'N 078°06'E — 05:40:53.1 238 271 54 07:45:49.7 187 165 07:52:47.4 103 77 09:38:26.1 56 360 40 07:49:18.8 145 121 57 203 0.918 0.842 0.260 06m58sBangalore 12°59'N 077°35'E 895 05:46:31.4 233 262 52 — — 09:41:07.4 62 8 38 07:53:29.7 146 123 53 202 0.846 0.774Bombay 18°58'N 072°50'E 8 05:46:43.5 223 254 44 — — 09:34:30.4 75 33 38 07:48:10.7 147 136 49 191 0.645 0.541Calcutta 22°32'N 088°22'E 6 06:37:15.5 229 222 46 — — 09:59:05.9 64 10 20 08:27:34.8 146 108 36 219 0.835 0.761Delhi 28°40'N 077°13'E — 06:23:15.8 214 225 39 — — 09:40:59.6 84 44 27 08:09:10.3 148 129 38 200 0.531 0.413Hyderabad 17°23'N 078°29'E 531 05:59:24.0 228 248 49 — — 09:45:17.8 67 16 33 08:02:00.3 146 122 48 204 0.771 0.687Jaipur 26°55'N 075°49'E — 06:15:42.8 215 230 40 — — 09:39:11.3 83 43 29 08:04:37.8 148 131 40 198 0.542 0.425Kanpur 26°28'N 080°21'E — 06:25:18.6 219 225 42 — — 09:48:12.2 78 33 25 08:14:56.1 147 122 38 206 0.622 0.514Karaikkudi 10°04'N 078°47'E — 05:44:19.1 237 268 54 07:48:32.1 189 164 07:55:38.4 101 74 09:40:04.7 56 360 39 07:52:05.5 145 119 56 204 0.918 0.842 0.278 07m06sKanpur 26°28'N 080°21'E — 06:25:18.6 219 225 42 — — 09:48:12.2 78 33 25 08:14:56.1 147 122 38 206 0.622 0.514Karaikkudi 10°04'N 078°47'E — 05:44:19.1 237 268 54 07:48:32.1 189 164 07:55:38.4 101 74 09:40:04.7 56 360 39 07:52:05.5 145 119 56 204 0.918 0.842 0.278 07m06sKumbakonam 10°58'N 079°23'E — 05:48:10.5 236 264 54 07:53:07.5 168 142 07:57:09.8 122 93 09:41:55.6 57 0 37 07:55:08.5 145 118 54 206 0.917 0.842 0.082 04m02sLucknow 26°51'N 080°55'E 122 06:27:28.0 219 224 42 — — 09:48:58.7 78 33 25 08:16:22.5 147 121 37 207 0.623 0.516Madras 13°05'N 080°17'E 16 05:55:32.4 234 256 53 — — 09:45:13.9 59 3 35 08:00:40.5 145 116 51 208 0.892 0.823Madurai 09°56'N 078°07'E — 05:41:47.0 237 270 54 07:48:24.5 164 140 07:51:42.9 127 102 09:38:56.7 57 1 40 07:50:03.5 145 121 56 203 0.918 0.842 0.053 03m18sNagappattinam 10°46'N 079°50'E — 05:49:17.7 237 263 55 07:51:59.2 197 170 07:59:58.9 93 63 09:42:19.8 56 359 37 07:55:59.5 145 116 54 207 0.917 0.842 0.384 08m00sNagercoil 08°10'N 077°26'E — 05:35:56.2 239 276 54 07:40:10.6 216 196 07:50:02.0 75 50 09:35:44.9 55 358 42 07:45:07.1 145 123 59 201 0.918 0.843 0.669 09m51sNagpur 21°09'N 079°06'E — 06:09:58.8 224 238 46 — — 09:47:09.6 71 23 30 08:07:46.4 146 122 44 205 0.706 0.611New Delhi 28°36'N 077°12'E 212 06:23:04.2 214 225 39 — — 09:41:00.7 84 44 27 08:09:06.0 148 129 38 200 0.532 0.414Palayankottai 08°43'N 077°44'E — 05:38:02.4 239 274 54 07:42:22.2 206 185 07:51:27.6 84 59 09:36:54.5 56 359 41 07:46:55.5 145 122 58 202 0.918 0.843 0.514 09m05sPatna 25°36'N 085°07'E — 06:34:42.2 223 221 43 — — 09:55:27.8 72 22 22 08:23:51.9 147 114 36 213 0.717 0.623Pudukkottai 10°23'N 078°49'E — 05:45:04.3 237 267 54 07:50:10.4 175 150 07:55:13.8 115 88 09:40:29.0 57 0 38 07:52:42.1 145 119 55 205 0.918 0.842 0.130 05m03sPune 18°32'N 073°52'E — 05:48:34.2 224 253 45 — — 09:36:47.1 73 29 37 07:50:44.5 147 134 49 193 0.670 0.570Quilon 08°53'N 076°36'E — 05:34:31.1 238 276 53 — — 09:35:19.6 57 2 42 07:43:58.5 146 126 58 198 0.915 0.842Rajapalaiyam 09°27'N 077°34'E — 05:38:56.2 237 272 54 07:45:56.3 165 143 07:49:29.9 125 102 09:37:32.6 57 1 41 07:47:42.9 145 123 57 201 0.918 0.842 0.060 03m34sSivakasi 09°27'N 077°49'E — 05:39:47.2 238 272 54 07:45:31.2 179 157 07:51:18.4 111 87 09:37:55.7 57 0 40 07:48:24.9 145 122 57 202 0.918 0.842 0.170 05m47sThanjavur 10°48'N 079°09'E — 05:47:02.9 236 265 54 07:52:28.2 166 139 07:56:03.7 124 97 09:41:25.1 57 0 38 07:54:15.8 145 118 55 205 0.918 0.842 0.064 03m36sTirunelveli 08°44'N 077°42'E — 05:37:57.5 238 274 54 07:42:22.4 205 184 07:51:19.6 86 61 09:36:52.7 56 359 41 07:46:51.6 145 122 58 202 0.918 0.843 0.491 08m57sTrivandrum 08°29'N 076°55'E — 05:34:47.5 238 276 54 07:40:33.5 189 170 07:47:49.1 102 79 09:35:20.7 56 0 42 07:44:11.6 146 125 59 199 0.918 0.843 0.279 07m16sTuticorin 08°47'N 078°08'E — 05:39:32.6 239 273 55 07:43:16.8 215 193 07:53:00.3 75 49 09:37:35.4 55 358 41 07:48:09.3 145 121 58 203 0.918 0.843 0.655 09m44sVirudunagar 09°36'N 077°58'E — 05:40:35.9 237 271 54 07:46:17.2 178 155 07:51:52.9 112 88 09:38:20.0 57 0 40 07:49:05.1 145 122 57 202 0.918 0.842 0.158 05m36sVishakhapatnam 17°42'N 083°18'E — 06:14:29.9 231 239 51 — — 09:52:15.1 62 7 28 08:13:35.9 145 112 44 213 0.850 0.777MALDIVESMale 04°10'N 073°30'E — 05:15:21.5 244 296 51 07:20:20.8 245 242 07:31:06.0 49 40 09:23:15.1 54 359 50 07:25:44.2 327 321 65 186 0.919 0.844 0.857 10m45sNEPALKathmandu 27°43'N 085°19'E 1348 06:39:03.6 221 218 41 — — 09:55:01.9 75 27 20 08:25:19.0 147 116 34 213 0.677 0.577PAKISTANFaisalabad 31°25'N 073°05'E — 06:21:25.2 208 223 36 — — 09:28:42.7 92 60 29 08:00:19.0 150 138 36 193 0.422 0.299Islamabad 33°42'N 073°10'E — 06:27:35.4 206 218 34 — — 09:26:10.3 96 65 27 08:01:33.6 150 139 34 193 0.386 0.263Karachi 24°52'N 067°03'E 4 05:48:11.0 213 246 36 — — 09:16:43.8 90 62 39 07:36:19.0 151 152 44 178 0.452 0.330Lahore 31°35'N 074°18'E — 06:24:20.7 209 221 36 — — 09:31:38.9 91 58 28 08:03:32.5 149 136 36 195 0.436 0.314SRI LANKAColombo 06°56'N 079°51'E 7 05:42:06.1 242 275 57 — — 09:37:24.6 51 351 40 07:49:34.8 325 296 58 207 0.902 0.833Jaffna 09°40'N 080°00'E — 05:47:41.8 238 266 56 07:49:32.7 236 209 07:59:42.2 53 22 09:41:17.0 54 356 38 07:54:38.4 325 296 55 207 0.918 0.842 0.975 10m09s

 22 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

BRUNEI DARUSSALAMBandar Seri Beg* 04°56'N 114°55'E 3 07:45:20.8 286 219 35 — — 09:33:42.6 11 291 11 08:42:35.2 329 254 23 245 0.235 0.129BURMA (MYANMAR) Chauk 20°54'N 094°50'E — 06:51:16.7 237 217 45 08:32:31.5 269 223 08:39:46.7 24 336 10:02:59.7 57 357 15 08:36:09.4 327 280 32 227 0.913 0.834 0.460 07m15sLashio 22°56'N 097°45'E — 07:00:15.4 238 212 42 08:37:31.4 272 224 08:44:26.2 23 334 10:04:56.2 57 357 12 08:40:59.0 327 279 27 229 0.912 0.832 0.434 06m55sMagway 20°09'N 094°55'E — 06:50:39.4 238 218 46 08:34:37.1 311 264 08:36:53.6 342 294 10:02:40.2 55 355 16 08:35:44.9 326 279 32 227 0.913 0.834 0.035 02m16sMandalay 22°00'N 096°05'E 77 06:55:30.1 237 215 44 08:34:38.4 263 217 08:42:17.2 31 343 10:03:59.3 57 357 14 08:38:28.2 327 280 30 227 0.913 0.833 0.560 07m39sMaymyo 22°02'N 096°28'E — 06:56:26.6 238 214 43 08:35:27.7 271 225 08:42:27.6 23 334 10:04:09.2 57 357 13 08:38:57.9 327 279 29 228 0.913 0.833 0.434 07m00sMeiktila 20°52'N 095°52'E — 06:53:48.7 239 216 45 08:36:11.6 309 261 08:38:48.2 345 296 10:03:25.3 56 355 14 08:37:29.5 327 279 31 228 0.913 0.834 0.048 02m37sMonywa 22°05'N 095°08'E — 06:53:19.2 236 215 44 08:33:00.2 239 194 08:41:34.8 54 8 10:03:36.0 58 359 14 08:37:18.1 327 281 30 226 0.913 0.834 0.961 08m35sMyingyan 21°28'N 095°23'E — 06:53:15.4 237 216 45 08:33:25.6 264 218 08:41:03.7 30 342 10:03:29.0 57 357 15 08:37:15.0 327 280 31 227 0.913 0.834 0.545 07m38sMyitkyina 25°23'N 097°24'E — 07:01:43.3 235 211 39 08:39:18.9 181 136 08:43:57.9 114 68 10:05:17.4 61 4 11 08:41:38.2 148 102 26 228 0.912 0.832 0.168 04m39sPakokku 21°20'N 095°05'E — 06:52:22.6 237 216 45 08:32:50.8 261 215 08:40:41.1 32 345 10:03:17.7 57 357 15 08:36:46.4 327 280 31 227 0.913 0.834 0.590 07m50sShwebo 22°34'N 095°42'E — 06:55:10.9 236 214 43 08:34:01.8 237 191 08:42:34.0 57 10 10:04:00.9 58 359 14 08:38:18.5 327 280 30 227 0.913 0.833 0.998 08m32sSittwe 20°09'N 092°54'E — 06:45:26.8 236 220 47 08:28:35.5 246 202 08:37:13.7 46 360 10:01:40.3 57 358 18 08:32:55.2 326 281 34 225 0.914 0.835 0.823 08m38sYangon 16°47'N 096°10'E — 06:50:29.3 244 219 49 — — 10:00:46.6 49 345 17 08:34:44.5 326 275 34 229 0.817 0.740Yenangyaung 20°28'N 094°52'E — 06:50:52.8 238 217 46 08:33:12.3 288 241 08:38:36.4 5 318 10:02:48.5 56 355 16 08:35:54.3 326 279 32 227 0.913 0.834 0.221 05m24sCAMBODIAPhnum Pénh 11°33'N 104°55'E 12 07:12:28.0 261 215 46 — — 09:54:22.9 33 321 13 08:40:19.8 327 264 29 238 0.548 0.432LAOSVientiane 17°58'N 102°36'E 170 07:08:17.0 249 213 43 — — 10:02:44.3 46 340 10 08:43:18.7 327 271 27 234 0.738 0.647INDONESIABandung 06°54'S 107°36'E — 07:39:09.0 301 226 49 — — 08:54:53.9 351 266 31 08:18:21.8 326 245 40 248 0.084 0.028Bandung 06°54'S 107°36'E — 07:39:09.0 301 226 49 — — 08:54:53.9 351 266 31 08:18:21.8 326 245 40 248 0.084 0.028Brebes 06°53'S 109°03'E — 07:47:44.1 306 228 46 — — 08:51:05.4 348 262 31 08:20:17.5 326 245 38 249 0.060 0.017Cianjur 06°49'S 107°08'E — 07:36:14.4 300 225 50 — — 08:56:27.3 353 268 31 08:17:52.3 326 245 40 248 0.093 0.033Cibinong 06°27'S 106°51'E — 07:33:39.0 298 224 51 — — 08:59:02.7 354 270 31 08:18:06.2 326 246 40 248 0.106 0.040Cilacap 07°44'S 109°00'E — 07:51:24.6 309 230 45 — — 08:45:04.9 344 259 33 08:18:48.7 326 244 39 249 0.042 0.010Ciledug 06°54'S 108°44'E — 07:45:51.1 305 227 46 — — 08:51:54.9 348 263 31 08:19:51.4 326 245 38 248 0.065 0.019Cimahi 06°53'S 107°32'E — 07:38:42.8 301 226 49 — — 08:55:09.3 351 266 31 08:18:18.1 326 245 40 248 0.085 0.029Ciparay 07°03'S 107°43'E — 07:40:19.7 302 226 48 — — 08:53:43.1 350 265 32 08:18:16.0 326 245 40 248 0.078 0.025Depok 06°24'S 106°50'E — 07:33:25.6 298 224 51 — — 08:59:20.4 354 270 31 08:18:09.9 326 246 40 248 0.107 0.041Garut 07°13'S 107°54'E — 07:42:00.5 303 227 48 — — 08:52:13.0 349 264 32 08:18:13.9 326 245 40 248 0.072 0.022Indramayu 06°20'S 108°19'E — 07:41:22.9 302 226 47 — — 08:56:28.9 351 266 30 08:20:15.3 326 245 39 248 0.084 0.028Jakarta 06°10'S 106°48'E 8 07:32:38.9 297 224 51 — — 09:00:36.9 355 271 31 08:18:30.7 326 246 40 247 0.113 0.044Majalaya 07°03'S 107°45'E — 07:40:31.4 302 226 48 — — 08:53:38.1 350 265 32 08:18:18.7 326 245 40 248 0.078 0.025Medan 03°35'N 098°40'E — 06:49:48.9 265 226 59 — — 09:40:03.6 26 311 25 08:22:21.3 325 261 42 237 0.473 0.352Pringsewu 05°24'S 104°55'E — 07:21:26.8 291 223 54 — — 09:07:18.4 1 277 30 08:17:10.1 326 248 42 246 0.162 0.075Purwokerto 07°25'S 109°14'E — 07:51:23.5 308 229 45 — — 08:46:39.7 345 259 32 08:19:38.5 326 244 38 249 0.045 0.011Semarang 06°58'S 110°25'E — 07:57:16.4 311 231 42 — — 08:45:36.1 343 258 31 08:21:51.7 327 244 36 249 0.035 0.008Serang 06°07'S 106°09'E — 07:29:06.9 296 224 52 — — 09:02:03.3 357 272 31 08:17:41.9 326 247 41 247 0.125 0.051Tangerang 06°11'S 106°37'E — 07:31:43.2 297 224 51 — — 09:00:52.6 355 271 31 08:18:13.9 326 246 40 247 0.116 0.045Tasikmalaya 07°20'S 108°12'E — 07:44:17.3 305 227 47 — — 08:50:37.5 348 263 32 08:18:26.1 326 244 39 249 0.064 0.019Tembilahan 00°19'S 103°09'E — 07:08:07.9 277 221 56 — — 09:27:40.4 14 294 25 08:22:56.7 325 254 40 242 0.305 0.188MACAUMacau 22°14'N 113°35'E — 07:31:47.1 255 208 29 — — — 08:53:51.7 330 270 14 240 0.680 0.580MALAYSIAKuala Lumpur 03°10'N 101°42'E 34 07:01:22.2 269 222 56 — — 09:38:09.1 22 305 23 08:26:10.1 325 258 39 239 0.409 0.286PHILIPPINESCebu 10°18'N 123°54'E — 07:59:55.6 288 219 22 — — 09:39:46.3 14 295 0 08:52:18.7 331 256 10 246 0.246 0.137Davao 07°04'N 125°36'E 27 08:09:57.6 298 224 20 — — 09:28:05.0 4 282 2 08:50:28.2 331 253 11 247 0.144 0.063Manila 14°35'N 121°00'E 15 07:49:03.6 276 214 25 — — — 08:53:56.5 331 261 11 245 0.390 0.267Quezon City 14°38'N 121°03'E — 07:49:06.3 275 214 24 — — — 08:53:59.3 331 261 11 245 0.391 0.268SINGAPORESingapore 01°17'N 103°51'E 10 07:10:08.3 276 220 54 — — 09:32:00.4 16 297 23 08:26:20.2 326 255 38 242 0.329 0.210TAIWANT'aipei 25°03'N 121°30'E 6 07:42:28.6 259 207 20 — — — 08:57:28.7 332 271 5 244 0.653 0.549THAILANDBangkok 13°45'N 100°31'E 16 07:00:30.9 253 217 48 — — 09:58:08.3 41 332 15 08:37:30.0 326 269 32 234 0.673 0.573VIETNAMHa Noi 21°02'N 105°51'E 6 07:16:54.0 249 209 37 — — 10:05:03.0 48 343 6 08:48:07.1 328 273 21 236 0.761 0.673Ho Chi Minh 10°45'N 106°40'E 10 07:17:28.5 264 215 44 — — 09:52:29.6 31 317 12 08:41:20.1 327 262 28 239 0.501 0.381

Annular and Total Solar Eclipses of 2010 23

 Annular Solar Eclipse of 2010 January 15
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Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

CHINABaoshan 25°09'N 099°09'E — 07:05:08.7 237 210 39 08:39:20.5 232 186 08:47:35.0 63 15 10:05:54.6 60 1 9 08:43:28.3 148 100 25 229 0.912 0.831 0.905 08m14sBeijing 39°55'N 116°25'E — 07:32:48.0 234 198 15 — — — 08:52:28.4 153 108 3 239 0.823 0.743Changchun 43°53'N 125°19'E — 07:37:11.8 235 197 7 — — — 08:24 Set — — 0 241 0.568 0.453Chengdu 30°39'N 104°04'E — 07:17:24.1 235 204 30 — — 10:06:53.2 65 9 3 08:48:50.3 150 103 17 232 0.895 0.819Chongqing 29°34'N 106°35'E 261 07:20:53.1 239 204 29 08:46:47.9 239 191 08:54:37.4 60 10 10:07:28.2 61 4 1 08:50:43.1 150 101 15 234 0.910 0.827 0.994 07m50sChuxiong 25°02'N 101°30'E — 07:09:48.9 239 209 37 08:43:13.7 289 240 08:48:22.6 8 318 10:06:30.6 58 358 7 08:45:48.0 328 279 23 231 0.911 0.830 0.226 05m09sDongchuan 26°10'N 103°01'E — 07:13:23.6 239 207 35 08:44:33.0 281 232 08:50:27.5 16 326 10:06:58.7 58 359 6 08:47:30.3 329 279 21 232 0.911 0.829 0.323 05m55sDukou 26°40'N 101°39'E — 07:11:07.4 237 207 35 08:42:19.4 236 189 08:50:25.8 61 12 10:06:45.2 60 2 6 08:46:23.1 148 100 21 231 0.911 0.830 0.963 08m06sEnshi 30°17'N 109°19'E — 07:25:05.8 240 203 27 08:48:57.3 265 215 08:55:57.4 36 345 — 08:52:27.6 330 280 13 236 0.909 0.826 0.588 07m00sFuling 29°42'N 107°21'E — 07:22:05.4 239 204 29 08:47:23.0 249 200 08:55:04.7 51 1 10:07:30.5 61 3 1 08:51:14.2 330 280 15 235 0.909 0.827 0.848 07m42sGuanghua 32°25'N 111°36'E — 07:28:21.0 240 202 23 08:49:39.7 236 187 08:57:12.7 66 16 — 08:53:26.6 151 101 10 237 0.908 0.825 0.910 07m33sGuangzhou 23°06'N 113°16'E 18 07:31:06.3 254 207 29 — — — 08:53:56.2 330 271 13 240 0.706 0.610Harbin 45°45'N 126°41'E 145 07:36:57.9 234 197 5 — — — 08:13 Set — — 0 240 0.432 0.308Heze 35°17'N 115°27'E — 07:32:32.9 239 201 19 08:51:23.5 204 155 08:57:14.3 100 51 — 08:54:19.0 152 103 5 239 0.907 0.823 0.384 05m51sJinan 36°40'N 116°57'E — 07:33:46.4 239 200 17 08:53:35.7 163 115 08:54:58.8 142 93 — 08:54:16.9 153 104 4 240 0.907 0.822 0.018 01m23sJingmen 31°00'N 112°09'E — 07:29:00.2 242 203 24 08:51:44.6 295 245 08:56:07.8 7 315 — 08:53:56.0 331 280 10 238 0.908 0.825 0.186 04m23sJunxian 32°31'N 111°30'E — 07:28:13.9 239 202 23 08:49:37.8 231 182 08:57:06.4 71 21 — 08:53:22.4 151 102 10 237 0.908 0.825 0.830 07m29sKaifeng 34°51'N 114°21'E — 07:31:27.7 239 201 20 08:51:14.6 200 152 08:56:50.9 103 54 — 08:54:02.8 152 103 7 239 0.907 0.823 0.339 05m36sLaiwu 36°12'N 117°42'E — 07:34:32.4 240 200 16 08:51:40.0 208 159 08:57:44.2 97 47 — 08:54:42.2 153 103 3 241 0.907 0.822 0.438 06m04sLeshan 29°34'N 103°45'E — 07:16:23.3 236 205 31 08:46:38.3 178 131 08:50:32.0 120 72 10:07:03.0 63 6 3 08:48:34.9 149 102 18 232 0.910 0.828 0.127 03m54sLianyungang 34°39'N 119°16'E — 07:36:20.7 243 201 16 08:52:52.8 281 230 08:58:32.8 24 332 — 08:55:42.8 333 281 3 242 0.906 0.822 0.374 05m40sLüda 38°53'N 121°35'E — 07:36:55.5 239 199 12 — — — 08:54 Set — — 0 243 0.900 0.818Luzhou 28°54'N 105°27'E — 07:18:51.6 238 205 31 08:45:55.3 240 191 08:53:48.5 59 10 10:07:24.3 61 3 2 08:49:52.4 329 280 17 233 0.910 0.828 0.998 07m53sNanjing 32°03'N 118°47'E — 07:36:36.0 246 202 18 — — — 08:56:18.6 332 279 4 242 0.864 0.787Nanyang 33°00'N 112°32'E — 07:29:29.8 240 202 22 08:50:02.4 233 183 08:57:29.7 70 20 — 08:53:46.4 151 102 9 238 0.908 0.824 0.849 07m27sNeijiang 29°35'N 105°03'E — 07:18:29.1 237 204 31 08:46:07.4 211 163 08:53:03.9 88 39 10:07:16.8 62 5 2 08:49:35.8 150 101 17 233 0.910 0.828 0.521 06m56sPingdingshan 33°45'N 113°17'E — 07:30:21.4 239 201 21 08:50:24.6 221 172 08:57:26.3 82 32 — 08:53:55.7 152 102 8 238 0.908 0.824 0.648 07m02sPuyang 35°42'N 114°59'E — 07:32:02.3 238 200 19 08:52:49.6 170 122 08:55:10.3 134 85 — 08:53:59.6 152 104 6 239 0.907 0.823 0.051 02m21sQingdao 36°06'N 120°19'E — 07:36:50.5 242 201 15 08:51:48.4 248 198 08:59:00.9 58 7 — 08:55:25.0 333 283 2 242 0.906 0.821 0.913 07m13sRizhao 35°27'N 119°29'E — 07:36:19.0 242 201 16 08:51:57.3 257 207 08:58:59.7 49 358 — 08:55:28.8 333 282 2 242 0.906 0.821 0.754 07m02sShanghai 31°14'N 121°28'E 5 07:39:36.2 250 203 16 — — — 08:57:08.3 333 277 3 243 0.813 0.732Shenyang 41°48'N 123°27'E 42 07:37:04.2 237 198 9 — — — 08:38 Set — — 0 242 0.731 0.638Shuicheng 26°41'N 104°50'E — 07:16:56.4 240 206 33 08:48:30.3 320 269 08:49:46.8 338 288 10:07:16.8 58 358 4 08:49:08.1 329 279 19 234 0.910 0.829 0.013 01m17sSuining 30°31'N 105°34'E — 07:19:38.9 236 204 29 08:47:39.8 186 138 08:52:17.5 114 66 10:07:11.6 63 7 2 08:49:58.5 150 102 16 233 0.910 0.827 0.191 04m38sTai'an 36°12'N 117°07'E — 07:34:00.5 239 200 17 08:51:53.6 198 149 08:57:09.7 107 58 — 08:54:31.6 152 104 4 240 0.907 0.822 0.302 05m16sTaiyuan 37°55'N 112°30'E — 07:29:30.8 233 199 19 — — — 08:52:03.2 152 107 6 237 0.828 0.749Tianjin 39°08'N 117°12'E 4 07:33:33.1 236 199 15 — — — 08:53:09.3 153 107 3 240 0.850 0.773Wanxian 30°52'N 108°22'E — 07:23:51.4 239 203 27 08:48:01.4 231 182 08:55:38.8 70 20 — 08:51:50.5 150 101 13 235 0.909 0.826 0.831 07m37sWeifang 36°42'N 119°04'E — 07:35:37.2 240 200 15 08:51:43.9 212 163 08:57:59.7 94 44 — 08:54:51.9 153 104 2 242 0.906 0.821 0.489 06m16sWuhan 30°36'N 114°17'E 23 07:31:44.1 244 203 23 — — — 08:54:57.8 331 279 9 239 0.880 0.805Xiaguan 25°34'N 100°14'E — 07:07:39.1 237 209 37 08:40:37.3 242 194 08:48:48.7 55 6 10:06:17.4 59 1 8 08:44:43.5 328 280 23 230 0.911 0.831 0.938 08m11sXi'an 34°15'N 108°52'E — 07:25:11.8 235 201 24 — — — 08:51:33.7 151 104 11 235 0.872 0.797Xiangfan 32°03'N 112°01'E — 07:28:51.3 240 202 23 08:50:01.1 254 204 08:57:24.0 49 358 — 08:53:42.9 331 281 10 238 0.908 0.825 0.784 07m23sXintai 35°54'N 117°44'E — 07:34:38.0 240 200 17 08:51:27.7 219 170 08:58:11.9 86 36 — 08:54:50.0 153 103 4 241 0.907 0.822 0.604 06m44sXuzhou 34°16'N 117°11'E — 07:34:26.4 242 201 18 08:51:47.3 262 212 08:58:41.5 42 351 — 08:55:14.6 332 282 5 241 0.907 0.822 0.658 06m54sYibin 28°47'N 104°38'E — 07:17:28.7 238 205 32 08:45:20.3 228 180 08:53:07.7 70 21 10:07:18.2 61 4 3 08:49:14.4 149 101 18 233 0.910 0.828 0.811 07m47sYichang 30°42'N 111°17'E — 07:27:51.1 241 203 25 08:50:58.3 288 238 08:56:05.0 13 322 — 08:53:31.6 331 280 11 237 0.908 0.825 0.261 05m07sZaozhuang 34°53'N 117°34'E — 07:34:41.4 241 201 17 08:51:30.4 248 198 08:58:48.1 56 6 — 08:55:09.5 332 282 4 241 0.907 0.822 0.896 07m18sZhaotong 27°19'N 103°48'E — 07:15:23.6 239 206 33 08:44:36.9 258 209 08:52:10.5 40 350 10:07:12.1 60 1 4 08:48:24.0 329 280 19 233 0.910 0.829 0.678 07m34sZhengzhou 34°48'N 113°39'E — 07:30:43.4 238 201 20 08:51:35.0 187 139 08:55:58.5 116 67 — 08:53:46.6 152 103 7 238 0.907 0.824 0.189 04m23sZibo 36°47'N 118°01'E — 07:34:41.9 239 200 16 08:52:19.6 190 141 08:56:46.4 115 66 — 08:54:32.8 153 104 3 241 0.906 0.822 0.205 04m27sZigong 29°24'N 104°47'E — 07:17:59.0 237 205 31 08:45:52.7 212 164 08:52:53.5 87 38 10:07:15.8 62 5 3 08:49:23.3 149 101 17 233 0.910 0.828 0.535 07m01sHONG KONGNew Kowloon 22°20'N 114°10'E — 07:32:45.6 256 208 28 — — — 08:54:11.8 330 270 13 240 0.675 0.574KOREA, NORTHP'yongyang 39°01'N 125°45'E 29 07:39:35.5 242 200 9 08:36:31.0 — — 08:37 Set — — 0 243 0.710 0.613KOREA, SOUTHInch'on 37°28'N 126°38'E — 07:40:52.9 245 201 9 08:36:58.7 — — 08:37 Set — — 0 243 0.701 0.603Pusan 35°06'N 129°03'E 2 07:43:42.1 250 202 8 — — — 08:33 Set — — 0 244 0.613 0.502Seoul 37°33'N 126°58'E 10 07:41:02.7 245 201 9 08:35:26.1 — — 08:35 Set — — 0 243 0.681 0.580

 24 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
January Climate Statistics Percent of 

possible 

sunshine

Calculated 

Cloudiness

Prevailing 

wind

January 

Rainfall

Days 

with 

Rain

Average 

January 

High

Average 

January 

Low

Clear Few Scattered Broken Overcast Obscured % mm °C °C

Central African Republic

Bouar * 32.5 14.4 18.7 30.6 2.9 1 38

Bossangoa * 29.9 21.4 17.1 27.8 3.9 0 36 calm

Bangui * 59 20.4 10.5 21.9 40.8 4.7 1.7 49 calm 25 3 32 20

Mobaye * 16 15 15.5 46 4.5 3 53 calm

Democratic Republic of the Congo

Mbandaka 11.6 10.9 5.8 51.4 18.1 2.2 65

Buta 15.6 11.1 6.7 40 26.7 0 63

Kisangani 50 2.6 5.2 9.1 58.4 23.4 1.3 75 53 6 31 21

Uganda

Soroti * 2 9.8 20.6 58.8 8.3 0.5 65

Arua * 63 2.6 9.3 24.4 63.2 0.5 0 62 12 6 30

Masindi* 5.7 21.1 22.8 45.5 4.9 0 54 5 31 17

Entebbe Airport * 62 1.2 8.9 14.3 52.9 22.8 0 72 S 100 9 29 14

Kampala * 41 0 4.5 8.9 65.2 21.4 0 77 46 9 28 18

Jinja * 3.8 13 22.1 43.5 16.8 0.8 63

Kenya

Kusumu 74 3.6 24.9 22.3 45.2 3.9 0.2 53 E 48 6 29 18

Kitale* 69 7.9 30.8 17.2 40.5 3.1 0.5 48 E - NE 20 8 27 11

Eldoret* 6.9 28 20.5 42.4 2.1 0 49 E - NE 34 3 27 5

Lodwar 85 15.8 32.8 20.5 29.8 1.1 0 38 calm 9 1 36 22

Nairobi* 76 7.5 16.3 20 50.1 6.2 0 57 N - NE 58 4 26 11

Garissa* 67 0.9 2.4 8.7 71.9 16 0 76 S - SE 37 23

Mombasa 71 0 5 26 63.9 5.2 0 67 calm 34 3 33 22

Lamu* (coast) 0 4.3 25.2 69 1.5 0 67 E 1 30 26

Seychelles

Seychelles Airport (Victoria) 40 0 2 15.6 68.9 13.4 0 74 W 379 17 30 24

Maldives

Hanimaadhoo 0.5 51.4 15.6 30.9 1.7 0 41

Male* 67 0 24.7 24.9 44.9 5.5 0 55 75 3 30 25

Kadhdhoo 0 28.2 19.5 43.1 9.2 0 56

India

Minicoy 77 1.7 23.6 36.7 34.5 3.5 0 50 NE 13 1.7 31 23

Kollam (Quilon) 20 1.2

Thiruvananthapuram 72 4.1 29.7 28.8 35.3 2 0 47 SW 23 1.6 32 22

Madurai* 71 11.4 36.5 18 26.9 7.2 0 42 16 1 30 21

Cuddalore 7 27.7 31.3 30.4 3.6 0 45 29 21

Sri Lanka

Colombo 68 3.2 20.5 25.6 43.6 7.1 0 56 NE 58 5 31 22

Jaffna 70 4 29 23

Trincomalee 0 12.5 16.3 59.6 11.5 0 67 NE 116 7 28 24

Bangladesh

Cox's Bazar 69.5 14.5 9.9 5.3 0.8 0 12 9 26 15

Burma

Sittwe* 79 56.5 17.7 13.8 10.8 1.3 0 19 11 <1 28 15

Mindat* 32.2 32.7 15.9 15.9 1.9 1.4 28 4 19 9

Kalewa* 11.1 48.6 24.1 11.1 4.6 0.5 32 2 26 13

Mandalay* 82 51.3 32.6 8.5 6.2 1.4 0 15 4 0.1 29 13

Lashio* 75 19.9 42.1 19.2 14.8 2.6 1.5 31 8 1 25 5

China

Tengchong* 74 11.8 46.8 8.7 28.3 4.4 0 38 16 2.8 16 1

Xichang* 72 25.5 47.1 3.9 16.2 7.4 0 29 6 1.2 16 4

Kunming 69 24.1 32.5 8.4 25.3 9.7 0 38 SW 12 2.2 15 2

Chongqing* 15.8 2 0.7 9.9 71.6 0 80 20 10 10 6

Yichang* 29 21.2 5.7 2.3 21.8 48.8 0.2 68 19 3.8 9 2

Zengzhou* 51 33.4 9.6 3.4 24.6 27 2 51 9 1.8 6 -5

Qingdao* 60 36.8 12.3 5.4 19.2 23.9 2.4 46 11 1.9 3 -4

Table 2.15: Climate statistics for January are given for sites along the annular eclipse path. Location names with a star (*) are in the annular eclipse path.

Explanation of columns:

Percent of possible sunshine: the average number of daily sunshine hours recorded at the station for the month divided by the duration of daylight. 

This is the best estimate of the probability of seeing the eclipse.

Sky condition: Clear means no cloud, few means 1 or 2 oktas (eights) of sky cover, scattered means 3 or 4 oktas, broken means 5 to 7 oktas, and overcast 

means no sky visible at all. Obscured refers to a fog layer through which the sky cannot be seen; it is treated as overcast.

Calculated cloudiness: an average cloudiness derived from the frequency and sky cover in the sky condition columns.

Prevailing wind: the most common direction from which the wind blows during the month.

Rainfall: average monthly rainfall

Days with rain: average number of days in January with 0.2 mm of rain or more.

Average high, low: average daily maximum and minimum temperatures for January.

Table 2.16: Climate Statistics for January along the Annular Eclipse Path

Percent Frequency of Sky Condition

Annular and Total Solar Eclipses of 2010 25

 Annular Solar Eclipse of 2010 January 15
N

S

W E

P1

P2

P3

P4

Kilometers

 0 1000 2000 3000 4000 5000

Annular Solar Eclipse of 2010 Jan 15

Ecliptic Conjunction = 07:12:28.5 TD ( = 07:11:22.4 UT )

 Greatest Eclipse = 07:07:39.0 TD ( = 07:06:33.0 UT )

Eclipse Magnitude = 0.9190 Gamma = 0.4002

Saros Series = 141 Member = 23 of 70

Sun at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 19h47m51.1s

Dec. = -21°07'38.7"

S.D. = 00°16'15.5"

H.P. = 00°00'08.9"

Moon at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 19h47m25.3s

Dec. = -20°46'54.8"

S.D. = 00°14'44.3"

H.P. = 00°54'05.4"

External/Internal

Contacts of Penumbra

P1 = 04:05:27.5 UT

P2 = 06:50:06.7 UT

P3 = 07:22:37.6 UT

P4 = 10:07:35.1 UT

External/Internal

Contacts of Umbra

U1 = 05:13:54.8 UT

U2 = 05:21:15.8 UT

U3 = 08:51:40.3 UT

U4 = 08:59:03.7 UT

Local Circumstances at Greatest Eclipse

 Lat. = 01°37.4'N Sun Alt. = 66.4°

Long. = 069°17.4'E Sun Azm. = 164.9°

Path Width = 333.1 km Duration = 11m07.8s

Constants & Ephemeris

 !T = 66.0 s

 k1 = 0.2725076

 k2 = 0.2722810

!b = 0.0" !l = 0.0"

Eph. = JPL DE200/LE200

Geocentric Libration

(Optical + Physical)

l = 1.48°

b = -0.48°

c = -8.81°

Brown Lun. No. = 1077

FIGURE 2.1: ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH

Greatest Eclipse 

 Sub Solar 

0.20

0.40

0.60

0.80

0.20

0.40

0.60

0.80

07:30 

UT

07:00 

UT

08:30 

UT

08:00 

UT

06:30 

UT

06:00 

UT

06:30 

UT

NASA 2010 Eclipse Bulletin, Espenak & Anderson

 Path of Annular Eclipse 

 26 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Equidistant Conic Projection 

Central Lat,Lng = 3.0 30.0 Semi W,H = 16.0 10.0 Lat 1,2 = 0.0 10.0 

Scale = 27.00 mm/° = 1: 4123000 P Factor = 0.21  2008 Sep 22 15:36:03 

WorldMap v2.00, F. Espenak High Res World Data [WPD1] 

Bujumbura 

Maroua

Bangui

Bouar 

Moundou 

Ndjamena

Beni

Bukavu

Bunia 

Butembo 

Gemena

Isiro 

Kalemie Kananga 

Kikwit

Kinshasa

Kisangani 

Mbandaka

Mbuji-Mayi

Djibouti

Addis

Ababa 

Gonder

Eldoret 

Kisumu

Machakos

Meru

Mombasa 

Nairobi 

Nakuru

Kigali

Kismaayo

Moqadisho 

Nyala 

Arusha

Dar-es-Salaam 

Mwanza

Tabora Tanga 

Zanzibar

Jinja 

Kampala 

Masaka

Mbale 

FIGURE 2.2: PATH OF THE ECLIPSE THROUGH AFRICA

Annular Solar Eclipse of 2010 Jan 15

UGANDA

KENYA

CEN. 

AFR. 

REP.

DEM. 

REP. 

of the 

CONGO

CONGO

TANZANIA

CHAD

SUDAN

ETHIOPIA

Path of Annular Eclipse 

 0.9 

 0.9 

 0.8 

 0.7 

 0.8 

 0.7 

05:30 UT 05:20 UT 07m41s 

11°

05:30 UT

08m32s

25°

05:40 UT

09m08s

34°

Maximum Eclipse Sunrise at 

Central 

Line 

of 

Annular 

Eclipse 

Kilometers

 0 200 400 600 800

NASA 2010 Eclipse Bulletin, Espenak & Anderson

Somalia

Annular and Total Solar Eclipses of 2010 27

 Annular Solar Eclipse of 2010 January 15
 28 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Annular and Total Solar Eclipses of 2010 29

 Annular Solar Eclipse of 2010 January 15
 30 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Equidistant Conic Projection 

Central Lat,Lng = 25.0 93.0 Semi W,H = 28.0 20.0 Lat 1,2 = 15.0 30.0 

Scale = 16.00 mm/° = 1: 6958000 P Factor = 0.21  2008 Sep 23 10:49:50 High Res World Data [WPD1] 

Kabul 

Chittagong

Dacca 

Phnum Pénh

Beijing

Chengdu

Chongqing

Guangzhou

Nanjing Shanghai

Shenyang

Shuicheng 

Wuhan 

Xi'an

Zibo

Ahmadabad 

Mumbai

Bangalore 

Calcutta

Delhi 

Hyderabad 

Kanpur

Madras

Nagpur

Pune

Mashhad 

Alma-Ata

P'yongyang

Soul

Frunze

Male

Yangon

Karachi 

Lahore

Manila

Colombo 

T'aipei 

Dusanbe 

Bangkok 

Taskent 

Ha Noi

Ho Chi Minh 

Hong Kong

BURMA

Kilometers

 0 500 1000 1500

07:30 UT

10m47s

63°

07:40 UT

10m34s

61°

07:50 UT

10m18s

57°

08:00 UT

10m00s

53°

08:10 UT

09m40s

48°

08:20 UT

09m18s

43°

08:30 UT

08m54s

36°

08:40 UT

08m27s

28°

08:50 UT

07m53s

17°

 0.9 

 0.8 

 0.7 

 0.6 

 0.5 

 0.4 

 0.3 

 0.2 

 0.9 

 0.8 

 0.7 

 0.6 

 0.5 

08:30 UT

UT 08:00 

UT 07:30 

Eclipse Ends at Sunset 

Maximum Eclipse at Sunset 

FIGURE 2.6: PATH OF THE ECLIPSE THROUGH ASIA

Annular Solar Eclipse of 2010 Jan 15

NASA 2010 Eclipse Bulletin, Espenak & Anderson

CHINA

INDIA

THAILAND

PAKISTAN

NEPAL

BANGLADESH

Annular and Total Solar Eclipses of 2010 31

 Annular Solar Eclipse of 2010 January 15
 32 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Annular and Total Solar Eclipses of 2010 33

 Annular Solar Eclipse of 2010 January 15
 34 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Annular and Total Solar Eclipses of 2010 35

 Annular Solar Eclipse of 2010 January 15
 36 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Annular and Total Solar Eclipses of 2010 37

 Annular Solar Eclipse of 2010 January 15
 38 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15
Annular and Total Solar Eclipses of 2010 39

 Annular Solar Eclipse of 2010 January 15
 40 Annular and Total Solar Eclipses of 2010

Annular Solar Eclipse of 2010 January 15

 S.D. = 00°14'56.6"

 Dec. = -21°07'44.4"

N

S

E W

Annular Solar Eclipse of 2010 Jan 15

Maximum Eclipse = 07:00:00.0 UT

Moon/Sun Diameter Ratio = 0.9190

000°

180°

090° 270°

Arc-Seconds

 0 1 2 3 4 5

Seconds

 0 2 4 6 8 10

NASA 2010 Eclipse Bulletin, Espenak & Anderson

Seconds

 2 1 0-1-2

Seconds

-2-1 0 1 2

 3

 2

 1

 0

 -1

 -2

 -3

 -3

 -2

 -1

 0

 1

 2

 3

Sun at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 19h47m50.0s

 Dec. = -21°07'45.0"

 S.D. = 00°16'15.6"

 H.P. = 00°00'08.9"

Moon at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 19h47m50.6s

 H.P. = 00°54'52.8"

Geographic Position

Name = Central Line at 07:00 UT

Lat. = 00°49'54.3"N

Long. = 067°52'06.9"E

Elev. = 0.0 m

Eclipse Contacts

C1 = 04:53:13.0 UT

C2 = 06:54:24.7 UT

C3 = 07:05:34.7 UT

C4 = 09:05:25.5 UT

Limb Corrected Contacts

C2* = 06:54:32.6 UT ( 7.9s)

C3* = 07:05:27.2 UT ( -7.5s)

Local Circumstances at Maximum Eclipse

 Sun Alt. = 66.2° Path Width = 335.4 km

Sun Azm. = 157.7° Duration = 11m10.0s

PA(N.Limit) = 151.1° A.Vel. (M:S) = 0.236"/s

Ephemeris & Constants

Eph. = DE200/LE200

 !T = 66.0 s

 k1 = 0.2725076

 k2 = 0.2722810

!b = 0.00" !l = 0.00"

Calculated Center of Figure

!b ́ = -0.24" !l ́ = 0.46"

Topocentric Libration

(Optical + Physical)

l = 1.58°

b = -0.12°

c = -8.84°

 4 3 -3-4 -4-3 3 4

FIGURE 2.15: LUNAR LIMB PROFILE FOR JANUARY 15 AT 07:00 UT

Moon 

Zenith

North

Northern 

Limit

Southern Limit

Second

Contact

Third

Contact

Contact Time 

Correction 

Scale

Contact Time 

Correction 

Scale

Third Contact

Time Correction Curve

Second Contact

Time Correction Curve 

Mean Limb

(Center of Mass)

(Center of Figure)

Mean Limb

True Limb
Annular and Total Solar Eclipses of 2010 41

 Annular Solar Eclipse of 2010 January 15

3. Total Solar Eclipse of 2010 Jul 11

3.1 Introduction

On Sunday, 2010 July 11, a total eclipse of the Sun is 

visible from within a narrow corridor that traverses Earth’s 

Southern Hemisphere (Espenak and Anderson 2006). The path 

of the Moon’s umbral shadow crosses the South Pacific Ocean 

where it makes no landfall except for Mangaia (Cook Islands) 

and Easter Island (Isla de Pascua or Rapa Nui). The path of 

totality ends just after reaching southern Chile and Argentina. 

The Moon’s penumbral shadow produces a partial eclipse that 

is visible from a much larger region covering the South Pacific 

and southern South America (Figure 3.1).

3.2 Umbral Path and Visibility

At 18:15 UT, the Moon’s umbral shadow first makes 

contact with Earth as the path of totality begins in the South 

Pacific. The eclipse track is 179 km wide and the duration of 

totality on the central line is 2 min 42 s. Regrettably, the nearest 

land is either 700 km to the northwest (Tonga) or 1800 km to 

the southwest (New Zealand). It is most unfortunate that the 

dearth of solid land with the track is one of the most noteworthy 

characteristics of this eclipse.

As the shadow travels northeast, the path grows wider 

and the duration increases. At 18:19 UT, the track just misses 

Rarotonga—the largest and most populous of the Cook 

Islands—by just 25 km (Figure 3.2). Rarotonga’s 14,000 inhabitants witness a very deep 0.993 magnitude partial eclipse. 

Two minutes later (18:21 UT), the umbra makes the first of 

its very few landfalls after covering 1450 km of open ocean. 

Mangaia (Auau Enua)—the second largest and most southerly 

of the Cook Islands—is only 15 km south of the central line. 

Its normal population of 1900 will undoubtedly grow with 

many new visitors there to enjoy 3 min 18 s of total eclipse. 

The Sun’s altitude is 14°, the umbra’s velocity is 2.7 km/s, and 

the path width is 200 km. 

Leaving the Cook Islands behind, the umbra passes 

tantalizingly close to the Society Islands of French Polynesia 

(Figure 3.3). Alas, such exotic destinations as Moorea, Bora 

Bora, and Tahiti all lie outside the eclipse track. The southeastern coastline of Tahiti lies just 20 km beyond the northern 

limit and gets a 0.996 magnitude partial eclipse at 18:28 UT. 

In comparison, Papeete—Tahiti's capital (pop. 131,000) on 

the northwest coast—experiences a 0.984 magnitude partial. 

Because of its close proximity to the path, one or more eclipse 

cruises will be based out of Tahiti. While they cannot offer the 

rigid stability of a land-based observing site, the mobility of 

cruise ships can increase the possibility of avoiding clouds.

After the Society Islands, the Moon’s shadow passes 

over a number of small atolls of the Tuamotu Archipelago 

(Figure 3.4), only a few of which are inhabited. Hikueru—a 

10 × 15 km oval-shaped atoll—has a population of ~125 and 

a small territorial airport. It may be suitable for small expeditions who can expect the total phase to last 4 min 20 s. One 

of the more isolated atolls of the Tuamotus is Tatakoto. The 

4 × 14 km wide islet has a population of ~250 and is within 

20 km of the central line. The duration of totality is 4 min 35 s 

with the Sun 36° above the horizon (18:48 UT).

The umbra now embarks on a lonely trek with no landfall 

for the next 1.4 h as it races 3300 km across the South Pacific. 

During this period, the axis of the Moon’s shadow passes closest to the center of Earth (gamma = –0.6788) as the instant of 

greatest eclipse is reached at 19:33:31 UT (latitude 09° 45′S, 

longitude 121° 53′W). The maximum duration of totality is 

5min 20s, the Sun’s altitude is 47°, the path width is 258 km, 

and the umbra’s velocity is 0.60 km/s. 

The seclusion of the lunar shadow’s solitary journey is 

finally interrupted at 20:11 UT when it encounters Easter Island, a.k.a. Isla de Pascua or Rapa Nui, as the Polynesians call 

it (Figure 3.5). Renowned as one of the world’s most isolated 

inhabited islands, Easter Island is 3,600 km west of Chile. It 

possesses 887 enormous monolithic statues created by the 

native Rapanui people hundreds of years ago. Dominated by 

three extinct volcanoes, the triangular-shaped island measures 

approximately 11 × 23 km. From the capital, Hanga Roa, totality lasts 4 min 41 s, with the Sun at an altitude of 40°. The 

3,800 inhabitants of the isle are accustomed to tourism, but 

the eclipse is expected to bring record numbers to this remote 

destination.

After Easter Island, the Moon’s umbra covers another 

3700 km of ocean during 38 min before beginning its final 

landfall along the rugged shores of southern Chile at 20:49 UT 

(Figure 3.6). The shadow is now an extremely elongated ellipse traveling at a velocity of 8.7 km/s and accelerating. The 

central line duration is 02 min 57 s with the Sun 5° above 

the horizon. However, the desolate, fjord-lined coast of the 

Chilean Archipelago affords no suitable locations for eclipse 

observing. Quickly crossing the Andes, the shadow enters 

Argentina where it encounters El Calafate, a tourist village of 

8000 located on the southern shore of Lake Argentino. The 

Sun’s altitude is only 1° during the 2 min 47 s total phase, 

but the lake may offer an adequate line-of-sight to the eclipse 

hanging just above the Andes’s silhouetted skyline.

The path ends 130 km southeast of El Calafate as the umbra slips off Earth’s surface and returns to space at 20:52 UT. 

Over the course of 2 h 39 min, the umbra travels along a track 

approximately 11,100 km long that covers 0.48% of Earth’s 

surface area. It will be 29 months before the next total solar 

eclipse occurs on 2012 Nov 13.

3.3 Maps of the Total Eclipse Path

Maps of the Jul 11 total eclipse path are given in Figures 3.1 through 3.6. Figure 3.1 is an orthographic projection 

map of Earth showing the path of penumbral (partial) and umbral (total) eclipse. The limits of the Moon’s penumbral shadow 

define the region of visibility of the partial eclipse. The much 

narrower path of the umbral shadow defines the zone where 

the total eclipse is visible. For a more detailed description of 

Figure 3.1, see Section 1.2.

Annular and Total Solar Eclipses of 2010 43

Total Solar Eclipse of 2010 July 11
Figures 3.2 through 3.6 offer more detailed maps of the 

path of totality wherever it crosses land. A complete description 

of these figures can be found in Sections 1.3 and 1.4.

3.4 Total Eclipse Elements and Path Tables

Tables 3.1 through 3.7 give elements for the eclipse, as 

well as basic characteristics of the path of totality. The geocentric ephemeris for the Sun and Moon, various parameters, 

constants, and the Besselian elements (polynomial form) are 

found in Table 3.1. All external and internal contacts of penumbral and umbral shadows with Earth are listed in Table 3.2. 

They include TDT and geodetic coordinates with and without 

corrections for ∆T.

The path of the umbral shadow is delineated at 5min 

intervals (in Universal Time) in Table 3.3. Coordinates of 

the northern limit, the southern limit, and the central line are 

listed along with the Sun’s altitude, path width, and central line 

duration of totality. Table 3.4 presents a physical ephemeris for 

the umbral shadow and includes the topocentric ratio of the 

Moon and Sun’s apparent diameters, the eclipse obscuration, 

the path width, the dimensions of the umbral shadow, and its 

ground velocity.

Table 3.5 gives the local circumstances for each central 

line position listed in Tables 3.3 and 3.4. Table 3.6 presents 

topocentric values from the central path for the Moon’s horizontal parallax, semi-diameter, relative angular velocity with 

respect to the Sun, and libration in longitude. In addition, 

corrections to the path limits due to the lunar limb profile are 

listed. A detailed description of these tables can be found in 

Section 1.5.

3.5 Total Eclipse Local Circumstances Tables

Local circumstances for a number of cities, islands, and 

places in the Pacific Ocean and South America are presented 

in Table 3.7. The table gives the local circumstances at each 

contact and at maximum eclipse for every location. The coordinates are listed along with the location’s elevation (in meters) 

above sea level. The Universal Time of each contact is given 

to a tenth of a second, along with position angles P and V and 

the altitude of the Sun. Two additional columns are included 

if the location lies within the path of totality. The “umbral 

depth” is a relative measure of a location’s position with respect 

to the central line and path limits. The last column gives the 

duration of totality. For a more information about these tables, 

see Section 1.6.

3.6 Total Eclipse Lunar Limb Profile

Along the 2010 total eclipse path, the Moon’s topocentric 

libration (physical plus optical) in longitude ranges from 

l=–2.5° to l=–3.8°; thus, a limb profile with the appropriate 

libration is required in any detailed analysis of contact times, 

central durations, etc. A profile with an intermediate value, 

however, is useful for planning purposes and may even be 

adequate for most applications. The lunar limb profile presented in Figure 3.7 includes corrections for center of mass 

and ellipticity (Morrison and Appleby 1981). It is generated for 

19:30 UT, near the time of greatest eclipse. The umbral shadow 

is then located in the Pacific Ocean at latitude 19° 18.6′S and 

longitude 121° 59.4′W. The Moon’s topocentric libration is 

l=–3.13°, and the topocentric semi-diameters of the Sun and 

Moon are 944.0 and 998.7 arcsec, respectively. The Moon’s 

angular velocity with respect to the Sun is 0.342 arcsec/s. 

The times of the four eclipse contacts from this location 

appear to the lower right in Figure 3.7. The limb-corrected 

times of second and third contacts are listed with the applied 

correction to the center of mass prediction. The time correction curves can be used for estimating corrections to the 

times of second and third contacts as a function of the position angle of the contact. More information on this topic and 

a detailed description of the limb profile figure can be found 

in Section 1.8.

3.7 Weather Prospects for the Total Eclipse

3.7.1 Weather Overview

The 2010 total eclipse comes at the depths of the Southern 

Hemisphere winter, ordinarily a time of frequent storms and 

alternating high- and low-pressure systems that bring a lot of 

changeable weather, winds, and cloudiness. Fortunately, latitude comes to the rescue for the first half of the shadow track, as 

it travels in and north of the belt of high-pressure anticyclones 

that girdle Earth at about 30°S (Figure 3.8). This high-pressure 

belt is a region where the air descends from higher levels in the 

atmosphere, warming and drying by adiabatic compression. 

It is a zone of mostly sunny skies and pleasant temperatures, 

akin to the Caribbean in the Northern Hemisphere winter, but 

it is not without its temperamental weather. Cold fronts from 

storms in the “Roaring Forties”—latitudes between 40°S and 

60°S—are able to move into anticyclonic barrier, bringing 

showery weather and cloudy skies to the eclipse path when 

they do. Beyond Easter Island, the eclipse track dips into the 

Roaring Forties, and cloudiness—at least over the eastern 

Pacific and the coast of Chile—becomes much heavier.

In addition to passing cold fronts and the impact of the 

Roaring Forties, there is a semi-permanent feature of southern 

meteorology known as the South Pacific Convergence Zone 

(SPCZ). The SPCZ is a band of low-level wind convergence 

lying over the warmest waters of the southwest Pacific and so, 

like the ITCZ along the equator, is a region of frequent showers and thundershowers along with the associated cloudiness. 

In July, alas, the SPCZ lies at the northern limit of its annual 

range, stretching from the Solomon Islands near New Guinea, 

across Samoa and the Cook Islands. In recent years, perhaps 

in response to global climate changes, the SPCZ has tended 

to move north and east, to a position that more directly affects 

the eclipse track. To avoid the influences of the low-latitude 

storms and the thunderstorms of the SPCZ, eclipse watchers 

must head to the north and east—to the extremities of French 

Polynesia or beyond (Figure 3.9).

In spite of the weather factors that promote cloudiness 

along the eastern and western extremities of the eclipse path, 

 44 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
the western Pacific is actually in the midst of its seasonal 

dry spell during July. Closer to the South American coast, 

just the opposite is true, though at Easter Island, the difference in precipitation between the wet and dry seasons is less 

pronounced than at Tahiti and the Cook Islands (Figure 3.10). 

At the end of the path in Argentina, where winter influences 

would be expected to bring the most difficult conditions, the 

Andes Mountains act as a very effective barrier to the Pacific 

storms and the weather is quite promising instead.

Islands in the Cook Islands and French Polynesia are either 

mountainous volcanic peaks (Tahiti, Mangaia, and also Easter 

Island) or low, flat atolls (Tuamotus). The latter are too small 

and low to affect the flow from the sea, so the weather observations from those sites reflect the conditions on the water. On 

the other hand, the mountainous islands impose a considerable 

orographic modification on wind, cloud, and precipitation—

generally to increase cloud and rainfall and divert the winds. 

The humid tropical air is always ready to form clouds if lifted 

by any of several processes. Large islands are darker than 

the sea, and warm more readily in sunlight. Warm air, being 

buoyant, rises upward, forming clouds at some small distance 

above the surface. Winds blowing onto the land are compelled 

to rise as they encounter the mountainous topography, adding 

to the impact of the solar heating, and usually cloaking the 

mountain ridges and peaks with a cap of cloud, especially in 

the afternoon hours. 

The reverse process occurs at night in the case of solar 

heating, and on the lee side of the terrain in the case of orographic lifting. Winds blow downslope on crossing the highest 

point of the terrain, so clouds dissipate and rain ends. The 

whole process is complicated by the complexities of the topography, but in general, the lee side of the mountains on Mangaia 

and Easter Island will have a slightly greater tendency to sunny 

weather. The degree of impact will depend on the height and 

lie of the terrain, and on both islands the cloud-producing 

processes will dominate those that dry out the air. 

3.7.2 Cook Islands

Mangaia, the only Cook Island within the eclipse path 

(Figure 3.2), has a latitude that puts it securely within the influence of the SPCZ though the Convergence Zone has a mixed 

personality, sometimes quiet and barely evident, other times 

especially active and full of convection and rain. Cold fronts, 

migrating northward from lower latitudes, reinforce the SPCZ 

or attend the islands with their own independent weather. It 

is easy to be pessimistic about the weather prospects, but the 

climate statistics for Mangaia give reason for some optimism: 

July is the driest month at nearby Rarotonga (Figure 3.10), with 

an average of about 100 mm of rainfall and Mangaia follows the 

same pattern. Mangaia’s cloudiness is similar to that of Rarotonga (Table 3.8) with an average cloud cover of 64% calculated 

from the observed frequency of the various cloud categories. 

Rarotonga reports an average sunshine amount of 52% and it 

is probably only slightly less than this at Mangaia. 

Mangaia Island is 9 km in diameter, rugged, with a modest 170 m peak in its interior. It is mostly tree-covered in its 

interior and so combines the cloud-producing features of low 

albedo and a rising topography, although this forcing is modest compared to Tahiti. On most days when the SPCZ is weak 

or distant and the skies are sunny, the afternoon convective 

clouds are small and confined to the interior. Clouds such as 

these will dissipate quickly in the cooling that accompanies 

an eclipse. When more organized weather visits, the small 

dimensions of the island and limited terrain are unlikely to 

have much influence, either to reinforce the rainfall on the 

windward side or to dissipate the clouds to leeward. Whatever 

influence the island can muster will be confined to the lowest 

cloud levels. There is no prevailing wind at Mangaia, but the 

stronger weather systems tend to come with easterlies and 

southeasterlies. 

On quiet days, rains on Mangaia tend to come in the 

afternoon after a sunny morning, and may be quite heavy for 

a brief time. Daylong rains are more unusual, but do occur 

from time to time. This diurnal pattern favors the eclipse, 

which occurs in the morning hours, before maximum heating 

and maximum cloudiness. Winds blowing against Mangaia 

(on the windy days—one-third of the wind observations are 

calm) may cause the formation of an arc of cloudiness offshore 

where the winds converge and are diverted to flow around the 

island. These arc clouds (much like the bow wave of a boat) 

will likely remain offshore during an eclipse. 

3.7.3 Tahiti and French Polynesia

At Tahiti, July is the second-driest month (Figure 3.10) and 

at Hereheretue, in the Tuamotu Islands, July is the driest. While 

this pattern is similar to that at Rarotonga, the amount of rain in 

July is about half that in the more southeasterly Cook Islands. 

The drier weather is reflected in the cloud cover statistics, with 

average cloudiness dropping to between 44% and 53% across 

much of Polynesia, a figure 10% to 20% less than in the Cook 

Islands, in large part due to the reduced influence of the SPCZ. 

Sunshine statistics are also generous, though somewhat erratic, 

with very encouraging measurements of 65% to 70% of the 

maximum possible in most of the islands. 

Periods of bad weather are often associated with the passage of cold fronts that arrive from the southwest, sometimes 

lingering for several days. The stronger fronts have a tendency 

to stall near the islands and the eclipse track. Even though 

Tahiti is in the midst of its dry season, a persistent frontal 

band can drop large amounts of rain for several days in a row. 

Should a cold front occur on eclipse day, the only escape would 

be to sail out from under it, most likely by heading eastward 

down the path.

With only a limited number of places to stay on Mangaia 

and the atolls of French Polynesia, most southwest Pacific observers will choose to watch this eclipse from shipboard. From 

a climatological perspective, ships should place themselves as 

far eastward along the track as schedule permits. This puts the 

SPCZ well behind and increases the probability that temperatezone cold fronts will be left behind (Figure 3.9). Cloud systems 

tend to become smaller and more disorganized in the more 

northerly latitudes, and thus easier to avoid when eclipse day 

arrives. Closer to Tahiti, the SPCZ cloudiness will have to 

Annular and Total Solar Eclipses of 2010 45

Total Solar Eclipse of 2010 July 11
be watched cautiously, though the island typically marks the 

easternmost extent of its influence.

In satellite imagery, high- and mid-level clouds associated 

with the SPCZ tend to move from west to east in the upper 

level flow. Low-level clouds usually move in the opposite 

direction, but are much more variable and cannot be counted 

on from one day to the next; frequently they just hang around 

without seeming to go anywhere. When strong highs pass to 

the south of the island, the pressure gradient is compressed 

and stronger than normal easterly trade winds—known as a 

Mara’umu—can bring winds of 50 km/h and 3 m wave heights 

in the seas, sometimes lingering for days or even over several 

weeks. These enhanced trade winds bring heavy rains to the 

windward side of Tahiti, but such orographic effects will not 

be a factor along the eclipse track as there are no islands with 

a significant topography under the lunar shadow’s path in 

French Polynesia. 

Frontal clouds will come up from the south or southwest, 

usually in the form of bands that are 100 or 200 km wide. On 

top of this complicated pattern is the tendency for clouds—

especially low-level clouds—to form and dissipate over one- to 

three-hour periods, making prediction from satellite imagery 

very difficult. “Chasing” an opening in the clouds may be a 

frustrating experience so positioning the ship where climatology is most favorable at the start will make eclipse-day planning a less hectic event. Positions to the northeast along the 

path will also increase the eclipse duration. Cyclones should 

not be a problem, as the hurricane season runs from November 

to March.

When the SPCZ keeps to the south (its more usual position) and cold fronts are not in the area, westward-moving 

cloud clusters known as “easterly waves” may be the only 

weather feature to watch for. Easterly waves are more-or-less 

circular areas of convection with varying dimensions, up to 

200 km or thereabouts. They may bring heavy overcast or 

scattered thundershowers, but are readily seen and predicted 

in satellite images. 

A careful watch on the satellite images will show “zones” 

of descending air where both high and low-level clouds tend 

to disappear. These zones will not be very distinct, and they 

will not be completely free of cloud, but once identified, can 

be counted on for favorable circumstances for a half-day or 

longer. From the ship’s deck, such areas will have smaller 

convective clouds (primarily shallow cumulus), and thinner 

high-level cirrus. 

A ship’s mobility will increase the chances of seeing the 

eclipse by an estimated 5%, limited, in large part, because 

cloud patterns are not easily predicted. The biggest advantage 

to be given to a shipboard site is the ability to move east of the 

Tuamotu Islands to tap the best climatology along the track. 

For those eclipse watchers who are determined to settle on 

land, the Tuamotus offer a few places with airports, including 

Hao, Hikueru, Tatakoto, and Anaa. Other islands will have to 

be reached by boat, a prospect that greatly extends the travel 

time.

3.7.4 Tropical Cyclones

In the southern Pacific, the tropical cyclone season runs 

from November to April. For regions along the eclipse path, 

the frequency is relatively low, with about nine storms per year 

on average across the whole basin east of Australia. While 

statistics are somewhat poor, the Cook Islands near Rarotonga 

(including Mangaia) experience one tropical storm every seven 

years, while in Tahiti they are about half that rate. In El Niño 

years, cyclones tend to be widespread between 10° and 30° S 

latitude, from Australia to 130°W, which pretty much covers 

the whole track through the Cook Islands and Polynesia. In La 

Niña years, cyclones tend to be fewer in number, forming and 

traveling much closer to the Australian coast. In any event, the 

possibility of a tropical cyclone is virtually nil during July.

3.7.5 Easter Island

Easter Island lies on the south side of the anticyclonic 

belt that circles Earth at 30° S latitude, and as a consequence, 

is much more exposed to the influence of the westerlies and 

storms in the Roaring Forties. In July, Easter Island is in its 

wet winter season (Figure 3.10) and sunshine is at a premium. 

Still, it is an exotic destination, and the sunshine statistics show 

a percentage of the maximum possible (50%) that is similar 

to that at Rarotonga (and Mangaia) in the Cook Islands (Table 

3.8). The prospect of stunning photographs of the eclipse over 

the Moai has tremendous appeal. 

Easter Island has three large volcanoes and a number of 

smaller ones, and the cloud on the mountaintops is a persistent 

feature of the winter weather. The weather is extremely changeable when it is inclined to be cloudy, and there is no advantage 

in chasing from one site to the other at the last minute to find a 

sunny haven. There is a strong convective element to the cloud 

types, even when large weather systems reach the island, and 

because of this, clouds can form and dissipate within minutes. 

On sunny days, clouds will tend to form in the afternoon, but 

will dissipate as the eclipse approaches. 

Given the nature of the cloudiness described above, there 

are still a few tricks to help pick a successful eclipse site. Do 

not go uphill unless the day is spectacularly sunny. Especially, 

do not locate on the upwind side of a volcanic hill. Coastal sites 

exposed to the wind may have a little less cloudiness if the wind 

is not too strong, as the cooler air from the sea will suppress 

the immediate formation of cloud as it reaches land. Sites in the 

lee of the larger volcanoes may be a little sunnier if the weather 

is not too thick, but usually, the clouds will form on the slopes 

and blow downwind; the flanks of the larger peaks may offer 

safer sites. There is no strong prevailing wind—they can come 

from any quarter according to the weather of the day. 

Given all of the complexities of the wind and weather, 

the south coast seems like the safest bet, perhaps at Tongariki 

where the Moai offer great visual appeal. With easterly or 

westerly winds, the village at Hanga Roa is promising, but 

southerlies or northerlies will carry clouds from the peaks of 

Terrevaka or Rana Kao onto the town. Northerlies at Tongariki 

will have a slight downslope flow, which tends to dry the air 

 46 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
out a bit, but the volcano Pakaiki lies just to the east and flow 

from its peak will have to be watched carefully. The beach 

at Anakena is promising under a northerly onshore flow, and 

may be one of the best sites for a large group because of the 

facilities available there. 

Unless there is a large and active weather system over the 

island on eclipse day, there will certainly be mixtures of sun 

and cloud that will make site selection difficult. If mobility is 

an option, eclipse watchers should wait until the last possible 

moment to assess the character of the cloud and wind before 

picking a viewing site.

3.7.6 South America

The Chilean Archipelago, while imbibed with towering 

forested slopes that fall into dark mysterious water, is also 

exposed to the full force of the westerlies and nearly devoid 

of community, thus making for a poor or impossible eclipse 

site. Once across the Andes however, and into Argentina, the 

weather improves significantly and the eclipse comes to its 

sunset ending near the resort town of El Calafate. The Andes 

block the flow of the westerlies, stripping them of their moisture and clouds, and leaving a drier and sunnier airflow to 

descend onto the plains of southern Argentina. No sunshine 

data are available for Argentina, but cloud-cover statistics 

(Table 3.8) show an encouraging average cloudiness for July 

at El Calafate of 55%. While this is about 10% higher than 

Tahiti, the data are similar to the values in the Cook Islands 

and parts of Polynesia. 

The winter season brings cool temperatures, although 

nothing like the winters in the Northern Hemisphere. Average 

highs reach 6°C and average lows descend to a chilly (for the 

Southern Hemisphere) –5°C. 

Because the Sun is close to setting during the eclipse, sight 

lines will have to be carefully arranged to avoid the distant 

mountains. That will be a tough challenge, as the eclipsed Sun 

is only 1° above the horizon, although the presence of several 

lakes aligned toward the west and northwest will help. The long 

view through the atmosphere will increase the probability that 

even a small amount of cloudiness will block totality. 

3.7.7 Summary

French Polynesia is the clear-cut choice for the best 

weather prospects, but land-based sites are scarce and most 

observers will opt for a shipboard eclipse experience. Mangaia 

and Easter Island are the largest islands in the track, with moreor-less the same chances of sunshine—about 50%. If observing 

requirements dictate solid ground, then the choice is among one 

of these or the few reachable islands in the Tuamotus. Easter 

Island has, by far, the most developed infrastructure and the 

most convenient travel, but the small French Polynesian atolls 

offer the best weather. Easter Island, of course, has that aura 

of mystery that will more than compensate for the limited 

weather prospects.

Argentina is not a good choice if the eclipse alone is your 

goal. The very low altitude of the Sun, mountain-toothed 

horizon, and modest chances of sunshine suggest that more 

tropical destinations would be better.

Annular and Total Solar Eclipses of 2010 47

Total Solar Eclipse of 2010 July 11
TABLE 3.1

ELEMENTS OF THE TOTAL SOLAR ECLIPSE OF 2010 JULY 11

Equatorial Conjunction: 19:52:01.30 TDT J.D. = 2455389.327793

(Sun & Moon in R.A.) (=19:50:55.11 UT)

Ecliptic Conjunction: 19:41:33.49 TDT J.D. = 2455389.320527

(Sun & Moon in Ec. Lo.) (=19:40:27.31 UT)

Instant of 19:34:37.63 TDT J.D. = 2455389.315713

Greatest Eclipse: (=19:33:31.45 UT)

Geocentric Coordinates of Sun & Moon at Greatest Eclipse (JPL DE200/LE200):

Sun: R.A. = 07h23m57.621s Moon: R.A. = 07h23m15.844s

Dec. =+22°02'10.95" Dec. =+21°22'29.30"

Semi-Diameter = 15'43.94" Semi-Diameter = 16'26.67"

Eq.Hor.Par. = 08.65" Eq.Hor.Par. = 1°00'20.87"

∆ R.A. = 10.187s/h ∆ R.A. = 154.225s/h

∆ Dec. = -20.41"/h ∆ Dec. = -515.89"/h

Lunar Radius k1 = 0.2725076 (Penumbra) Shift in ∆b = 0.00"

Constants: k2 = 0.2722810 (Umbra) Lunar Position: ∆l = 0.00"

Geocentric Libration: l = -3.2° Brown Lun. No. = 1083

(Optical + Physical) b = 0.9° Saros Series = 146 (27/76)

c = 6.6° nDot = -26.00 "/cy**2

Eclipse Magnitude = 1.05804 Gamma =-0.67877 ∆T = 66.2 s

Polynomial Besselian Elements for: 2010 Jul 11 20:00:00 TDT (=t0)

n x y d l1 l2 μ

0 0.0740999 -0.7170312 22.0357037 0.5344427 -0.0116561 118.614319

1 0.5572523 -0.1366581 -0.0053410 -0.0000908 -0.0000904 15.000069

2 -0.0000276 -0.0001121 -0.0000052 -0.0000124 -0.0000123 0.000002

3 -0.0000090 0.0000024 0.0000000 0.0000000 0.0000000 0.000000

Tan ƒ1 = 0.0045988 Tan ƒ2 = 0.0045759

At time t1 (decimal hours), each Besselian element is evaluated by:

a = a0 + a1*t + a2*t2 + a3*t3 (or a = ∑ [an*tn]; n = 0 to 3)

where: a = x, y, d, l1, l2, or μ

t = t1 - t0 (decimal hours) and t0 = 20.00 TDT

The Besselian elements were derived from a least-squares fit to elements

calculated at five uniformly spaced times over a 6-hour period centered at

t0. Thus, they are valid over the period 17.00 ≤ t1 ≤ 23.00 TDT.

All times are expressed in Terrestrial Dynamical Time (TDT).

Saros Series 146: Member 27 of 76 eclipses in series.

 48 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
TABLE 3.2

SHADOW CONTACTS AND CIRCUMSTANCES

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

∆T = 66.2 s

=000°16'35.5"

Terrestrial

Dynamical Ephemeris True

Time Latitude Longitude† Longitude*

h m s

External/Internal

Contacts of Penumbra: P1 17:10:43.8 11°38.9'S 161°30.4'W 161°13.8'W

P4 21:58:20.5 36°47.3'S 075°48.4'W 075°31.9'W

Extreme

North/South Limits

of Penumbral Path: N1 18:00:45.9 04°40.3'N 179°17.7'E 179°34.3'E

S1 21:08:25.8 20°55.6'S 054°37.4'W 054°20.8'W

External/Internal

Contacts of Umbra: U1 18:16:18.3 26°18.4'S 171°08.5'W 170°51.9'W

U2 18:19:36.0 27°25.4'S 171°23.1'W 171°06.5'W

U3 20:49:25.7 51°22.0'S 071°23.4'W 071°06.8'W

U4 20:52:47.2 50°21.7'S 071°03.1'W 070°46.5'W

Extreme

North/South Limits

of Umbral Path: N1 18:17:01.6 26°02.9'S 171°27.3'W 171°10.7'W

S1 18:18:54.5 27°40.6'S 171°04.8'W 170°48.2'W

N2 20:52:03.3 50°07.6'S 070°36.2'W 070°19.6'W

S2 20:50:08.0 51°35.5'S 071°50.3'W 071°33.7'W

Extreme Limits

of Central Line: C1 18:17:56.7 26°51.4'S 171°16.1'W 170°59.5'W

C2 20:51:07.0 50°51.4'S 071°12.4'W 070°55.8'W

Instant of

Greatest Eclipse: G0 19:34:37.6 19°44.9'S 122°09.1'W 121°52.5'W

Circumstances at

Greatest Eclipse: Sun’s Altitude = 47.1° Path Width = 258.6 km

Sun’s Azimuth = 13.5° Central Duration = 05m20.2s

_____________________________________________________________________________

† Ephemeris Longitude is the terrestrial dynamical longitude assuming a

uniformly rotating Earth.

* True Longitude is calculated by correcting the Ephemeris Longitude for

the non-uniform rotation of Earth.

(T.L. = E.L. + 1.002738*∆T/240, where ∆T(in seconds) = TDT - UT)

Note: Longitude is measured positive to the East.

Because ∆T is not known in advance, the value used in the predictions is an

extrapolation based on pre-2009 measurements. The actual value is expected

to fall within ±0.3 seconds of the estimated ∆T used here.

Annular and Total Solar Eclipses of 2010 49

Total Solar Eclipse of 2010 July 11
TABLE 3.3

PATH OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

∆T = 66.2 s

Universal Northern Limit Southern Limit Central Line Sun Path Central

Time Latitude Longitude Latitude Longitude Latitude Longitude Alt Width Durat.

° km

Limits 26°02.9'S 171°10.7'W 27°40.6'S 170°48.2'W 26°51.4'S 170°59.5'W 0 179 02m42.4s

18:20 20°50.8'S 157°59.3'W 23°57.1'S 161°17.4'W 22°19.8'S 159°27.6'W 12 197 03m15.1s

18:25 18°54.4'S 152°08.8'W 21°29.5'S 154°04.9'W 20°10.7'S 153°03.5'W 19 209 03m37.8s

18:30 17°44.8'S 147°59.6'W 20°10.9'S 149°29.3'W 18°57.0'S 148°42.5'W 24 219 03m55.0s

18:35 16°58.8'S 144°38.3'W 19°20.7'S 145°54.6'W 18°09.2'S 145°15.0'W 28 227 04m09.5s

18:40 16°28.2'S 141°46.0'W 18°47.8'S 142°54.2'W 17°37.6'S 142°19.0'W 32 235 04m22.1s

18:45 16°09.0'S 139°13.5'W 18°27.2'S 140°16.4'W 17°17.7'S 139°44.0'W 35 241 04m33.3s

18:50 15°58.9'S 136°55.3'W 18°16.1'S 137°54.5'W 17°07.1'S 137°24.2'W 37 247 04m43.1s

18:55 15°56.2'S 134°48.0'W 18°12.7'S 135°44.6'W 17°04.1'S 135°15.7'W 39 252 04m51.7s

19:00 16°00.1'S 132°49.1'W 18°16.0'S 133°43.8'W 17°07.7'S 133°15.9'W 41 256 04m59.1s

19:05 16°09.8'S 130°56.9'W 18°25.2'S 131°50.1'W 17°17.2'S 131°23.1'W 43 259 05m05.4s

19:10 16°24.8'S 129°10.0'W 18°39.8'S 130°02.0'W 17°31.9'S 129°35.6'W 44 261 05m10.5s

19:15 16°44.7'S 127°27.2'W 18°59.3'S 128°18.3'W 17°51.7'S 127°52.5'W 45 262 05m14.6s

19:20 17°09.4'S 125°47.7'W 19°23.6'S 126°38.0'W 18°16.1'S 126°12.6'W 46 262 05m17.5s

19:25 17°38.6'S 124°10.6'W 19°52.4'S 125°00.1'W 18°45.1'S 124°35.1'W 47 261 05m19.4s

19:30 18°12.2'S 122°35.1'W 20°25.7'S 123°23.8'W 19°18.6'S 122°59.4'W 47 260 05m20.3s

19:35 18°50.3'S 121°00.7'W 21°03.5'S 121°48.5'W 19°56.5'S 121°24.5'W 47 258 05m20.0s

19:40 19°32.9'S 119°26.5'W 21°45.8'S 120°13.4'W 20°38.9'S 119°49.9'W 47 255 05m18.8s

19:45 20°20.0'S 117°51.9'W 22°32.7'S 118°37.7'W 21°25.9'S 118°14.8'W 46 252 05m16.5s

19:50 21°11.9'S 116°16.2'W 23°24.5'S 117°00.6'W 22°17.7'S 116°38.5'W 46 249 05m13.3s

19:55 22°08.7'S 114°38.5'W 24°21.4'S 115°21.3'W 23°14.5'S 115°00.0'W 45 245 05m09.1s

20:00 23°10.9'S 112°57.8'W 25°23.8'S 113°38.6'W 24°16.8'S 113°18.4'W 43 241 05m03.9s

20:05 24°18.9'S 111°13.1'W 26°32.3'S 111°51.5'W 25°25.0'S 111°32.6'W 42 237 04m57.8s

20:10 25°33.4'S 109°23.0'W 27°47.7'S 109°58.3'W 26°39.9'S 109°41.0'W 40 233 04m50.7s

20:15 26°55.2'S 107°25.6'W 29°10.9'S 107°57.0'W 28°02.3'S 107°41.8'W 38 228 04m42.7s

20:20 28°25.7'S 105°18.6'W 30°43.3'S 105°44.8'W 29°33.7'S 105°32.3'W 36 224 04m33.7s

20:25 30°06.6'S 102°58.5'W 32°27.2'S 103°17.8'W 31°16.0'S 103°09.0'W 33 219 04m23.6s

20:30 32°00.8'S 100°20.1'W 34°25.8'S 100°29.7'W 33°12.2'S 100°26.0'W 30 214 04m12.3s

20:35 34°12.7'S 097°14.8'W 36°45.0'S 097°09.4'W 35°27.5'S 097°13.7'W 26 209 03m59.4s

20:40 36°51.0'S 093°26.0'W 39°36.2'S 092°54.4'W 38°11.7'S 093°12.9'W 21 204 03m44.4s

20:45 40°16.5'S 088°13.0'W 43°32.5'S 086°39.3'W 41°50.5'S 087°33.0'W 15 197 03m25.7s

20:50 46°09.3'S 078°12.1'W - - 50°24.0'S 071°53.8'W 1 183 02m47.2s

Limits 50°07.6'S 070°19.6'W 51°35.5'S 071°33.7'W 50°51.4'S 070°55.8'W 0 183 02m45.4s

 50 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
TABLE 3.4

PHYSICAL EPHEMERIS OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

∆T = 66.2 s

Universal Central Line Diameter Eclipse Sun Sun Path Major Minor Umbra Central

Time Latitude Longitude Ratio Obscur. Alt Azm Width Axis Axis Veloc. Durat.

° ° km km km km/s

18:16.8 26°51.4'S 170°59.5'W 1.0441 1.0902 0.0 65.1 179.2 - 147.2 - 02m42.4s

18:20 22°19.8'S 159°27.6'W 1.0480 1.0982 12.0 59.8 197.0 761.8 159.4 3.160 03m15.1s

18:25 20°10.7'S 153°03.5'W 1.0502 1.1029 19.2 56.5 209.5 504.6 166.5 1.842 03m37.8s

18:30 18°57.0'S 148°42.5'W 1.0517 1.1062 24.2 53.9 219.2 416.3 171.4 1.385 03m55.0s

18:35 18°09.2'S 145°15.0'W 1.0529 1.1087 28.3 51.3 227.5 368.9 175.1 1.138 04m09.5s

18:40 17°37.6'S 142°19.0'W 1.0539 1.1107 31.7 48.8 234.8 338.7 178.1 0.980 04m22.1s

18:45 17°17.7'S 139°44.0'W 1.0547 1.1124 34.6 46.2 241.3 317.8 180.7 0.871 04m33.3s

18:50 17°07.1'S 137°24.2'W 1.0554 1.1139 37.1 43.5 247.0 302.5 182.9 0.791 04m43.1s

18:55 17°04.1'S 135°15.7'W 1.0560 1.1151 39.3 40.6 251.8 291.0 184.7 0.732 04m51.7s

19:00 17°07.7'S 133°15.9'W 1.0565 1.1162 41.2 37.6 255.7 282.1 186.2 0.687 04m59.1s

19:05 17°17.2'S 131°23.1'W 1.0569 1.1171 42.9 34.4 258.6 275.3 187.6 0.654 05m05.4s

19:10 17°31.9'S 129°35.6'W 1.0573 1.1178 44.2 31.0 260.7 270.0 188.6 0.629 05m10.5s

19:15 17°51.7'S 127°52.5'W 1.0575 1.1184 45.3 27.5 261.8 266.1 189.5 0.612 05m14.6s

19:20 18°16.1'S 126°12.6'W 1.0578 1.1188 46.2 23.9 262.0 263.2 190.2 0.602 05m17.5s

19:25 18°45.1'S 124°35.1'W 1.0579 1.1192 46.7 20.1 261.4 261.4 190.7 0.597 05m19.4s

19:30 19°18.6'S 122°59.4'W 1.0580 1.1194 47.1 16.3 260.0 260.5 191.0 0.597 05m20.3s

19:35 19°56.5'S 121°24.5'W 1.0580 1.1195 47.1 12.4 257.9 260.4 191.1 0.603 05m20.0s

19:40 20°38.9'S 119°49.9'W 1.0580 1.1194 46.9 8.4 255.3 261.3 191.0 0.613 05m18.8s

19:45 21°25.9'S 118°14.8'W 1.0579 1.1193 46.4 4.6 252.3 263.0 190.8 0.628 05m16.5s

19:50 22°17.7'S 116°38.5'W 1.0578 1.1190 45.7 0.7 248.8 265.6 190.3 0.649 05m13.3s

19:55 23°14.5'S 115°00.0'W 1.0576 1.1185 44.7 356.9 245.0 269.4 189.7 0.675 05m09.1s

20:00 24°16.8'S 113°18.4'W 1.0573 1.1180 43.4 353.2 241.1 274.4 188.9 0.707 05m03.9s

20:05 25°25.0'S 111°32.6'W 1.0570 1.1173 41.9 349.6 236.9 280.8 187.9 0.748 04m57.8s

20:10 26°39.9'S 109°41.0'W 1.0566 1.1164 40.1 346.1 232.7 289.2 186.6 0.798 04m50.7s

20:15 28°02.3'S 107°41.8'W 1.0561 1.1153 38.0 342.7 228.3 300.0 185.0 0.860 04m42.7s

20:20 29°33.7'S 105°32.3'W 1.0555 1.1141 35.5 339.3 223.8 314.1 183.2 0.939 04m33.7s

20:25 31°16.0'S 103°09.0'W 1.0548 1.1126 32.8 335.9 219.1 333.1 180.9 1.043 04m23.6s

20:30 33°12.2'S 100°26.0'W 1.0539 1.1108 29.6 332.5 214.3 359.8 178.2 1.186 04m12.3s

20:35 35°27.5'S 097°13.7'W 1.0529 1.1086 25.8 328.9 209.2 400.1 175.0 1.397 03m59.4s

20:40 38°11.7'S 093°12.9'W 1.0516 1.1058 21.2 324.8 203.6 469.3 170.8 1.754 03m44.4s

20:45 41°50.5'S 087°33.0'W 1.0497 1.1019 15.1 319.7 196.9 628.5 165.0 2.561 03m25.7s

20:50 50°24.0'S 071°53.8'W 1.0452 1.0925 0.8 307.2 183.5 9822.8 150.7 48.256 02m47.2s

20:50.0 50°51.4'S 070°55.8'W 1.0450 1.0920 0.0 306.5 182.8 - 149.9 - 02m45.4s

Annular and Total Solar Eclipses of 2010 51

Total Solar Eclipse of 2010 July 11
TABLE 3.5

LOCAL CIRCUMSTANCES ON THE CENTRAL LINE

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

∆T = 66.2 s

Central Line

Maximum Eclipse First Contact Second Contact Third Contact Fourth Contact .

U.T. Durat. Alt U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt

18:20 03m15.1s 12 - - - - 18:18:23 97 217 18:21:38 277 37 19:34:32 98 229 26

18:25 03m37.8s 19 17:15:54 276 30 5 18:23:12 98 220 18:26:49 278 40 19:44:45 100 235 34

18:30 03m55.0s 24 17:17:46 277 32 10 18:28:03 99 223 18:31:58 279 43 19:53:30 101 242 39

18:35 04m09.5s 28 17:20:04 278 34 14 18:32:56 100 226 18:37:05 280 47 20:01:26 103 248 42

18:40 04m22.1s 32 17:22:39 279 36 17 18:37:49 101 230 18:42:12 281 50 20:08:48 104 254 45

18:45 04m33.3s 35 17:25:26 279 38 20 18:42:44 102 233 18:47:17 282 54 20:15:42 105 261 47

18:50 04m43.1s 37 17:28:25 280 40 22 18:47:39 103 237 18:52:22 283 58 20:22:11 106 267 49

18:55 04m51.7s 39 17:31:33 281 43 24 18:52:35 104 241 18:57:26 284 62 20:28:18 108 273 50

19:00 04m59.1s 41 17:34:51 282 45 27 18:57:31 105 245 19:02:30 285 67 20:34:06 109 279 50

19:05 05m05.4s 43 17:38:18 282 48 29 19:02:28 106 249 19:07:33 286 71 20:39:36 110 285 51

19:10 05m10.5s 44 17:41:54 283 51 30 19:07:25 107 254 19:12:36 287 76 20:44:51 111 291 50

19:15 05m14.6s 45 17:45:40 284 54 32 19:12:23 108 258 19:17:38 288 80 20:49:51 111 296 50

19:20 05m17.5s 46 17:49:35 285 57 34 19:17:22 109 263 19:22:39 289 85 20:54:37 112 301 49

19:25 05m19.4s 47 17:53:40 286 61 35 19:22:21 109 268 19:27:40 290 90 20:59:12 113 306 48

19:30 05m20.3s 47 17:57:56 287 65 36 19:27:20 110 273 19:32:40 291 95 21:03:36 114 310 47

19:35 05m20.0s 47 18:02:24 288 68 38 19:32:20 111 278 19:37:40 291 100 21:07:50 114 314 46

19:40 05m18.8s 47 18:07:02 288 72 39 19:37:21 112 282 19:42:39 292 104 21:11:55 115 317 44

19:45 05m16.5s 46 18:11:53 289 76 39 19:42:22 113 287 19:47:38 293 109 21:15:52 115 320 43

19:50 05m13.3s 46 18:16:56 290 81 40 19:47:23 113 292 19:52:37 293 114 21:19:41 116 323 41

19:55 05m09.1s 45 18:22:13 291 85 40 19:52:25 114 296 19:57:34 294 118 21:23:22 116 325 39

20:00 05m03.9s 43 18:27:44 292 90 41 19:57:28 114 300 20:02:32 294 122 21:26:57 116 327 37

20:05 04m57.8s 42 18:33:28 292 95 41 20:02:31 115 304 20:07:29 295 126 21:30:25 116 329 35

20:10 04m50.7s 40 18:39:28 293 100 40 20:07:34 115 308 20:12:25 295 129 21:33:46 116 331 32

20:15 04m42.7s 38 18:45:44 293 105 39 20:12:38 115 311 20:17:21 295 133 21:37:00 116 332 30

20:20 04m33.7s 36 18:52:16 294 110 38 20:17:43 116 314 20:22:17 296 136 21:40:07 116 333 27

20:25 04m23.6s 33 18:59:06 294 115 37 20:22:48 116 317 20:27:12 296 138 21:43:05 116 334 24

20:30 04m12.3s 30 19:06:17 295 119 35 20:27:54 116 320 20:32:06 296 141 21:45:54 116 335 20

20:35 03m59.4s 26 19:13:52 295 124 32 20:33:00 115 322 20:36:59 295 143 21:48:29 116 335 16

20:40 03m44.4s 21 19:21:59 295 129 28 20:38:08 115 324 20:41:52 295 145 21:50:45 115 335 12

20:45 03m25.7s 15 19:31:00 294 133 22 20:43:17 114 325 20:46:43 294 146 21:52:24 114 334 6

20:50 02m47.2s 1 19:44:30 292 138 8 20:48:36 112 325 20:51:23 292 146 - - - -

20:50 02m45.5s 1 19:44:55 292 138 8 20:48:38 112 325 20:51:23 292 145 - - - -

 52 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
TABLE 3.6

TOPOCENTRIC DATA AND PATH CORRECTIONS DUE TO LUNAR LIMB PROFILE

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

∆T = 66.2 s

North South

Moon Moon Moon Topo North Limit Limit Central

Universal Topo Topo Rel. Lib. Sun Sun Path Limit —————————— —————————— Durat.

Time H.P. S.D. Ang.V Long Alt. Az. Az. P.A. Int. Ext. Int. Ext. Corr.

" " "/s ° ° ° ° ° ' ' ' ' s

18:20 3632.8 989.2 0.464 -2.53 12.0 59.8 68.6 6.6 -0.3 0.5 0.6 -2.3 -2.2

18:25 3640.7 991.3 0.435 -2.58 19.2 56.5 71.9 7.7 -0.2 0.6 0.3 -2.4 -2.7

18:30 3646.0 992.8 0.416 -2.62 24.2 53.9 74.9 8.7 -0.1 0.7 0.2 -3.0 -3.3

18:35 3650.2 993.9 0.401 -2.66 28.3 51.3 77.9 9.8 0.1 0.7 0.1 -3.1 -3.9

18:40 3653.6 994.8 0.388 -2.71 31.7 48.8 80.9 10.8 0.2 0.7 -0.1 -3.0 -4.1

18:45 3656.4 995.6 0.378 -2.75 34.6 46.2 83.9 11.8 0.3 1.0 -0.3 -2.5 -4.6

18:50 3658.8 996.3 0.370 -2.79 37.1 43.5 87.0 12.8 0.3 1.1 -0.3 -3.0 -4.9

18:55 3660.9 996.8 0.362 -2.83 39.3 40.6 90.2 13.8 0.3 1.5 -0.3 -3.3 -5.2

19:00 3662.6 997.3 0.357 -2.88 41.2 37.6 93.4 14.8 0.2 1.4 -0.4 -3.2 -5.4

19:05 3664.1 997.7 0.352 -2.92 42.9 34.4 96.6 15.8 0.2 1.1 -0.4 -3.3 -5.5

19:10 3665.3 998.0 0.348 -2.96 44.2 31.0 99.8 16.8 0.2 0.9 -0.2 -3.8 -5.6

19:15 3666.3 998.3 0.345 -3.00 45.3 27.5 102.9 17.8 0.2 0.7 -0.2 -4.2 -5.5

19:20 3667.1 998.5 0.343 -3.05 46.2 23.9 106.0 18.7 0.2 0.9 -0.1 -4.3 -5.8

19:25 3667.6 998.6 0.342 -3.09 46.7 20.1 108.9 19.6 0.2 1.2 -0.1 -4.0 -6.0

19:30 3668.0 998.7 0.342 -3.13 47.1 16.3 111.7 20.4 0.3 1.4 0.0 -3.3 -6.2

19:35 3668.1 998.8 0.342 -3.18 47.1 12.4 114.3 21.2 0.3 1.3 0.0 -2.7 -6.3

19:40 3668.0 998.7 0.344 -3.22 46.9 8.4 116.8 22.0 0.4 1.2 0.0 -2.2 -6.3

19:45 3667.7 998.7 0.346 -3.26 46.4 4.6 119.0 22.7 0.5 1.6 0.0 -2.6 -6.3

19:50 3667.2 998.5 0.348 -3.30 45.7 0.7 121.1 23.3 0.6 1.7 -0.0 -2.8 -6.4

19:55 3666.5 998.4 0.352 -3.35 44.7 356.9 123.0 23.9 0.7 1.7 -0.0 -2.8 -6.3

20:00 3665.6 998.1 0.356 -3.39 43.4 353.2 124.6 24.4 0.7 1.5 -0.1 -2.7 -6.1

20:05 3664.4 997.8 0.361 -3.43 41.9 349.6 126.1 24.8 0.8 1.3 -0.1 -2.5 -5.9

20:10 3663.0 997.4 0.367 -3.48 40.1 346.1 127.4 25.2 0.9 1.2 -0.1 -2.3 -5.8

20:15 3661.2 996.9 0.375 -3.52 38.0 342.7 128.4 25.5 1.0 1.4 -0.1 -2.2 -5.6

20:20 3659.1 996.4 0.383 -3.56 35.5 339.3 129.3 25.6 1.0 1.5 -0.1 -2.2 -5.5

20:25 3656.6 995.7 0.392 -3.61 32.8 335.9 129.9 25.7 1.0 1.5 -0.1 -2.3 -5.4

20:30 3653.6 994.9 0.404 -3.65 29.6 332.5 130.3 25.6 1.0 1.5 -0.1 -2.2 -5.2

20:35 3649.9 993.9 0.417 -3.69 25.8 328.9 130.5 25.4 0.9 1.4 -0.1 -2.2 -5.1

20:40 3645.3 992.6 0.434 -3.73 21.2 324.8 130.3 25.0 0.8 1.2 -0.1 -2.5 -5.1

20:45 3638.9 990.9 0.456 -3.78 15.1 319.7 129.7 24.3 0.7 1.6 -0.0 -2.8 -5.0

20:50 3623.6 986.6 0.511 -3.82 0.8 307.2 126.9 22.0 0.7 1.6 -0.0 -2.8 -5.0

Annular and Total Solar Eclipses of 2010 53

Total Solar Eclipse of 2010 July 11
TABLE 3.7

LOCAL CIRCUMSTANCES FOR PACIFIC OCEAN & SOUTH AMERICA

TOTAL SOLAR ECLIPSE OF 2010 JULY 11

Location Name Latitude Longitude Elev. First Contact Second Contact Third Contact Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P V Alt U.T. P V U.T. P V U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

m h m s ° ° ° h m s ° ° h m s ° ° h m s ° ° ° h m s ° ° ° °

PACIFIC OCEANCOOK ISLANDSMangaia Is. 21°55'S 157°55'W — 17:15:06.6 276 30 1 18:19:27.3 105 226 18:22:45.4 269 30 19:36:50.8 98 230 28 18:21:06.0 7 128 14 59 1.048 1.000 0.856 03m18sMauke Is. 20°09'S 157°23'W — 17:13:48.5 274 26 1 — — 19:36:03.4 101 231 29 18:19:57.8 187 306 15 59 0.988 0.991Rarotonga Is. 21°14'S 159°46'W — — — — 19:32:53.5 100 229 26 18:18:39.5 186 305 12 60 0.993 0.996FIJILautoka 17°37'S 177°27'E — — — — 19:01:53.4 116 227 4 18:43 Rise — — 0 67 0.286 0.178Suva 18°08'S 178°25'E 6 — — — 19:03:19.0 115 226 5 18:40 Rise — — 0 67 0.351 0.239FRENCH POLYNESIABora-Bora 16°30'S 151°45'W — 17:13:51.2 272 23 7 — — 19:43:56.2 105 238 37 18:23:24.0 188 307 22 57 0.941 0.937Moorea Is. 17°32'S 149°40'W — 17:15:53.4 274 28 9 — — 19:49:49.8 103 241 39 18:27:14.0 188 310 24 55 0.983 0.987Papeete, Tahiti 17°32'S 149°34'W 2 17:15:57.6 274 28 9 — — 19:50:04.1 103 241 39 18:27:22.9 188 311 24 55 0.984 0.987Rikitea 23°08'S 134°57'W — 17:39:16.0 289 58 23 — — 20:33:32.3 100 270 44 19:02:09.3 14 159 36 36 0.887 0.869Hikueru 17°35'S 142°39'W 2 17:22:14.1 278 35 16 18:37:08.7 95 224 18:41:28.4 286 55 20:07:50.6 104 253 45 18:39:18.0 191 319 31 49 1.054 1.000 0.910 04m20sTatakoto 17°22'S 138°26'W 2 17:27:13.0 280 40 21 18:45:37.7 112 245 18:50:12.4 273 47 20:19:26.6 106 264 48 18:47:54.6 12 146 36 45 1.055 1.000 0.835 04m35sSAMOA, WESTERNApia 13°50'S 171°44'W — — — — 19:06:45.0 116 228 16 18:05:50.7 185 290 3 67 0.664 0.588TONGANuku'alofa 21°08'S 175°12'W — — — — 19:12:35.6 106 224 11 18:20 Rise — — 0 67 0.768 0.716EASTER ISLAND (ISLA DE PASCUA, CHILE) Hanga Roa 27°09'S 109°26'W — 18:40:35.9 293 101 40 20:08:30.0 129 322 20:13:10.9 282 116 21:34:16.3 116 330 32 20:10:50.6 25 219 40 346 1.056 1.000 0.767 04m41sGALAPAGOS ISLANDS (ECUADOR)Isla Santa Cruz 00°38'S 090°23'W — 20:07:57.9 221 97 53 — — 20:39:40.7 198 82 46 20:23:55.4 209 90 50 306 0.020 0.003SOUTH AMERICAARGENTINABuenos Aires 34°36'S 058°27'W 27 20:13:43.8 260 128 7 — — — 20:57 Set — — 0 297 0.446 0.336Córdoba 31°24'S 064°11'W — 20:11:52.8 260 128 13 — — — 21:04:11.5 204 78 4 299 0.438 0.329El Calafate 50°20'S 072°15'W — 19:44:15.1 292 138 9 20:48:30.1 118 331 20:51:17.1 286 140 — 20:49:53.8 22 235 1 308 1.045 1.000 0.902 02m47sLa Plata 34°55'S 057°57'W — 20:13:44.6 260 129 7 — — — 20:55 Set — — 0 297 0.437 0.327Lomas de Zamora 34°46'S 058°24'W — 20:13:31.5 261 129 7 — — — 20:57 Set — — 0 297 0.448 0.338Mar del Plata 38°00'S 057°33'W — 20:09:36.2 266 131 6 — — — 20:45 Set — — 0 298 0.452 0.343Mendoza 32°53'S 068°49'W 800 20:03:39.3 267 130 17 — — — 21:01:56.8 204 75 7 302 0.542 0.444Rosario 32°57'S 060°40'W — 20:13:52.7 259 128 10 — — — 21:04:48.9 204 77 1 297 0.438 0.329San Miguel de T* 26°49'S 065°13'W — 20:17:46.1 252 124 16 — — — 21:04:26.8 205 82 7 299 0.319 0.209BOLIVIALa Paz 16°30'S 068°09'W 3658 20:39:13.3 226 108 20 — — 21:22:52.5 186 73 10 21:01:23.3 206 91 15 299 0.061 0.018BRAZILJardim 21°28'S 056°09'W — 20:50:53.5 220 105 5 — — — 21:06:58.9 204 90 2 294 0.039 0.009Porto Alegre 30°04'S 051°11'W 10 20:29:31.6 243 120 2 — — — 20:39 Set — — 0 295 0.096 0.036CHILEConcepción 36°50'S 073°03'W — 19:53:54.7 277 133 18 — — — 20:58:25.7 204 69 8 306 0.707 0.641Santiago 33°27'S 070°40'W — 20:00:24.7 270 131 18 — — — 21:00:51.8 205 74 8 303 0.583 0.492Valparaíso 33°02'S 071°38'W 41 19:59:27.0 270 130 19 — — — 21:00:27.3 205 74 9 304 0.585 0.494PARAGUAYAsuncion 25°16'S 057°40'W 139 20:33:13.2 238 117 8 — — — 21:06:47.6 204 86 1 295 0.173 0.085PERULima 12°03'S 077°03'W 120 20:24:15.3 231 110 32 — — 21:18:56.8 184 71 21 20:52:11.9 208 91 27 302 0.081 0.028URUGUAYMontevideo 34°53'S 056°11'W 22 20:15:29.2 259 128 5 — — — 20:48 Set — — 0 297 0.368 0.256

 54 Annularand Total Solar Eclipses of 2010

TotalSolarEclipse of 2010 July 11
July Climate 

Statistics

Percent 

of 

possible 

sunshine

Calculated 

Cloudiness July Precip.

Ave. 

no. 

days 

with 

rain

Ave. 

no. 

days 

with 

tstms

Ave. 

no. 

days 

with 

snow

Days 

with 

fog

Ave. 

July 

High

Ave. 

July 

Low

Clear Few 

Scatter

ed Broken 

Overcast Obscur- ed

% mm (°C) (°C)

Cook IslandsMangaia Island* 0.3 16.7 21.7 45.3 16.0 0.0 63 159 15.3 0.4 25 19Rarotonga 52 0.0 13.1 25.9 50.4 10.6 0.0 63 104 16.5 0.3 0.1 25 20Mauke 2.2 30.3 15.1 42.1 10.3 0.0 55 115 11.9 0.2 26 21TahitiPapeete 68 0.2 38.1 25.1 32.9 3.7 0.0 46 53 7.4 0.4 29 21Tuamotu Atoll Takaroa 66 0.2 38.7 30.2 26.7 4.1 0.2 44Rikitea 45 0.0 26.0 28.0 40.1 5.9 0.0 54Hao* 0.4 20.2 36.1 41.8 1.5 0.0 53 76.1 10.2 27 23Hereheretue 68 0.4 20.2 36.1 41.8 1.5 0.0 53 72.3 12 27 22Austral IslandsRapa Iti 38 0.0 8.1 13.9 57.9 20.1 0.0 73 207 21 16Tubuai 51 0.3 19.6 16.8 52.4 10.8 0.0 62 144.9 24 18ChileEaster Island * 50 0.0 7.4 20.3 57.1 15.2 0.0 70 111 18.1 21 16Puerto Natales 0.0 13.9 25.0 41.7 16.7 2.8 65 33 11.4 4 -1ArgentinaEl Calafate* 7.8 18.8 24.7 34.4 14.3 0.0 55 42 3.6 0 3.4 1 6 -5* This location is in the path of totality.

Table 3.8: Climate Statistics for July along the Total Eclipse Path

Percent Frequency of Sky Condition

Annular and Total Solar Eclipses of 2010 55

Total Solar Eclipse of 2010 July 11
N

S

W E

Kilometers

 0 1000 2000 3000 4000 5000

Total Solar Eclipse of 2010 Jul 11

Ecliptic Conjunction = 19:41:33.5 TD ( = 19:40:27.3 UT )

 Greatest Eclipse = 19:34:37.6 TD ( = 19:33:31.4 UT )

Eclipse Magnitude = 1.0580 Gamma = -0.6788

Saros Series = 146 Member = 27 of 76

Sun at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 07h23m57.6s

Dec. = +22°02'11.0"

S.D. = 00°15'43.9"

H.P. = 00°00'08.7"

Moon at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 07h23m15.8s

Dec. = +21°22'29.3"

S.D. = 00°16'26.7"

H.P. = 01°00'20.9"

External/Internal

Contacts of Penumbra

P1 = 17:09:37.6 UT

P4 = 21:57:14.3 UT

External/Internal

Contacts of Umbra

U1 = 18:15:12.1 UT

U2 = 18:18:29.9 UT

U3 = 20:48:19.6 UT

U4 = 20:51:41.0 UT

Local Circumstances at Greatest Eclipse

 Lat. = 19°44.9'S Sun Alt. = 47.1°

Long. = 121°52.5'W Sun Azm. = 13.5°

Path Width = 258.6 km Duration = 05m20.2s

Constants & Ephemeris

 !T = 66.2 s

 k1 = 0.2725076

 k2 = 0.2722810

!b = 0.0" !l = 0.0"

Eph. = JPL DE200/LE200

Geocentric Libration

(Optical + Physical)

l = -3.25°

b = 0.86°

c = 6.62°

Brown Lun. No. = 1083

P1

P4

FIGURE 3.1: ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH

Greatest Eclipse 

 Sub Solar 

 Path of Total Eclipse 

0.20

0.40

0.60

0.80

0.60

0.80

19:30 

UT

19:00 

UT

20:30 UT

20:00 UT

18:30 

UT

21:00 

UT

NASA 2010 Eclipse Bulletin, Espenak & Anderson

 56 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
Annular and Total Solar Eclipses of 2010 57

Total Solar Eclipse of 2010 July 11
 58 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
Annular and Total Solar Eclipses of 2010 59

Total Solar Eclipse of 2010 July 11
 60 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
Annular and Total Solar Eclipses of 2010 61

Total Solar Eclipse of 2010 July 11
N

S

E W

Total Solar Eclipse of 2010 Jul 11

Maximum Eclipse = 19:30:00.0 UT

Moon/Sun Diameter Ratio = 1.0580

000°

180°

090° 270°

Arc-Seconds

 0 1 2 3 4 5

Seconds

 0 1 2 3 4 5

Seconds

 2 1 0 -1 -2

Seconds

 -2 -1 0 1 2

 3

 2

 1

 0

 -1

 -2

 -3

 -3

 -2

 -1

 0

 1

 2

 3

Sun at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 07h23m57.1s

 Dec. = +22°02'17.8"

 S.D. = 00°15'44.0"

 H.P. = 00°00'08.7"

Moon at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 07h23m58.0s

 Dec. = +22°02'16.8"

 S.D. = 00°16'38.7"

 H.P. = 01°01'08.0"

Geographic Position

Name = Central Line at 19:30 UT

Lat. = 19°18'36.1"S

Long. = 122°59'21.3"W

Elev. = 0.0 m

Eclipse Contacts

C1 = 17:57:56.4 UT

C2 = 19:27:20.1 UT

C3 = 19:32:40.3 UT

C4 = 21:03:36.0 UT

Limb Corrected Contacts

C2* = 19:27:22.9 UT ( 2.8s)

C3* = 19:32:37.0 UT ( -3.3s)

Local Circumstances at Maximum Eclipse

 Sun Alt. = 47.1° Path Width = 260.0 km

Sun Azm. = 16.3° Duration = 05m20.2s

PA(N.Limit) = 20.4° A.Vel. (M:S) = 0.342"/s

Ephemeris & Constants

Eph. = DE200/LE200

 !T = 66.2 s

 k1 = 0.2725076

 k2 = 0.2722810

!b = 0.00" !l = 0.00"

Calculated Center of Figure

!b ́ = -0.19" !l ́ = 0.52"

Topocentric Libration

(Optical + Physical)

l = -3.13°

b = 0.18°

c = 6.68°

FIGURE 3.7: LUNAR LIMB PROFILE FOR JULY 11 AT 19:30 UT

Second Contact

Time Correction Curve 

Contact Time 

Correction 

Scale

Third Contact

Time Correction Curve

Contact Time 

Correction 

Scale

NASA 2010 Eclipse Bulletin, Espenak & Anderson

Mean Limb

(Center of Mass)

(Center of Figure)

Mean Limb

True Limb

Third

Contact

Second

Contact

Northern 

Limit

Moon 

North

Zenith

Southern Limit

 62 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
Annular and Total Solar Eclipses of 2010 63

Total Solar Eclipse of 2010 July 11
 64 Annular and Total Solar Eclipses of 2010

Total Solar Eclipse of 2010 July 11
4. Observing Eclipses

4.1 Eye Safety and Solar Eclipses

A solar eclipse is probably the most spectacular astronomical event that many people will experience in their lives. There 

is a great deal of interest in watching eclipses, and thousands 

of astronomers (both amateur and professional) and other 

eclipse enthusiasts travel around the world to observe and 

photograph them.

A solar eclipse offers students a unique opportunity to 

see a natural phenomenon that illustrates the basic principles 

of mathematics and science taught through elementary and 

secondary school. Indeed, many scientists (including astronomers) have been inspired to study science as a result of seeing 

a total solar eclipse. Teachers can use eclipses to show how 

the laws of motion and the mathematics of orbits can predict 

the occurrence of eclipses. The use of pinhole cameras and 

telescopes or binoculars to observe an eclipse leads to an 

understanding of the optics of these devices. The rise and fall 

of environmental light levels during an eclipse illustrate the 

principles of radiometry and photometry, while biology classes 

can observe the associated behavior of plants and animals. It 

is also an opportunity for children of school age to contribute 

actively to scientific research—observations of contact timings at different locations along the eclipse path are useful in 

refining our knowledge of the orbital motions of the Moon 

and Earth, and sketches and photographs of the solar corona 

can be used to build a three-dimensional picture of the Sun’s 

extended atmosphere during the eclipse.

Observing the Sun, however, can be dangerous if the proper precautions are not taken. The solar radiation that reaches 

the surface of Earth ranges from ultraviolet (UV) radiation at 

wavelengths longer than 290 nm, to radio waves in the meter 

range. The tissues in the eye transmit a substantial part of the 

radiation between 380–400 nm to the light-sensitive retina 

at the back of the eye. While environmental exposure to UV 

radiation is known to contribute to the accelerated aging of 

the outer layers of the eye and the development of cataracts, 

the primary concern over improper viewing of the Sun during an eclipse is the development of “eclipse blindness” or 

retinal burns.

Exposure of the retina to intense visible light causes damage to its light-sensitive rod and cone cells. The light triggers 

a series of complex chemical reactions within the cells which 

damages their ability to respond to a visual stimulus, and in 

extreme cases, can destroy them. The result is a loss of visual 

function, which may be either temporary or permanent depending on the severity of the damage. When a person looks 

repeatedly, or for a long time, at the Sun without proper eye 

protection, this photochemical retinal damage may be accompanied by a thermal injury—the high level of visible and 

near-infrared radiation causes heating that literally cooks 

the exposed tissue. This thermal injury or photocoagulation 

destroys the rods and cones, creating a small blind area. The 

danger to vision is significant because photic retinal injuries 

occur without any feeling of pain (the retina has no pain receptors), and the visual effects do not become apparent for at least 

several hours after the damage is done (Pitts 1993). Viewing 

the Sun through binoculars, a telescope, or other optical devices without proper protective filters can result in immediate 

thermal retinal injury because of the high irradiance level in 

the magnified image. 

The only time that the Sun can be viewed safely with the 

naked eye is during a total eclipse, when the Moon completely 

covers the disk of the Sun. It is never safe to look at a partial 

or annular eclipse, or the partial phases of a total solar eclipse, 

without the proper equipment and techniques. Even when 99% 

of the Sun’s surface (the photosphere) is obscured during the 

partial phases of a solar eclipse, the remaining crescent Sun 

is still intense enough to cause a retinal burn, even though 

illumination levels are comparable to twilight (Chou 1981 

and 1996, and Marsh 1982). Failure to use proper observing 

methods may result in permanent eye damage and severe 

visual loss. This can have important adverse effects on career 

choices and earning potential, because it has been shown that 

most individuals who sustain eclipse-related eye injuries are 

children and young adults (Penner and McNair 1966, Chou 

and Krailo 1981, and Michaelides et al. 2001).

The same techniques for observing the Sun outside of 

eclipses are used to view and photograph annular solar eclipses 

and the partly eclipsed Sun (Sherrod 1981, Pasachoff 2000, 

Pasachoff and Covington 1993, and Reynolds and Sweetsir 

1995). The safest and most inexpensive method is by projection. A pinhole or small opening is used to form an image of 

the Sun on a screen placed about a meter behind the opening. 

Multiple openings in perfboard, a loosely woven straw hat, or 

even interlaced fingers can be used to cast a pattern of solar 

images on a screen. A similar effect is seen on the ground 

below a broad-leafed tree: the many “pinholes” formed by 

overlapping leaves creates hundreds of crescent-shaped images. Binoculars or a small telescope mounted on a tripod can 

also be used to project a magnified image of the Sun onto a 

white card. All of these methods can be used to provide a safe 

view of the partial phases of an eclipse to a group of observers, 

but care must be taken to ensure that no one looks through the 

device. The main advantage of the projection methods is that 

nobody is looking directly at the Sun. The disadvantage of 

the pinhole method is that the screen must be placed at least 

a meter behind the opening to get a solar image that is large 

enough to be easily seen.

The Sun can only be viewed directly when filters specially 

designed to protect the eyes are used. Most of these filters have 

a thin layer of chromium alloy or aluminum deposited on their 

surfaces that attenuates both visible and near-infrared radiation. A safe solar filter should transmit less than 0.003% (density ~4.5) of visible light and no more than 0.5% (density ~2.3) 

of the near-infrared radiation from 780–1400 nm. (In addition 

to the term transmittance [in percent], the energy transmission 

of a filter can also be described by the term density [unit less] 

where density, d, is the common logarithm of the reciprocal of 

transmittance, t, or d=log10[1/t]. A density of ‘0’ corresponds 

to a transmittance of 100%; a density of ‘1’ corresponds to a 

transmittance of 10%; a density of ‘2’ corresponds to a transAnnular and Total Solar Eclipses of 2010 65

Observing Eclipses
mittance of 1%, etc.). Figure 4.1 shows transmittance curves 

for a selection of safe solar filters.

One of the most widely available filters for safe solar viewing is shade number 14 welder’s glass, which can be obtained 

from welding supply outlets. A popular inexpensive alternative 

is aluminized polyester that has been specially made for solar 

observation. (This material is commonly known as “mylar,” 

although the registered trademark “Mylar®” belongs to Dupont, which does not manufacture this material for use as a 

solar filter. Note that “space blankets” and aluminized polyester 

film used in gardening are NOT suitable for this purpose!) Unlike the welding glass, aluminized polyester can be cut to fit 

any viewing device, and does not break when dropped. It has 

been pointed out that some aluminized polyester filters may 

have large (up to approximately 1mm in size) defects in their 

aluminum coatings that may be hazardous. A microscopic 

analysis of examples of such defects shows that despite their 

appearance, the defects arise from a hole in one of the two 

aluminized polyester films used in the filter. There is no large 

opening completely devoid of the protective aluminum coating. 

While this is a quality control problem, the presence of a defect 

in the aluminum coating does not necessarily imply that the 

filter is hazardous. When in doubt, an aluminized polyester 

solar filter that has coating defects larger than 0.2mm in size, 

or more than a single defect in any 5mm circular zone of the 

filter, should not be used.

An alternative to aluminized polyester that has become 

quite popular is “black polymer” in which carbon particles are 

suspended in a resin matrix. This material is somewhat stiffer 

than polyester film and requires a special holding cell if it is 

to be used at the front of binoculars, telephoto lenses, or telescopes. Intended mainly as a visual filter, the polymer gives a 

yellow-white image of the Sun (aluminized polyester produces 

a blue-white image). This type of filter may show significant 

variations in density of the tint across its extent; some areas 

may appear much lighter than others. Lighter areas of the filter 

transmit more infrared radiation than may be desirable. The 

advent of high resolution digital imaging in astronomy, especially for photographing the Sun, has increased the demand 

for solar filters of higher optical quality. Baader AstroSolar 

Safety Film, a metal-coated resin, can be used for both visual 

and photographic solar observations. A much thinner material, it has excellent optical quality and much less scattered 

light than polyester filters. The Baader material comes in two 

densities: one for visual use and a less dense version optimized 

for photography. Filters using optically flat glass substrates are 

available from several manufacturers, but are more expensive 

than polyester and polymer filters.

Many experienced solar observers use one or two layers 

of black-and-white film that has been fully exposed to light 

and developed to maximum density. Not all black-and-white 

films contain silver so care must be taken to use a silver-based 

emulsion. The metallic silver contained in the film acts as a 

protective filter; however, any black-and-white negative containing images is not suitable for this purpose. More recently, 

solar observers have used floppy disks and compact disks (CDs 

and CD-ROMs) as protective filters by covering the central 

openings and looking through the disk media. However, the 

optical quality of the solar image formed by a floppy disk or 

CD is relatively poor compared to aluminized polyester or 

welder’s glass. Some CDs are made with very thin aluminum 

coatings that are not safe—if a lighted light bulb can be seen 

through the CD, it should not be used! No filter should be used 

with an optical device (e.g., binoculars, telescope, camera) 

unless it has been specifically designed for that purpose and 

is mounted at the front end. Some sources of solar filters are 

listed below.

Unsafe filters include color film, black-and-white film 

that contains no silver (i.e., chromogenic film), film negatives 

with images on them, smoked glass, sunglasses (single or 

multiple pairs), photographic neutral density filters and polarizing filters. Most of these transmit high levels of invisible 

infrared radiation, which can cause a thermal retinal burn 

(see Figure 4.1). The fact that the Sun appears dim, or that no 

discomfort is felt when looking at the Sun through the filter, 

is no guarantee that the eyes are safe. 

Solar filters designed to thread into eyepieces that are often 

provided with inexpensive telescopes are also unsafe. These 

glass filters often crack unexpectedly from overheating when 

the telescope is pointed at the Sun, and retinal damage can 

occur faster than the observer can move the eye from the eyepiece. Avoid unnecessary risks. Local planetariums, science 

centers, or amateur astronomy clubs can provide additional 

information on how to observe the eclipse safely.

There are some concerns that ultraviolet-A (UVA) radiation (wavelengths from 315–380 nm) in sunlight may also adversely affect the retina (Del Priore 1999). While there is some 

experimental evidence for this, it only applies to the special 

case of aphakia, where the natural lens of the eye has been 

removed because of cataract or injury, and no UV-blocking 

spectacle, contact or intraocular lens has been fitted. In an 

intact normal human eye, UVA radiation does not reach the 

retina because it is absorbed by the crystalline lens. In aphakia, 

normal environmental exposure to solar UV radiation may 

indeed cause chronic retinal damage. The solar filter materials 

discussed in this article, however, attenuate solar UV radiation 

to a level well below the minimum permissible occupational 

exposure for UVA (ACGIH 2004), so an aphakic observer is at 

no additional risk of retinal damage when looking at the Sun 

through a proper solar filter.

In the days and weeks before a solar eclipse, there are often 

news stories and announcements in the media, warning about 

the dangers of looking at the eclipse. Unfortunately, despite the 

good intentions behind these messages, they frequently contain 

misinformation, and may be designed to scare people from 

viewing the eclipse at all. This tactic may backfire, however, 

particularly when the messages are intended for students. A 

student who heeds warnings from teachers and other authorities not to view the eclipse because of the danger to vision, and 

later learns that other students did see it safely, may feel cheated 

out of the experience. Having now learned that the authority 

figure was wrong on one occasion, how is this student going 

 66 Annular and Total Solar Eclipses of 2010

Observing Eclipses
to react when other health-related advice about drugs, AIDS2

, 

or smoking is given (Pasachoff 2001). Misinformation may be 

just as bad, if not worse, than no information.

Remember that the total phase of an eclipse can, and 

should, be seen without any filters, and certainly never by 

projection! It is completely safe to do so. Even after observing 

14 solar eclipses, the author finds the naked-eye view of the 

totally eclipsed Sun awe-inspiring. The experience should be 

enjoyed by all.

Sect. 4.1 was contributed by:

B. Ralph Chou, MSc, OD

Associate Professor, School of Optometry

University of Waterloo

Waterloo, Ontario, Canada N2L 3G1

4.2 Sources for Solar Filters

The following is a brief list of sources for filters that are 

specifically designed for safe solar viewing with or without 

a telescope. The list is not meant to be exhaustive, but is a 

representative sample of sources for solar filters currently 

available in North America and Europe. For additional sources, 

see advertisements in Astronomy and or Sky & Telescope

magazines. (The inclusion of any source on the following list 

does not imply an endorsement of that source by either the 

authors or NASA.)

Sources in the USA:

American Paper Optics, 3080 Bartlett Corporate Drive, Bartlett, 

TN 38133, (800) 767-8427 or (901) 381-1515

Astro-Physics, Inc., 11250 Forest Hills Rd., Rockford, IL 61115, 

(815) 282-1513.

Celestron International, 2835 Columbia Street, Torrance, CA 

90503, (310) 328-9560.

Coronado Technology Group, 1674 S. Research Loop, Suite 

436, Tucson, AZ 85710-6739, (520) 760-1561, (866) 

SUNWATCH.

 DayStar Filters LLC, 149 Northwest OO Highway, Warrensburg, 

MO 64093, (660) 747-2100.

Meade Instruments Corporation, 16542 Millikan Ave., Irvine, 

CA 92606, (714) 756-2291.

Rainbow Symphony, Inc., 6860 Canby Ave., #120, Reseda, CA 

91335, (818) 708-8400.

Telescope and Binocular Center, P.O. Box 1815, Santa Cruz, CA 

95061-1815, (408) 763-7030.

Thousand Oaks Optical, Box 4813, Thousand Oaks, CA 91359, 

(805) 491-3642.

Sources in Canada:

Kendrick Astro Instruments, 2920 Dundas St. W., Toronto, 

Ontario, Canada M6P 1Y8, (416) 762-7946.

Khan Scope Centre, 3243 Dufferin Street, Toronto, Ontario, 

Canada M6A 2T2, (416) 783-4140.

2. Acquired Immunodeficiency Syndrome

Perceptor Telescopes TransCanada, Brownsville Junction Plaza, 

Box 38, Schomberg, Ontario, Canada L0G 1T0, (905) 

939-2313.

Sources in Europe:

Baader Planetarium GmbH, Zur Sternwarte, 82291 Mammendorf, Germany, 0049 (8145) 8802.

4.3 Eclipse Photography

A solar eclipse can be safely photographed provided the 

above precautions are followed. Almost any kind of camera 

can be used to capture this rare event, but Single Lens Reflex 

(SLR) cameras offer interchangeable lenses and zooms. A 

lens with a fairly long focal length is recommended in order 

to produce as large an image of the Sun as possible. A standard 50mm lens on a 35mm film camera yields a minuscule 

0.5mm solar image, while a 200mm telephoto or zoom lens 

produces a 1.9mm image (Figure 4.2). A better choice would 

be one of the small, compact, catadioptic or mirror lenses that 

have become widely available in the past 20 years. The focal 

length of 500mm is most common among such mirror lenses 

and yields a solar image of 4.6mm. 

With one solar radius of corona on either side, an eclipse 

view during totality will cover 9.2mm. Adding a 2x teleconverter will produce a 1000mm focal length, which doubles the 

Sun’s diameter to 9.2mm. Focal lengths in excess of 1000mm 

usually fall within the realm of amateur telescopes. 

Consumer digital cameras have become affordable in 

recent years and many of these may be used to photograph the 

eclipse. Most recommendations for 35mm SLR cameras apply 

to digital SLR (DSLR) cameras as well. The primary difference is that the imaging chip in most DSLR cameras is only 

about 2/3 the area of a 35mm film frame (check the camera’s 

technical specifications). This means that the Sun’s relative size 

will be 1.5 times larger in a DSLR camera so a shorter focal 

length lens can be used to achieve the same angular coverage 

compared to a 35mm SLR camera. For example, a 500mm lens 

on a digital camera produces the same relative image size as 

a 750mm lens on a 35mm camera (Figure 4.2). Another issue 

to consider is the lag time between digital frames required to 

write images to the DSLR’s memory card. Better DSLRs have 

a buffer to temporarily store a burst of images before they are 

written to the card. It is also advisable to turn off the autofocus because it is not reliable under these conditions; focus the 

camera manually instead. Preparations must also be made for 

adequate battery power and space on the memory card.

If full disk photography of an annular or partial eclipse 

is planned, the focal length of the optics must not exceed 

2500mm on 35mm format (1700mm on digital). Longer focal 

lengths permit photography of only a magnified portion of the 

Sun’s disk. In order to photograph the Sun’s corona during a 

total eclipse, the focal length should be no longer than about 

1500mm (1000mm on digital); however, a shorter focal length 

of 1000mm (700mm digital) requires less critical framing and 

can capture some of the longer coronal streamers. Figure 4.2 

Annular and Total Solar Eclipses of 2010 67

Observing Eclipses
shows the apparent size of the Sun (or Moon) and the outer 

corona in both film and digital formats for a range of lens focal 

lengths. For any particular focal length, the diameter of the 

Sun’s image (on 35mm film) is approximately equal to the 

focal length divided by 109 (Table 4.1).

A solar filter must be used on the lens throughout the 

partial phases for both photography and safe viewing. Such 

filters are most easily obtained through manufacturers and 

dealers listed in Sky & Telescope and Astronomy magazines 

(see Sect. 4.2, “Sources for Solar Filters”). These filters typically attenuate the Sun’s visible and infrared energy by a factor 

of 100,000. The actual filter factor and choice of International 

Organization for Standardization (ISO) speed, however, will 

play critical roles in determining the correct photographic 

exposure. Almost any ISO can be used because the Sun gives 

off abundant light. The easiest method for determining the 

correct exposure is accomplished by running a calibration 

test on the uneclipsed Sun. Shoot a roll of film of the mid-day 

Sun at a fixed aperture (f/8 to f/16) using every shutter speed 

from 1/1000s to 1/4s. After the film is developed, note the best 

exposures and use them to photograph all the partial phases. 

With a digital camera, the process is even easier: shoot a range 

of different exposures and use the camera’s histogram display 

to evaluate the best exposure. The Sun’s surface brightness 

remains constant throughout the eclipse, so no exposure 

compensation is needed except for the narrow crescent phases, 

which require two more stops due to solar limb darkening. 

Bracketing by several stops is also necessary if haze or clouds 

interfere on eclipse day. 

Certainly the most spectacular and awe-inspiring phase 

of an eclipse is totality. For a few brief minutes or seconds, the 

Sun’s pearly white corona, red prominences, and chromosphere 

are visible. The great challenge is to obtain a set of photographs 

that captures these fleeting phenomena. The most important 

point to remember is that during the total phase, all solar 

filters must be removed. The corona has a surface brightness 

a million times fainter than the photosphere, so photographs 

of the corona must be made without a filter. Furthermore, it is 

completely safe to view the totally eclipsed Sun directly with 

the naked eye. No filters are needed, and in fact, they would 

only hinder the view. The average brightness of the corona 

varies inversely with the distance from the Sun’s limb. The 

inner corona is far brighter than the outer corona so no single 

exposure can capture its full dynamic range. The best strategy 

is to choose one aperture or f/number and bracket the exposures 

over a range of shutter speeds (e.g., 1/1000 s to 1s). Rehearsing 

this sequence is highly recommended because great excitement 

accompanies totality and there is little time to think.

Exposure times for various combinations of ISO speeds, 

apertures (f/number) and solar features (chromosphere, prominences, inner, middle, and outer corona) are summarized in 

Table 4.2. The table was developed from eclipse photographs 

made by F. Espenak, as well as from photographs published 

in Sky and Telescope. To use the table, first select the ISO 

speed in the upper left column. Next, move to the right to the 

desired aperture or f/number for the chosen ISO speed. The 

shutter speeds in that column may be used as starting points 

for photographing various features and phenomena tabulated in 

the ‘Subject’ column at the far left. For example, to photograph 

prominences using ISO 400 at f/16, the table recommends an 

exposure of 1/1000. Alternatively, the recommended shutter 

speed can be calculated using the ‘Q’ factors tabulated along 

with the exposure formula at the bottom of Table 4.2. Keep in 

mind that these exposures are based on a clear sky and a corona 

of average brightness. The exposures should be bracketed one 

or more stops to take into account the actual sky conditions 

and the variable nature of these phenomena. 

Point-and-shoot cameras with wide angle lenses are excellent for capturing the quickly changing light in the seconds 

before and during totality. Use a tripod or brace with the camera 

on a wall or fence because slow shutter speeds will be needed. 

In addition, disable or turn off the camera’s electronic flash so 

that it does not interfere with anyone else’s view of the eclipse. 

If the flash cannot be turned off, cover it with black tape.

Another eclipse effect that is easily captured with pointand-shoot cameras should not be overlooked. Use a straw hat 

or a kitchen sieve and allow its shadow to fall on a piece of 

white cardboard placed several feet away. The small holes act 

like pinhole cameras and each one projects its own image of 

the eclipsed Sun. The effect can also be duplicated by forming 

a small aperture with the fingers of one’s hands and watching 

the ground below. The pinhole camera effect becomes more 

prominent with increasing eclipse magnitude. Virtually any 

camera can be used to photograph the phenomenon, but automatic cameras must have their flashes turned off because this 

would otherwise obliterate the pinhole images.

For more information on eclipse photography, observations, and eye safety, see the “Further Reading” sections in 

the References.

4.4 Contact Timings from the Path Limits

Precise timings of beading phenomena made near the 

northern and southern limits of the umbral path (i.e., the 

graze zones), may be useful in determining the diameter of 

the Sun relative to the Moon at the time of the eclipse. Such 

measurements are essential to an ongoing project to try to 

detect changes in the solar diameter.

Because of the conspicuous nature of the eclipse phenomena and their strong dependence on geographical location, 

scientifically useful observations can be made with relatively 

modest equipment. A small telescope of 3- to 5-in (75–125mm) 

aperture, portable shortwave radio, and portable camcorder 

comprise standard equipment used to make such measurements. Time signals are broadcast via shortwave stations such 

as WWV and CHU in North America (5.0, 10.0, 15.0, and 

20.0 MHz are example frequencies to try for these signals 

around the world), and are recorded simultaneously as the 

eclipse is videotaped. Those using video are encouraged to 

use one of the Global Positioning System (GPS) video time 

inserters, such as the Kiwi OSD by PFD systems (http://www.

pfdsystems.com) in order to link specific Baily’s bead events 

with lunar features.

 68 Annular and Total Solar Eclipses of 2010

Observing Eclipses
The safest timing technique consists of observing a projection of the Sun rather than directly imaging the solar disk 

itself. If a video camera is not available, a tape recorder can be 

used to record time signals with verbal timings of each event. 

Inexperienced observers are cautioned to use great care in 

making such observations. 

The method of contact timing should be described in detail, along with an estimate of the error. The precision requirements of these observations are ±0.5s in time, 1 arcsec (~30m) 

in latitude and longitude, and ±20m (~60ft) in elevation. Commercially available GPS receivers are now the easiest and best 

way to determine one’s position to the necessary accuracy. GPS 

receivers are also a useful source for accurate Universal Time 

as long as they use the one-pulse-per-second signal for timing; 

many receivers do not use that, so the receiver’s specifications 

must be checked. The National Marine Electronics Association 

(NMEA) sequence normally used can have errors in the time 

display of several tenths of a second. 

The observer’s geodetic coordinates are best determined 

with a GPS receiver. Even simple handheld models are fine if 

data are obtained and averaged until the latitude, longitude, 

and altitude output become stable. Positions can also be measured from United States Geological Survey (USGS) maps or 

other large scale maps as long as they conform to the accuracy 

requirement above. Some of these maps are available on Web 

sites such as <http://www.topozone.co>. Coordinates determined 

directly from Web sites are useful for checking, but are usually not 

accurate enough for eclipse timings. If a map or GPS is unavailable, then a detailed description of the observing site should 

be included, providing information such as distance and directions of the nearest towns or settlements, nearby landmarks, 

identifiable buildings, and road intersections; digital photos of 

key annotated landmarks are also important.

Expeditions are coordinated by the International Occultation Timing Association (IOTA). For information on possible 

solar eclipse expeditions that focus on observing at the eclipse 

path limits, refer to <http://www.eclipsetours.com>. For specific 

details on equipment and observing methods for observing at 

the eclipse path limits, refer to <http://www.eclipsetours.com/

edge>. For more information on IOTA and eclipse timings, 

contact:

Dr. David W. Dunham, IOTA

Johns Hopkins University/Applied Physics Lab.

MS MP3-135

11100 Johns Hopkins Rd.

Laurel, MD 20723–6099, USA

Phone: (240) 228-5609

E-mail: dunham@starpower.net

Web Site: http://www.lunar-occultations.com/iota

Reports containing graze observations, eclipse contact, 

and Baily’s bead timings, including those made anywhere 

near, or in, the path of totality or annularity can be sent to

Dr. Dunham at the address listed above.

4.5 Plotting Eclipse Paths on Maps

To assist hand-plotting of high-resolution maps of the 

umbral path, high resolution tables of graze zone coordinates 

at longitude increments of 7.5 ́ are available via the NASA Web 

sites for the 2010 annular eclipse <http://eclipse.gsfc.nasa.gov/

SEmono/ASE2010/ASE2010.html>, and the 2010 total eclipse 

<http://eclipse.gsfc.nasa.gov/SEmono/TSE2010/TSE2010.

html>.

Global Navigation Charts (1:5,000,000), Operational Navigation Charts (scale 1:1,000,000), and Tactical Pilotage Charts 

(1:500,000) of the world are published by the National Imagery 

and Mapping Agency. Sales and distribution of these maps are 

through the National Ocean Service. For specific information 

about map availability, purchase prices, and ordering instructions, the National Ocean Service can be contacted by mail, 

telephone, or fax at the following:

NOAA Distribution Division, N/ACC3

National Ocean Service

Riverdale, MD 20737–1199, USA

Phone: (301) 436-8301 or (800) 638-8972

Fax: (301) 436-6829

It is also advisable to check the telephone directory for any 

map specialty stores in a given city or area. They often have 

large inventories of maps available for immediate delivery.

4.6 Eclipse Paths on Google Maps

The 2010 eclipse paths are also plotted on interactive 

Google Maps on the NASA Eclipse Web site. The northern 

and southern path limits of an eclipse path are plotted in blue 

and the central lines are red. The yellow lines crossing the path 

indicate the position of maximum eclipse at 10 min intervals. 

The four-way toggle arrows (upper left corner) are for navigating around the map. The zoom bar (left edge) is used to change 

the magnification. The three buttons (top right) turn on the map 

view, the satellite view, or the hybrid map/satellite view. 

The green marker labeled GE is the point of Greatest 

Eclipse. Clicking anywhere on a map marks a position and 

calculates the eclipse times at that location. Moving the cursor over a marker reveals the eclipse circumstances for that 

position. The marker predictions can also be viewed in a new 

window via the Eclipse Times Popup button. The information 

in the popup window can be selected, copied, and pasted into 

a word processor. All markers can be removed using the Clear 

Markers button above. Choosing the Large Map check box 

produces a bigger map (for users with large monitors and fast 

Internet connections).

The URL for the Google Map of the 2010 annular eclipse 

is <http://eclipse.gsfc.nasa.gov/SEgoogle/SEgoogle2001/SE2010Jan15Agoogle2.html>. The URL for Google Map of the 

2010 total eclipse is <http://eclipse.gsfc.nasa.gov/SEgoogle/

SEgoogle2001/SE2010Jul11Tgoogle2.html>. 

.

Annular and Total Solar Eclipses of 2010 69

Observing Eclipses
Table 4.1:

Field of View and Size of Sun’s Image for Various Photographic Focal Lengths

Focal Length Field of View Field of View Size of Sun

(35mm) (digital)

14 mm 98° x 147° 65° x 98° 0.2 mm

20 mm 69° x 103° 46° x 69° 0.2 mm

28 mm 49° x 74° 33° x 49° 0.2 mm

35 mm 39° x 59° 26° x 39° 0.3 mm

50 mm 27° x 40° 18° x 28° 0.5 mm

105 mm 13° x 19° 9° x 13° 1.0 mm

200 mm 7° x 10° 5°x 7° 1.8 mm

400 mm 3.4° x 5.1° 2.3° x 3.4° 3.7 mm

500 mm 2.7° x 4.1° 1.8° x 2.8° 4.6 mm

1000 mm 1.4° x 2.1° 0.9° x 1,4° 9.2 mm

1500 mm 0.9° x 1.4° 0.6° x 0.9° 13.8 mm

2000 mm 0.7° x 1.0° 0.5° x 0.7° 18.4 mm

Image Size of Sun (mm) = Focal Length (mm) / 109

Table 4.2: Solar Eclipse Exposure Guide

ISO __ ƒ/Number

25 1.4 2 2.8 4 5.6 8 11 16 22

50 2 2.8 4 5.6 8 11 16 22 32

100 2.8 4 5.6 8 11 16 22 32 44

200 4 5.6 8 11 16 22 32 44 64

400 5.6 8 11 16 22 32 44 64 88

800 8 11 16 22 32 44 64 88 128

1600 11 16 22 32 44 64 88 128 176

Subject Q __ Shutter Speed

Solar Eclipse

Partial

1 - 4.0 ND 11 — — — 1/4000 1/2000 1/1000 1/500 1/250 1/125

Partial

1 - 5.0 ND 8 1/4000 1/2000 1/1000 1/500 1/250 1/125 1/60 1/30 1/15

Baily's Beads2 11 — — — 1/4000 1/2000 1/1000 1/500 1/250 1/125

Chromosphere 10 — — 1/4000 1/2000 1/1000 1/500 1/250 1/125 1/60

Prominences 9 — 1/4000 1/2000 1/1000 1/500 1/250 1/125 1/60 1/30

Corona - 0.1 Rs 7 1/2000 1/1000 1/500 1/250 1/125 1/60 1/30 1/15 1/8

Corona - 0.2 Rs3 5 1/500 1/250 1/125 1/60 1/30 1/15 1/8 1/4 1/2

Corona - 0.5 Rs 3 1/125 1/60 1/30 1/15 1/8 1/4 1/2 1 sec 2 sec

Corona - 1.0 Rs 1 1/30 1/15 1/8 1/4 1/2 1 sec 2 sec 4 sec 8 sec

Corona - 2.0 Rs 0 1/15 1/8 1/4 1/2 1 sec 2 sec 4 sec 8 sec 15 sec

Corona - 4.0 Rs -1 1/8 1/4 1/2 1 sec 2 sec 4 sec 8 sec 15 sec 30 sec

Corona - 8.0 Rs -3 1/2 1 sec 2 sec 4 sec 8 sec 15 sec 30 sec 1 min 2 min

Exposure Formula: t = ƒ2 / (I X 2Q) where: t = exposure time (sec)

ƒ = ƒ/number or focal ratio

I = ISO film speed

Q = brightness exponent

Abbreviations: ND = Neutral Density Filter.

Rs = Solar Radii.

Notes: 1 Exposures for partial phases are also good for annular eclipses.

2 Baily's Beads are extremely bright and change rapidly.

3 This exposure also recommended for the 'Diamond Ring' effect.

F. Espenak - 2006 Oct

 70 Annular and Total Solar Eclipses of 2010

Observing Eclipses
 0 500 1000 1500 2000 2500

Wavelength (nm)

Density

SN 14 WELDER'S FILTER

THOUSAND OAKS T2 GLASS

B. R. Chou and F. Espenak, 2004

 0 500 1000 1500 2000 2500

( = log10 (1/Transmittance) ) 0

 1

 2

 3

 4

 5

 6

 7

 8

 3

 4

 5

 6

 7

 8

 2

 3

 4

 5

 6

 7

 8

SOLAR SKREEN

 3

 4

 5

 6

 7

 8

 3

 4

 5

 6

 7

 8

BAADER ASTROSOLAR FILM

PLUS X NEGATIVE

EXPOSED & DEVELOPED FILM

COLOR NEGATIVE (UNSAFE FOR SOLAR VIEWING!)

VISIBLE

 3

 4

 5

 6

 7

 8

THOUSAND OAKS BLACK POLYMER

FIGURE 4.1: SPECTRAL RESPONSE OF SOME COMMONLY AVAILABLE SOLAR FILTERS

Annular and Total Solar Eclipses of 2010 71

Observing Eclipses
0

5

10

15

20

25

30

35

m

m

 Film: 200 mm Digital: 135 mm

FIGURE 4.2 - LENS FOCAL LENGTH VS. IMAGE SIZE FOR ECLIPSE PHOTOGRAPHY

F. Espenak - 2006

The image size of the eclipsed Sun and corona is shown for a range of focal lengths on both 35 mm film 

cameras and digital SLR's which use a CCD 2/3 the size of 35 mm film. Thus, the same lens produces an 

image 1.5 x larger on a digital SLR as compared to film.

(scale for 35 mm film)

 Film: 400 mm Digital: 270 mm Film: 500 mm Digital: 330 mm

 Film: 1000 mm Digital: 670 mm Film: 1500 mm Digital: 1000 mm Film: 2000 mm Digital: 1330 mm

 72 Annular and Total Solar Eclipses of 2010

Observing Eclipses
5. Eclipse Resources

5.1 IAU Working Group on Eclipses

Professional scientists are asked to send descriptions of 

their eclipse plans to the Working Group on Eclipses of the 

Solar Division of the International Astronomical Union (IAU), 

so they can keep a list of observations planned. Send such 

descriptions, even in preliminary form, to:

International Astronomical Union/

Working Group on Eclipses 

Prof. Jay M. Pasachoff, Chair

Williams College–Hopkins Observatory

Williamstown, MA 01267, USA

Fax: (413) 597-3200

E-mail: eclipse@williams.edu

Web Site: http://www.eclipses.info

The members of the Working Group on Eclipses of the 

Solar Division of the IAU are: Jay M. Pasachoff (USA), Chair, 

Iraida S. Kim (Russia), Hiroki Kurokawa (Japan), Jagdev Singh 

(India), Vojtech Rusin (Slovakia), Fred Espenak (USA), Jay 

Anderson (Canada), Glenn Schneider (USA), Michael Gill 

(UK), and Yihua Yan (China).

5.2 IAU Solar Eclipse Education Committee

In order to ensure that astronomers and public health authorities have access to information on safe viewing practices, 

the Commission on Education and Development of the IAU, 

set up a Program Group on Public Education at the Times of 

Eclipses. Under Prof. Jay M. Pasachoff, the Committee has 

assembled information on safe methods of observing solar 

eclipses, eclipse-related eye injuries, and samples of educational materials on solar eclipses (see <http://www.eclipses.

info>).

For more information, contact Prof. Jay M. Pasachoff (contact information is found in Sect. 5.1). Information on safe solar 

filters can be obtained by contacting Program Group member 

Dr. B. Ralph Chou (bchou@sciborg.uwaterloo.ca).

5.3 Solar Eclipse Mailing List

The Solar Eclipse Mailing List (SEML) is an electronic 

news group dedicated to solar eclipses. Published by British 

eclipse chaser Michael Gill (eclipsechaser@yahoo.com), it 

serves as a forum for discussing anything and everything 

about eclipses and facilitates interaction between both the 

professional and amateur communities. 

The SEML is hosted at URL <http://groups.yahoo.com/

group/SEML/>. Complete instructions are available online for 

subscribing and unsubscribing. Up until mid-2004, the list manager of the SEML was Patrick Poitevin (solareclipsewebpages@

btopenworld.com). Archives of past SEML messages through 

July 2004 are available at <http://www.mreclipse.com/SENL/

SENLinde.htm>.

5.4 NASA Eclipse Bulletins on the Internet

To make the NASA solar eclipse bulletins accessible to 

as large an audience as possible, these publications are also 

available via the Internet. The bulletins can be read, or downloaded using a Web browser (Firefox, Safari, Internet Explorer, 

etc.) from the NASA Eclipse Web Site. The top-level Web 

addresses (URLs) for the currently available eclipse bulletins 

are as follows:

Annular Solar Eclipse of 1994 May 10

— http://eclipse.gsfc.nasa.gov/SEpubs/19940510/rp.html

Total Solar Eclipse of 1994 Nov 03

— http://eclipse.gsfc.nasa.gov/SEpubs/19941103/rp.html

Total Solar Eclipse of 1995 Oct 24

— http://eclipse.gsfc.nasa.gov/SEpubs/19951024/rp.html

Total Solar Eclipse of 1997 Mar 09

— http://eclipse.gsfc.nasa.gov/SEpubs/19970309/rp.html

Total Solar Eclipse of 1998 Feb 26

— http://eclipse.gsfc.nasa.gov/SEpubs/19980226/rp.html

Total Solar Eclipse of 1999 Aug 11

— http://eclipse.gsfc.nasa.gov/SEpubs/19990811/rp.html

Total Solar Eclipse of 2001 Jun 21

— http://eclipse.gsfc.nasa.gov/SEpubs/20010621/rp.html

Total Solar Eclipse of 2002 Dec 04

— http://eclipse.gsfc.nasa.gov/SEpubs/20021204/rp.html

Solar Eclipses of 2003: May 31 & Nov 23

— http://eclipse.gsfc.nasa.gov/SEpubs/20030000/rp.html

Total Solar Eclipse of 2006 Mar 29

— http://eclipse.gsfc.nasa.gov/SEpubs/20060329/rp.html

Total Solar Eclipse of 2008 Aug 01

— http://eclipse.gsfc.nasa.gov/SEpubs/20080801/rp.html

Total Solar Eclipse of 2009 Jul 22

— http://eclipse.gsfc.nasa.gov/SEpubs/20090722/rp.html

Annular and Total Solar Eclipses of 2010

— http://eclipse.gsfc.nasa.gov/SEpubs/2010/rp.html

The most recent bulletins are available in “PDF” format. 

All future NASA eclipse bulletins will be available over the 

Internet, at or before publication of each. Comments and suggestions are actively solicited to fix problems and improve on 

compatibility and formats..

5.5 Future Eclipse Paths on the Internet

Presently, the NASA eclipse bulletins are published 

12–24 months before each eclipse, however, there have been a 

growing number of requests for eclipse path data with an even 

greater lead time. To accommodate this need, predictions have 

been generated for all central solar eclipses from 1901 through 

2100. The umbral path characteristics have been calculated 

with a 1 min time interval compared to the 6min interval used 

in Fifty Year Canon of Solar Eclipses: 1986–2035 (Espenak 

1987). This provides enough detail for making preliminary 

plots of the path on larger scale maps. Links to global maps 

using an orthographic projection present the regions of partial 

and total (or annular) eclipse. There are also small animations 

that show the motion of the umbral and penumbral shadows 

Annular and Total Solar Eclipses of 2010 73

Eclipse Resources
across Earth for each eclipse. To present all this information, a 

series of Web pages break the 200 year period into decade-long 

intervals. The Web page for the decade 2001–2010 is: <http://

eclipse.gsfc.nasa.gov/SEcat/SEdecade2001.html>. Links to 

the other decades can be found on this page as well.

Google Maps is an excellent tool for a detailed look at past and 

future eclipse paths. A series of Google Maps Web pages has been 

created for all central eclipses from 1901–2100. The indices and 

links for these maps are arranged in 20-year periods. For example, 

the Web page for the period 2001–2020 is: <http://eclipse.gsfc.

nasa.gov/SEgoogle/SEgoogle2001.html>. Links to the other 

20-year index pages also can be found on this page.

A Web-based search engine has been developed with the 

assistance of Xavier Jubier and Sumit Dutta. It accesses the 

entire catalog of Besselian elements used in Five Millennium 

Canon of Solar Eclipses: –1999 to +3000 (Espenak and Meeus 

2006). The user can search this data by eclipse type, duration, 

and date range. The resulting table has links to coordinate 

tables and eclipse paths plotted on Google Maps. The link 

for Five Millennium Solar Eclipse Search Engine is: <http://

eclipse.gsfc.nasa.gov/SEsearch/SEsearch.php>.

The coordinates of the Sun used in these tables and maps 

were calculated on the basis of the VSOP87 theory constructed 

by Bretagnon and Francou (1988). The Moon ephemeris is 

based on the theory ELP-2000/82 of Chapront-Touze and 

Chapront (1983). Neglecting the smallest periodic terms, the 

Moon’s position calculated in our program has a mean error 

(as compared to the full ELP theory) of about 0.0006 s of time 

in right ascension, and about 0.006 arcsec in declination. The 

corresponding error in the calculated times of the phases of a 

solar eclipse is of the order of 1/40 s, which is much smaller 

than the uncertainties in predicted values of ΔT, and also much 

smaller than the error due to neglecting the irregularities 

(mountains and valleys) in the lunar limb profile. The value 

for ∆T (the difference between Terrestrial Dynamical Time 

and Universal Time) is from direct measurements during 

the 20th century and extrapolation into the 21st century. The 

value used for the Moon’s mean radius is k=0.272281. These 

ephemerides and parameters are identical to those used in Five 

Millennium Canon of Solar Eclipses: –1999 to +3000 (Espenak 

and Meeus 2006). 

5.6 NASA Web Sites for 2010 Solar Eclipses

Two special Web sites have been set up to supplement 

this bulletin with additional predictions, tables, and data for 

the annular and total solar eclipses of 2010. Some of the data 

posted there include: 1) Mapping Coordinates for the Central 

Eclipse Path, and 2) Mapping Coordinates for the Zones of 

Grazing Eclipse. The URL of the NASA Web site for the 

2010 annular eclipse is <http://eclipse.gsfc.nasa.gov/SEmono/

ASE2010/ASE2010.html>. The URL of the NASA Web site for 

the 2010 total eclipse is <http://eclipse.gsfc.nasa.gov/SEmono/

TSE2010/TSE2010.html>.

5.7 Predictions for Eclipse Experiments

This publication provides comprehensive information on 

the 2010 annular and total solar eclipses to the professional, 

amateur, and lay communities. Certain investigations and 

eclipse experiments, however, may require additional information that lies beyond the scope of this work. The authors invite 

the international professional community to contact them 

for assistance with any aspect of eclipse prediction including predictions for locations not included in this publication, 

or for more detailed predictions for a specific location (e.g., 

lunar limb profile and limb-corrected contact times for an 

observing site).

This service is offered for the 2010 eclipses, as well as 

for previous eclipses in which analysis is still in progress. To 

discuss individual needs and requirements, please contact Fred 

Espenak (fred.espenak@nasa.gov).

5.8 Algorithms, Ephemerides, and Parameters

Algorithms for the eclipse predictions were developed 

by Espenak primarily from the Explanatory Supplement (Her 

Majesty’s Nautical Almanac Office 1974), with additional algorithms from Meeus et al. (1966), and Meeus (1989). The solar 

and lunar ephemerides were generated from the JPL DE200 

and LE200, respectively. All eclipse calculations were made 

using a value for the Moon’s radius of k = 0.2722810 for umbral 

contacts, and k = 0.2725076 (adopted IAU value) for penumbral 

contacts. Center of mass coordinates were used except where 

noted. Extrapolating from 2008 to 2010, values for ∆T of 66.0 s 

(annular eclipse) and 66.2s (total eclipse) were used to convert 

the predictions from Terrestrial Dynamical Time to Universal 

Time. The international convention of presenting date and time 

in descending order has been used throughout the bulletin (i.e., 

year, month, day, hour, minute, second).

The primary source for geographic coordinates used in 

the local circumstances tables is The New International Atlas

(Rand McNally 1991). Elevations for major cities were taken 

from Climates of the World (U.S. Dept. of Commerce 1972). 

The names and spellings of countries, cities, and other geopolitical regions are not authoritative, nor do they imply any 

official recognition in status. Corrections to names, geographic 

coordinates, and elevations are actively solicited in order to 

update the database for future eclipse bulletins.

AUTHOR’S NOTE

All eclipse predictions presented in this publication were 

generated on a Macintosh Dual 1.25 GHz PowerPC G4 computer. All calculations, diagrams, and opinions presented in 

this publication are those of the authors and they assume full 

responsibility for their accuracy.

 74 Annular and Total Solar Eclipses of 2010

Eclipse Resources
ACRONYMS

AIDS Acquired Immune Deficiency Syndrome

CAR Central African Republic

CD Compact Disk

DCW Digital Chart of the World

DMA Defense Mapping Agency (U.S.)

DRC Democratic Republic of the Congo

DSLR Digital-Single Lens Reflex

GPS Global Positioning System

IAU International Astronomical Union

IOTA International Occultation Timing Association

ISO International Organization for Standardization

ITCZ Intertropical Convergence Zone

JNC Jet Navigation Charts

JPL Jet Propulsion Laboratory

NMEA National Marine Electronics Association

ONC Operational Navigation Charts

SASE Self Addressed Stamped Envelope

SEML Solar Eclipse Mailing List

SLR Single Lens Reflex

SPCZ South Pacific Convergence Zone

TDT Terrestrial Dynamical Time

TP Technical Publication

USGS United States Geological Survey

UT Universal Time

UV Ultraviolet

UVA Ultraviolet-A

WDBII World Data Bank II

UNITS

arcmin arc minute

arcsec arc second

ft foot

h hour

Hz Hertz

km kilometer

m meter

MHz MegaHertz

min minute

mm millimeter

nm nanometer

s second

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Annular and Total Solar Eclipses of 2010 77

 Acronyms, Units, and References
R EQUEST F ORM FOR NASA E CLIPSE B ULLETINS

NASA eclipse bulletins contain detailed predictions, maps and meteorology for future central solar eclipses 

of interest. Published as part of NASA's Technical Publication (TP) series, the bulletins are prepared in 

cooperation with the Working Group on Eclipses of the International Astronomical Union and are provided 

as a public service to both the professional and lay communities, including educators and the media. In 

order to allow a reasonable lead time for planning purposes, subsequent bulletins will be published 12 to 24 

months before each event. Comments, suggestions and corrections are solicited to improve the content and 

layout in subsequent editions of this publication series.

Single copies of the bulletins are available at no cost and may be ordered by sending a 9 x 12 inch 

SASE (self addressed stamped envelope) with sufficient postage for each bulletin (12 oz. or 340 g).

Use stamps only since cash or checks cannot be accepted. Requests within the U. S. may use the Postal 

Service's Priority Mail. Please print either the eclipse date (year & month) or NASA publication number in 

the lower left corner of the SASE and return with this completed form to either of the authors. Requests 

from outside the U. S. and Canada may use ten international postal coupons to cover postage. Exceptions to 

the postage requirements will be made for international requests where political or economic restraints 

prevent the transfer of funds to other countries. Professional researchers and scientists are exempt from the 

SASE requirements provided the request comes on their official or institutional stationary.

Permission is freely granted to reproduce any portion of this NASA Reference Publication. All uses and/or 

publication of this material should be accompanied by an appropriate acknowledgment of the source.

Request for: NASA TP-2008-214171—Annular and Total Solar Eclipses of 2010

Name of Organization: __________________________________________________________

(in English, if necessary): __________________________________________________________

Name of Contact Person: __________________________________________________________

Address: __________________________________________________________

__________________________________________________________

City/State/ZIP: __________________________________________________________

Country: __________________________________________________________

E-mail: __________________________________________________________

Type of organization: ___ University/College ___ Observatory ___ Library

(check all that apply) ___ Planetarium ___ Publication ___ Media

___ Professional ___ Amateur ___ Individual

Size of Organization: _______ (Number of Members)

* * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * * 

Return Requests Fred Espenak or Jay Anderson

and Comments to: NASA/GSFC Royal Astronomical Society of Canada

Code 693 189 Kingsway Ave.

Greenbelt, MD 20771 Winnipeg, MB, 

USA CANADA R3M 0G4

E-mail: fred.espenak@nasa.gov E-mail: jander@cc.umanitoba.ca

2008 Oct