NASA/TP—2007–214149

Total Solar Eclipse of 2008 August 01

F. Espenak and J. Anderson

March 2007
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March 2007

NASA/TP—2007–214149

Total Solar Eclipse of 2008 August 01

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
F. Espenak and J. Anderson

iii 

Preface

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

future central 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 18 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. (340 g). Detailed instructions and an order form can be found at the back of this publication.

The 2008 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 1:5,000,000 to 1:6,000,000 in order to show roads, 

cities and villages, and lakes and rivers, making them suitable for eclipse expedition planning. 

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. 3.1). 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.

Dr. Joe Gurman (GSFC/Solar Physics Branch) has made this and previous eclipse bulletins available over the Internet. They 

can be read or downloaded via the World Wide Web from Goddard’s Solar Data Analysis Center eclipse information page 

http://umbra.nascom.nasa.gov/eclipse/.

The NASA Eclipse Home Page 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 Home Page is http://sunearth.gsfc.nasa.gov/eclipse/eclipse.html.

In addition to the synoptic data provided by the Web site above, a special page for the 2008 total solar eclipse has been prepared: http://sunearth.gsfc.nasa.gov/eclipse/SEmono/TSE2008/TSE2008.html. It includes 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 upon 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 lifelong interest in eclipse prediction. Prof. Jay M. Pasachoff reviewed the manuscript and offered many helpful suggestions. Dr. 

David Dunham and Paul Maley reviewed and updated the information about eclipse contact timings. Internet availability of 

the eclipse bulletins is due to the efforts of Dr. Joseph B. Gurman. The support of Environment Canada is acknowledged in 
Total Solar Eclipse of 2008 August 01

iv

the acquisition of the weather data.

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 Total Solar Eclipse of 2008 August 01, Espenak and Anderson 2007”). 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: espenak@gsfc.nasa.gov E-mail: jander@cc.umanitoba.ca

Fax: (301) 286-0212

Past and Future 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

- - - - - - - - - - - future - - - - - - - - - - -

Total Solar Eclipse of 2009 July 22 — 2008

Total Solar Eclipse of 2010 July 11 — 2009
F. Espenak and J. Anderson

v 

Table of Contents

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

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

1.2 Umbral Path and Visibility. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1

1.3 Orthographic Projection Map of the Eclipse Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.4 Stereographic Projection Map of the Eclipse Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.5 Equidistant Conic Projection Map of the Eclipse Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.6 Detailed Maps of the Umbral Path. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

1.7 Elements, Shadow Contacts, and Eclipse Path Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3

1.8 Local Circumstances Tables. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4

1.9 Estimating Times of Second and Third Contacts. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5

1.10 Mean Lunar Radius. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6

1.11 Lunar Limb Profile. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6

1.12 Limb Corrections to the Path Limits: Graze Zones. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

1.13 Saros History. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

2. WEATHER PROSPECTS FOR THE ECLIPSE. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

2.1 Overview. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

2.2 The Canadian Archipelago. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

2.3 Northern Greenland. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10

2.4 Spitzbergen Island to the Russian Coast. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10

2.5 Siberia. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

2.6 Local Conditions Around Novosibirsk. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

2.7 China. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12

2.8 Local Conditions Around Hami. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12

2.9 Local Conditions Near Xi’an. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13

2.10 Getting Weather Information. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13

2.11 Summary. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14

3. OBSERVING THE ECLIPSE. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14

3.1 Eye Safety and Solar Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14

3.2 Sources for Solar Filters. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 16

3.3 Eclipse Photography. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17

3.4 Sky at Totality. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18

3.5 Contact Timings from the Path Limits. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18

3.6 Plotting the Path on Maps. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

4. ECLIPSE RESOURCES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

4.1 IAU Working Group on Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

4.2 IAU Solar Eclipse Education Committee. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

4.3 Solar Eclipse Mailing List. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

4.4 The 2007 International Solar Eclipse Conference. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

4.5 NASA Eclipse Bulletins on the Internet. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

4.6 Future Eclipse Paths on the Internet. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

4.7 NASA Web Site for 2008 Total Solar Eclipse. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

4.8 Predictions for Eclipse Experiments. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21

4.9 Algorithms, Ephemerides, and Parameters. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21

AUTHOR’S NOTE. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21

TABLES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23

FIGURES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 45

ACRONYMS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

UNITS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

BIBLIOGRAPHY. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

Further Reading on Eclipses. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 67

Further Reading on Eye Safety. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68

Further Reading on Meteorology. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68

F. Espenak and J. Anderson

1 

1. Eclipse Predictions

1.1 Introduction

On Friday, 2008 August 01, a total eclipse of the Sun is 

visible from within a narrow corridor that traverses half of 

Earth. The path of the Moon’s umbral shadow begins in northern Canada and extends across Greenland, the Arctic, central 

Russia, Mongolia, and China (Espenak and Anderson, 2006). 

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

Moon’s penumbral shadow, which includes northeastern North 

America, most of Europe, and Asia (Figures 1 and 2).

1.2 Umbral Path and Visibility

The path of totality begins in northern Canada (Figure 

3), where the Moon’s umbral shadow first touches down in 

the territory of Nunavut at 09:21 UT (Universal Time). Along 

the sunrise terminator in Queen Maud Gulf, the duration is 

1min 30s from the center of the 206 km wide path. Traveling 

over 9 km/s, the umbra quickly sweeps north across southern 

Victoria Island, Prince of Wales Island, and Northern Somerset 

Island (Figure 4). The shadow’s northern limit clips the southeastern corner of Cornwallis Island and just misses the high 

Arctic town of Resolute. The ~200 residents of this isolated 

settlement will witness a partial eclipse of magnitude 0.997 

at 09:26 UT with the Sun 7° above the horizon. 

Continuing on its northeastern trajectory, the umbra 

crosses Devon Island and reaches the southern coast of Ellesmere Island where it engulfs the tiny hamlet of Grise Fiord. The 

duration of total eclipse here is 1min 38s. The central line cuts 

across Nares Strait as the shadow straddles Ellesmere Island 

and Greenland (Figure 5). Canada’s remote outpost Alert, the 

northernmost permanently inhabited place on Earth, lies near 

the northern limit of the eclipse track and experiences 43 s of 

totality with the Sun at 16° altitude at 09:32 UT.

The northern half of the path encounters the open Arctic, 

while the southern half cuts across the many fjords of northern Greenland. Leaving the coast of Greenland, the shadow 

reaches its northernmost latitude (83° 47 ́) at 09:38 UT as it 

traverses the landless Arctic Ocean. Slowly curving to the 

southeast, the track passes between Franz Josef Land and 

Svalbard where George Land and Kvitoya Island are cut by 

its northern and southern limits, respectively (Figure 6). By 

the time the central line reaches the northern coast of Novaya 

Zemlya (10:00UT), the duration is 2min 23s with the Sun at 

31° (Figures 7 and 8). The track crosses both the island and the 

Kara Sea before reaching the Yamal Peninsula and the Russian 

mainland at 10:10 UT (Figures 8).

The instant of greatest eclipse occurs at 10:21:07 UT 

(latitude 65° 39 ́N, longitude 72° 18 ́E) when the axis of the 

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

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).

= +0.8307). When totality reaches its maximum duration of 

2min 27s, the Sun’s altitude is 34°, the path width is 237km, 

and the umbra’s velocity is 0.908km/s. The Russian city of 

Nadym (pop.ulation ~46,000) lies nearby and only loses 1 s of 

totality because of its short distance (~14 km) from the central 

line (Figure 9).

During the next hour, the Moon’s umbra works its way 

across central Asia. The shadow gradually picks up speed and 

its course changes from south-southeast to nearly east at its 

terminus (Figure 7). Central Russia is sparsely populated, however, there are a few small cities in the path of totality including 

Megion, Nizhnevartovsk, and Strezhevoy (Figure 10).

Novosibirsk, Russia’s third most populous city (pop. ~1.4 

million), lies only 18km from the central line. The midpoint 

of Novosibirsk’s 2min 18s total eclipse occurs at 10:45 UT 

with the Sun’s altitude at 30° (Figures 10 and 11). Three and 

a half minutes later, Barnaul (pop. ~600,000) is plunged into 

a 2min 16 s total eclipse.

As the umbral shadow exits Russia, it briefly encompasses the intersection of four nations: Russian, Kazakhstan, 

China, and Mongolia. After crossing the Altay Mountains, 

the center of the track follows the China-Mongolia border for 

several hundred kilometers while the central duration and the 

Sun’s altitude decrease (Figure 12). During this period, the 

central line crosses from Mongolia to China to Mongolia and 

finally back to China where it remains until the end of the 

eclipse track.

From Altay, China, the total eclipse begins at 10:59 UT 

and lasts 1min 25s with the Sun 25° above the horizon. Across 

the border, western Mongolia is very sparsely populated and 

the Altan Mountains bring cloudiness to the area. Ten minutes 

later, the umbra just misses Hami, China (pop. ~137,000) where 

a deep partial eclipse of magnitude 0.998 occurs at 11:10 UT. 

About 140km east of Hami, Yiwu lies just 25 km southwest of 

the central line (Figure 13). Inhabitants of this small town witness a total eclipse lasting 1min 56s with the Sun at an altitude 

of 19°. This region in northwest China is noteworthy because 

it offers some of the most promising weather prospects along 

the entire eclipse path. Its position between the Gobi Desert 

to the east and the Talikmakan Desert to the west spares it 

from the monsoon systems that affect much of Southeast Asia 

during the summer months.

During the final 10 min of the umbra’s track, it quickly 

sweeps across northern China as the duration of totality and 

the Sun’s altitude continue to decrease. Juiquan (pop. ~73,000) 

lies in the path near the southern limit, but it still experiences a 

total eclipse lasting 1min 08 s at 11:15 UT (Figure 14). Further 

east, the major city of Xi’an (pop. ~3.9 million) straddles the 

southern limit where maximum eclipse occurs with the Sun 

just 4° above the horizon (Figure 15). From the central line, 

106km to the north, the duration of totality still lasts 1min 35s. 

Seconds later, the Moon’s shadow lifts off Earth and the total 

eclipse ends (11:21 UT). Over the course of 2h, the Moon’s 

umbra travels along a path approximately 10,200 km long and 

covers 0.4% of Earth’s surface area.
Total Solar Eclipse of 2008 August 01

2

1.3 Orthographic Projection Map of the Eclipse 

Path

Figure 1 is an orthographic projection map of Earth 

(adapted from Espenak 1987) showing the path of penumbral 

(partial) and umbral (total) eclipse. The daylight terminator 

is plotted for the instant of greatest eclipse with north at the 

top. The sub-Earth point 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 

southern boundary lies the limit of the penumbra’s path. 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. 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 travels west to east within the 

penumbral path.

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 10min in Universal Time. Curves of constant 

eclipse magnitude2 delineate the locus of all points where the 

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 Figure 1, the Universal Time of geocentric 

conjunction between the Moon and Sun is given for equatorial 

and ecliptic coordinates followed by the instant of greatest 

eclipse. The eclipse magnitude is given for greatest eclipse. It 

is equivalent to the geocentric 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.

2. 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 

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%).

1.4 Stereographic Projection Map of the Eclipse 

Path

The stereographic projection of Earth in Figure 2 depicts 

the path of penumbral and umbral eclipse in greater detail. The 

map is oriented with north up. International political borders 

are shown and circles of latitude and longitude are plotted at 

30° increments. The region of penumbral or partial eclipse 

is identified by its southern limit, curves of eclipse begins or 

ends at sunrise and sunset, and curves of maximum eclipse at 

sunrise and sunset. Curves of constant eclipse magnitude are 

plotted for magnitudes 0.20, 0.40, 0.60, and 0.80, as are the 

limits of the path of total eclipse. Also included are curves of 

greatest eclipse at every half hour Universal Time.

Figures 1 and 2 may be used to quickly determine the 

approximate time and magnitude of maximum eclipse at any 

location within the eclipse path.

1.5 Equidistant Conic Projection Map of the 

Eclipse Path

Figures 3 and 7 are maps using an equidistant conic 

projection chosen to minimize distortion, and that isolate the 

Arctic and Asian portions of the umbral path. Curves of maximum eclipse and constant eclipse magnitude are plotted and 

labeled at intervals of 30min and 0.2 magnitudes, respectively. 

A linear scale is included for estimating approximate distances 

(in kilometers). Within the northern and southern limits of the 

path of totality, the outline of the umbral shadow is plotted at 

intervals of 5min or 10min. The duration of totality (minutes 

and seconds) and the Sun’s altitude correspond to the local 

circumstances on the central line at each shadow position.

1.6 Detailed Maps of the Umbral Path

The path of totality is plotted on a series of detailed maps 

appearing in Figures 4 to 6 and 8 to 15. The maps were chosen 

to isolate small regions along the entire land portion of the 

eclipse path. Curves of maximum eclipse are plotted at 5 min 

intervals along the track and labeled with the central line duration of 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 of the detailed maps varies from map to map 

depending partly on the population density and accessibility. 

The approximate scale of each map is as follows:

Figures 4 to 6 1:6,000,000

Figure 8 1:5,600,000

Figures 9 to 15 1:5,000,000

The scale of the maps 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. 
F. Espenak and J. Anderson

3 

Whenever possible, current names have been substituted for 

those in the database, but this correction has not been applied 

in all instances.

While Tables 1 to 6 deal with eclipse elements and specific 

characteristics of the path, the northern and southern limits, as 

well as the central line of the path, are plotted using data from 

Table 7. Although no corrections have been made for center of 

figure or lunar limb profile, they have little or no effect at this 

scale. 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 eclipse duration, 

i.e., totality, which are plotted within the path at 1/2min increments. These curves permit fast determination of approximate 

durations without consulting any tables.

No distinction is made between major highways and 

second-class soft-surface roads, 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 coordinates in Table 8. See Sect. 3.6 “Plotting 

the Path on Maps” for sources and more information. The paths 

also show the curves of maximum eclipse at 5min increments 

in Universal Time. These maps are also available at the NASA 

Web site for the 2008 total solar eclipse: http://sunearth.gsfc.

nasa.gov/eclipse/SEmono/TSE2008/TSE2008.html.

1.7 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 Table 1. The eclipse elements and predictions were derived from the DE200 and LE200 ephemerides 

(solar and lunar, respectively) developed jointly by the Jet 

Propulsion Laboratory 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. 1.11 “Lunar Limb Profile”). Times are expressed in 

either Terrestrial Dynamical Time (TDT) or in Universal Time, 

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 

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 f1

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 = 10.00 TDT.

The polynomial Besselian elements were derived from a 

least-squares fit to elements rigorously calculated at five separate times over a 6h period centered at t0; thus, the equation and 

elements are valid over the period 7.0 ≤ t1 ≤ 13.0 TDT.

Table 2 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).

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 (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 (total eclipse ends).

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

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 3min intervals (in Universal Time) in Table 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 umbral duration are calculated for the 
Total Solar Eclipse of 2008 August 01

4

central line position. Table 4 presents a physical ephemeris for 

the umbral shadow at 3min 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 central 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 umbral phase is given.

Local circumstances for each central line position, listed 

in Tables 3 and 4, are presented in Table 5. The first three 

columns give the Universal Time of maximum eclipse, the 

central line duration of 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 (total eclipse begins).

Third Contact: Instant of last internal tangency between the 

Moon and Sun (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.

Table 6 presents topocentric values from the central path 

at maximum eclipse for the Moon’s horizontal parallax, semidiameter, 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. This geometry is described 

in greater detail in the Sect. 1.12 “Limb Corrections to the Path 

Limits: Graze Zones.” Corrections to central line durations due 

to the lunar limb profile are also included. When added to the 

durations in Tables 3, 4, 5, and 7, a slightly shorter central total 

phase is predicted along most of the path because of several 

deep valleys along the Moon’s western limb.

To aid and assist in the plotting of the umbral path on 

large scale maps, the path coordinates are also tabulated at 1° 

intervals in longitude in Table 7. The latitude of the northern 

limit, southern limit, and central line for each longitude is 

tabulated to the nearest hundredth of an arc minute (~18.5m 

at the Equator) along with the Universal Time of maximum 

eclipse at the central line position. Finally, local circumstances 

on the central line at maximum eclipse are listed and include 

the Sun’s altitude and azimuth, the umbral path width, and the 

central duration of totality.

In applications where the zones of grazing eclipse are 

needed in greater detail, Table 8 lists these coordinates over 

land-based portions of the path at 1° intervals in longitude. 

The time of maximum eclipse is given at both northern and 

southern limits, as well as the path’s azimuth. The elevation 

and scale factors are also given (see Sect. 1.11 “Limb Corrections to the Path Limits: Graze Zones”). Expanded versions of 

Tables 7 and 8 using longitude steps of 7.5 ́ are available at the 

NASA 2008 Total Solar Eclipse Web site: http://sunearth.gsfc.

nasa.gov/eclipse/SEmono/TSE2008/TSE2008.html.

1.8 Local Circumstances Tables

Local circumstances for 308 cities; metropolitan areas; 

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

presented in Tables 9 to 16. The tables give the local circumstances at each contact and at maximum eclipse for every 

location. (For partial eclipses, maximum eclipse is the instant 

when the greatest fraction of the Sun’s diameter is occulted. For 

total eclipses, maximum eclipse is the instant of 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 

umbral 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 unitless parameter, 

which is defined as

 u = 1 – (2 x/W), (2)
F. Espenak and J. Anderson

5 

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 totality on the central line 

(in seconds), 

d is the duration of totality at location (in seconds), 

and 

u is the umbral depth. 

The final column gives the duration of 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.

For countries in the path of totality, expanded versions of 

the local circumstances tables listing additional locations are 

available via the NASA Web site for the 2008 total solar eclipse: 

http://sunearth.gsfc.nasa.gov/eclipse/SEmono/TSE2008/

TSE2008.html.

1.9 Estimating Times of Second and Third 

Contacts

The times of second and third contact for any location not 

listed in this publication can be estimated using the detailed 

maps (Figures 4 to 15). Alternatively, the contact times can be 

estimated from maps on which the umbral path has been plotted. Table 7 lists the path coordinates conveniently arranged 

in 1° increments of longitude to assist plotting by hand. The 

path coordinates in Table 3 define a line of maximum eclipse 

at 3min increments in time. These lines of maximum eclipse 

each represent the projection diameter of the umbral shadow at 

the given time; thus, any point on one of these lines will witness 

maximum eclipse (i.e., mid-totality) at the same instant. The 

coordinates in Table 3 should be plotted on the map in order 

to construct lines of maximum eclipse.

The estimation of contact times for any one point begins 

with an interpolation for the time of maximum eclipse at that 

location. The time of maximum eclipse is proportional to 

a point’s distance between two adjacent lines of maximum 

eclipse, measured along a line parallel to the central line. This 

relationship is valid along most of the path with the exception 

of the extreme ends, where the shadow experiences its largest 

acceleration. The central line duration of totality D and the 

path width W are similarly interpolated from the values of the 

adjacent lines of maximum eclipse as listed in Table 3. Because 

the location of interest probably does not lie on the central line, 

it is useful to have an expression for calculating the duration 

of totality d (in seconds) as a function of its perpendicular 

distance a from the central line:

 d = D [1 – (2 a/W)2]1/2, (4)

where: 

d is the duration of totality at location (in seconds), 

D is the duration of totality on the central line (in seconds), 

a is the perpendicular distance from the central line (in 

kilometers), and 

W is the width of the path (kilometers). 

If tm is the interpolated time of maximum eclipse for the location, then the approximate times of second and third contacts 

(t2 and t3, respectively) follow:

Second Contact: t2 = tm – d/2; (5)

Third Contact: t3 = tm + d/2. (6)

The position angles of second and third contact (either P

or V) for any location off the central line are also useful in 

some applications. First, linearly interpolate the central line 

position angles of second and third contacts from the values 

of the adjacent lines of maximum eclipse as listed in Table 5. 

If X2 and X3 are the interpolated central line position angles 

of second and third contacts, then the position angles x2 and 

x3 of those contacts for an observer located a kilometers from 

the central line are

Second Contact: x2 = X2 – arcsin (2 a/W), (7)

Third Contact: x3 = X3 + arcsin (2 a/W), (8)

where:

xn is the interpolated position angle (either P or V) of contact n at location, 

Xn is the interpolated position angle (either P or V) of 

contact n on central line, 

a is the perpendicular distance from the central line in 

kilometers (use negative values for locations south of 

the central line), and 

W is the width of the path in kilometers.
Total Solar Eclipse of 2008 August 01

6

1.10 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 

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 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 central 

durations, which are closer to the actual durations at total 

eclipses, this document departs from standard 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: -1999–3000 (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.

1.11 Lunar Limb Profile

Eclipse contact times, magnitude, and duration of 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) have shown 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 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.

Along the 2008 eclipse path, the Moon’s topocentric libration (physical plus optical) in longitude ranges from l = +4.6° 

to l=+3.6°; 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 16 includes corrections for center of mass and ellipticity 
F. Espenak and J. Anderson

7 

(Morrison and Appleby 1981). It is generated for 11:00 UT, 

which corresponds to northern China near Altay. The Moon’s 

topocentric libration is l=+3.80°, and the topocentric semidiameters of the Sun and Moon are 945.5 and 980.2arcsec, 

respectively. The Moon’s angular velocity with respect to the 

Sun is 0.539 arcsec/s. 

The radial scale of the limb profile in Figure 16 (at bottom) 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 11:00 UT, while the 

times of the four eclipse contacts at that 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 central 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 

Figure 16, 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 (arc seconds) from the mean lunar 

limb is then converted to a time correction ∆ by

∆ = dv cos[X – C], (10)

where: 

∆ 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 Figure 16. 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. For example, 

Table 16 gives the following data for Yiwi, China:

Second Contact = 11:08:09.6UT P2=129°, and 

Third Contact = 11:10:05.7UT P3=286°.

Using Figure 16, the measured time corrections and the resulting contact times are

C2= –1.2 s;

Second Contact = 11:08:09.6 –1.2 s = 11:08:08.4UT, and

C3= –1.1 s;

Third Contact = 11:10:05.7 –1.1 s= 11:10:04.6UT.

The above corrected values are within 0.2 s of a rigorous calculation using the true limb profile.
Total Solar Eclipse of 2008 August 01

8

1.12 Limb Corrections to the Path Limits: 

Graze Zones

The northern and southern umbral limits provided in this 

publication were derived using the Moon’s center of mass 

and a mean lunar radius. They have not been corrected for 

the Moon’s center of figure or the effects of the lunar limb 

profile. In applications where precise limits are required, 

Watts’s limb data must be used to correct the nominal or 

mean path. Unfortunately, a single correction at each limit is 

not possible because the Moon’s libration in longitude and the 

contact points of the limits along the Moon’s limb each vary 

as a function of time and position along the umbral path. This 

makes it necessary to calculate a unique correction to the limits 

at each point along the path. Furthermore, the northern and 

southern limits of the umbral path are actually paralleled by a 

relatively narrow zone where the eclipse is neither penumbral 

nor umbral. An observer positioned here will witness a slender 

solar crescent that is fragmented into a series of bright beads 

and short segments whose morphology changes quickly with 

the rapidly varying geometry between the limbs of the Moon 

and the Sun. These beading phenomena are caused by the 

appearance of photospheric rays that alternately pass through 

deep lunar valleys and hide behind high mountain peaks, as 

the Moon’s irregular limb grazes the edge of the Sun’s disk. 

The geometry is directly analogous to the case of grazing occultations of stars by the Moon. The graze zone is typically 

5–10km wide and its interior and exterior boundaries can be 

predicted using the lunar limb profile. The interior boundaries 

define the actual limits of the umbral eclipse (both total and 

annular) while the exterior boundaries set the outer limits of 

the grazing eclipse zone.

Table 6 provides topocentric data and corrections to the 

path limits due to the true lunar limb profile. At 3min intervals, the table lists the Moon’s topocentric horizontal parallax, 

semi-diameter, relative angular velocity with respect to the 

Sun, and lunar libration in longitude. The Sun’s central line 

altitude and azimuth is given, followed by the azimuth of the 

umbral path. The position angle of the point on the Moon’s 

limb, which defines the northern limit of the path, is measured 

counterclockwise (i.e., eastward) from the equatorial north 

point on the limb. The path corrections to the northern and 

southern limits are listed as interior and exterior components 

in order to define the graze zone. Positive corrections are in the 

northern sense, while negative shifts are in the southern sense. 

These corrections (minutes of arc in latitude) may be added 

directly to the path coordinates listed in Table 3. Corrections to 

the central line umbral durations due to the lunar limb profile 

are also included and they are almost all positive; thus, when 

added to the central durations given in Tables 3, 4, 5, and 7, a 

slightly shorter central total phase is predicted. This effect is 

caused by a significant departure of the Moon’s eastern limb 

from both the center of figure and center of mass limbs and 

to several deep valleys along the Moon’s western limb for the 

predicted libration during the 2008 eclipse.

Detailed coordinates for the zones of grazing eclipse at 

each limit for all land-based sections of the path are presented 

in Table 8. Given the uncertainties in the Watts data, these 

predictions should be accurate to ±0.3 arcsec. (The interior 

graze coordinates take into account the deepest valleys along 

the Moon’s limb, which produce the simultaneous second and 

third contacts at the path limits; thus, the interior coordinates 

that define the true edge of the path of totality.) They are 

calculated from an algorithm that searches the path limits 

for the extreme positions where no photospheric beads are 

visible along a ±30° segment of the Moon’s limb, symmetric 

about the extreme contact points at the instant of maximum 

eclipse. The exterior graze coordinates are arbitrarily defined 

and calculated for the geodetic positions where an unbroken 

photospheric crescent of 60° in angular extent is visible at 

maximum eclipse.

In Table 8, the graze zone latitudes are listed every 1° 

in longitude (at sea level) and include the time of maximum 

eclipse at the northern and southern limits, as well as the path’s 

azimuth. To correct the path for locations above sea level, Elev 

Fact (elevation factor) is a multiplicative factor by which the 

path must be shifted north or south perpendicular to itself, 

i.e., perpendicular to path azimuth, for each unit of elevation 

(height) above sea level. 

The elevation factor is the product, tan(90–A) × sin(D), 

where A is the altitude of the Sun, and D is the difference 

between the azimuth of the Sun and the azimuth of the limit 

line, with the sign selected to be positive if the path should 

be shifted north with positive elevations above sea level. To 

calculate the shift, a location’s elevation is multiplied by the 

elevation factor value. Negative values (usually the case for 

eclipses in the Northern Hemisphere) indicate that the path 

must be shifted south. For instance, if one’s elevation is 1000m 

above sea level and the elevation factor value is –0.50, then 

the shift is –500m (= 1000m × –0.50); thus, the observer must 

shift the path coordinates 500m in a direction perpendicular 

to the path and in a negative or southerly sense. 

The final column of Table 8 lists the Scale Fact (in kilometers per arc second). This scaling factor provides an indication 

of the width of the zone of grazing phenomena, because of the 

topocentric distance of the Moon and the projection geometry 

of the Moon’s shadow on Earth’s surface. Because the solar 

chromosphere has an apparent thickness of about 3 arcsec, 

and assuming a scaling factor value of 3.5km/arcsec, then the 

chromosphere should be visible continuously during totality 

for any observer in the path who is within 10.5 km (=3.5 × 3) 

of each interior limit. The most dynamic beading phenomena, 

however, occurs within 1.5arcsec of the Moon’s limb. Using the 

above scaling factor, this translates to the first 5.25 km inside 

the interior limits, but observers should position themselves 

at least 1 km inside the interior limits (south of the northern 

interior limit or north of the southern interior limit) in order to 

ensure that they are inside the path because of small uncertainties in Watts’s data and the actual path limits.

For applications where the zones of grazing eclipse are 

needed at a higher frequency of longitude interval, tables of 

coordinates every 7.5 ́ in longitude are available via the NASA 

Web site for the 2008 total solar eclipse: http://sunearth.gsfc.

nasa.gov/eclipse/SEmono/TSE2008/TSE2008.html. 
F. Espenak and J. Anderson

9 

1.13 Saros History

The periodicity and recurrence of solar (and lunar) eclipses 

is governed by the Saros cycle, a period of approximately 

6,585.3d (18yr 11 d 8h). When two eclipses are separated by 

a period of one Saros, they share a very similar geometry. 

The eclipses occur at the same node with the Moon at nearly 

the same distance from Earth and at the same time of year, 

thus, the Saros is useful for organizing eclipses into families 

or series. Each series typically lasts 12 or 13 centuries and 

contains 70 or more eclipses.

The total eclipse of 2008 is the 47th member of Saros series 

126 (Table 17), as defined by van den Bergh (1955). All eclipses 

in an even numbered Saros series occur at the Moon’s descending node and the Moon moves northward with each succeeding 

member in the family (i.e., gamma increases). Saros 126 is a 

senior-aged series that began with a small partial eclipse at high 

southern latitudes on 1179 Mar 10. After eight partial eclipses, 

each of increasing magnitude, the first umbral eclipse occurred 

on 1323 Jun 04. This event was a central annular eclipse with 

no southern limit (Espenak and Meeus, 2006). 

For the next five centuries, the series produced 27 more 

annular eclipses. On 1828 Apr 14, the first hybrid or annular 

total eclipse occurred. The nature of such an eclipse changes 

from annular to total or vice versa along different portions of 

the track. The dual nature arises from the curvature of Earth’s 

surface, which brings the middle part of the path into the umbra (total eclipse) while other, more distant segments remain 

within the antumbral shadow (annular eclipse).

Such hybrid eclipses are rather rare and account for only 

4.8% of the 11,898 solar eclipses occurring during the five 

millennium period from –1999 to +3000 (Espenak and Meeus, 

2006). The next two eclipses of Saros 126 were also hybrid with 

a steadily increasing duration of totality at greatest eclipse. The 

first purely total eclipse of the series occurred on 1882 May 17 

and had a maximum duration of 1min 50s.

Throughout of the 20th century, Saros 126 continued to 

produce total eclipses. The maximum central duration gradually increased with each event until the peak duration of 2min 

36s was reached on 1972 Jul 10. The duration of the following 

total eclipse on 1990 Jul 22 was 2 min 33 s. This decrease in 

duration was due to the large value of gamma (0.7595) which 

produced a high latitude eclipse track along the northern coast 

of Siberia (Espenak 1989). 

Because the 2008 eclipse has an even larger value of 

gamma (0.8306), its path sweeps over higher latitudes resulting 

in a shorter duration of 2min 27s. With just two more total 

eclipses left in Saros 126 (2026 and 2044), the series becomes 

partial again with the eclipse of 2062 Sep 03. Four more centuries of partial eclipses occur before the series terminates with 

the partial eclipse of 2459 May 03.

In summary, Saros series 126 includes 72 eclipses. It begins with 8 partials, followed by 28 annulars, 3 hybrids, and 

10 totals. It ends with a long string of 23 partial eclipses. From 

start to finish, the series spans a period of 1280 years.

2. Weather Prospects for the Eclipse

2.1 Overview

For most eclipses, weather prospects offer several choices. 

For instance, the previous total eclipse in 2006 had a very 

promising climatology in Saharan Africa, Egypt, and southern 

Turkey. The 2008 eclipse is more limiting in that the weather 

tends to be rather dismal along the majority of the track, even 

though the August 1 date comes at the peak of summer and 

summer sunshine. It is not until the path reaches southern 

Russia and northern China that the prospects for sunshine rise 

to values comparable to the 2006 total eclipse. 

China, near the cities of Hami and Jiuquan, has the best 

prospects (over 70%) while southern Siberia, between Novosibirsk and the Mongolian border, offers about a 60% probability 

of success. Other locations tempt for their stunning scenery 

or travel off the beaten path, but eclipse-seekers in these areas 

will have to compromise with poorer weather prospects. 

2.2 The Canadian Archipelago

On August 1, temperatures in the Canadian Arctic have 

just passed their annual peak. The polar ice pack is retreating 

rapidly under the onslaught of continuous daylight, headed 

for its minimum in mid-September. Over southern and central 

parts of the archipelago, snow cover has melted away from the 

land and at Alert, the world’s most northerly settlement, has 

declined to barely a centimeter in depth. It is not a snow-free 

world however, as all Arctic settlements along the eclipse track 

can experience snowstorms in July and August—storms that 

can drop as much as 20 cm of fresh snow.

Cyclonic weather systems (lows) tend to frequent the 

lower latitudes of the Canadian islands, being more common 

along the north coast of the mainland near Cambridge Bay 

than farther north at Resolute, Grise Fiord, and Alert. The 

impact of these systems on cloudiness is rather muted as skies 

tend to be gray whether or not a cyclonic disturbance is in the 

vicinity. At Cambridge Bay, the frequency of days with heavy 

cloud (8–10 tenths) is 70% and at Resolute, 77%. A significant 

part of this cloudiness comes in the form of fog, which occurs 

across the archipelago with a frequency of between 20 and 

30% in August.

The low-level cloudiness and fog are a consequence of the 

cooling of summer air masses as they pass over the cold Arctic Ocean waters, and suggests that conditions inland record 

greater amounts of sunshine than those at the coast. Satellite 

images for the region, however, usually show that the cloud 

cover simply blots out the landscape according to the weather 

of the day. Nevertheless, there is probably a small reward in 

moving inland a few kilometers in order to maximize the 

climatological probability of sunshine.

From a global perspective, cloud cover decreases southward, and so Cambridge Bay, close to where the eclipse begins, 

should be more inclined to a sunny day than any of the few stations farther north. This is seen quite dramatically in Figure 17, 

which shows the mean cloud cover along the central line as 
Total Solar Eclipse of 2008 August 01

10

measured from polar-orbiting and geostationary satellites. The 

eclipse track near Cambridge Bay has a mean cloudiness of 

slightly below 65% compared to values in the mid–and upper 

70 s for Resolute and Alert. This Cambridge Bay advantage, 

however, has a meager reflection in the observations of cloudiness from the surface (Table 18). 

Hourly records of sunshine—probably the best indication 

of the prospects of seeing the eclipse—show only a small variation across the Canadian Arctic. At Alert and Cambridge Bay, 

the percent of possible sunshine is close to 33%; at Resolute, 

it is only 22% (Table 18). As all of these means are for the 

month of August, it seems sensible to take an average of July 

and August to arrive at a more representative value for eclipse 

day. After making this adjustment, the percent of possible 

sunshine rises to 40, 31, and 36% for Cambridge Bay, Resolute, 

and Alert, respectively. 

The low altitude of the Sun over the Canadian Arctic is 

attractive for those who want to escape the endemic cloudiness by viewing from an airplane. The high frequency of low 

cloud is an advantage here, as the cloud top is more likely to 

be accessible to small aircraft with a limited ceiling. The low 

cloudiness—particularly the frequency of fog—has a downside, however, as Arctic flight schedules are notorious for being 

interrupted, sometimes for days on end, by poor visibilities 

in fog or occasional snowstorms. No seasoned traveler would 

visit the Canadian archipelago without leaving a few days leeway for bad weather on either side of scheduled events. Once 

again, Cambridge Bay has all the advantage here: the August 

climatological record shows a frequency of 9.5 with visibility 

less than 1 km compared to more than 73 at Resolute. 

2.3 Northern Greenland

While cloud cover and weather statistics for northern 

Canada are only just sufficient to make an informed decision 

about a viewing site, those along the portion of the eclipse track 

from the north coast of Greenland to Spitsbergen Island are 

completely inadequate. Only a few expeditions have visited 

the region and satellite images are complicated by observational biases and poor viewing angles. Geostationary satellites 

cannot see much farther north than about 65° latitude, while 

polar-orbiting satellite observations are complicated by snow 

and ice fields that make the automatic identification of cloud 

difficult. 

The Greenland ice cap has a high frequency of sunny 

skies because of an altitude that places it above the moist 

lower layers of the atmosphere. When air flows outward from 

the icy plateau, it is warmed by compression on its downhill 

journey to the ocean, and arrives at sea level with clear skies 

and (frequently) violent winds. An icebreaker offshore might 

be able to tap into one of these katabatic flows, as happened 

for the 2003 eclipse in Antarctica. 

The satellite record represented in Figure 17 suggests that 

average cloud cover increases along the track from 80% near 

Alert, to 95% near Spitsbergen Island, in general agreement 

with other databases that have been compiled by expeditions 

over the years. The cloud cover is not particularly forgiving, as 

it tends to be opaque and relatively devoid of openings. There 

are no permanent surface observing sites in northern Greenland, though some automatic stations do provide temperature 

data from the ice cap.

2.4 Spitsbergen Island to the Russian Coast

The eclipse passes between the islands of Svalbard and 

Franz Josef Land, touching each one of these archipelagos 

only on the shadow’s northern and southern limits, respectively. This region is much cloudier than Canada’s Arctic 

islands, with mean cloud amounts that exceed 90% (Figure 

17). Early explorers commented on the unending grayness of 

the region, which, unlike the more ice-bound regions above 

the 70th parallel, does not even give way to clearer skies in 

the winter months. 

The explanation lies in the presence of an extension of 

the Atlantic Gulf Stream that feeds relatively warm water into 

the Barents Sea through the gap between Iceland and Norway. 

Warm Atlantic airstreams saturate quickly as they flow over 

the cold Arctic waters and the result is an extremely high frequency of low cloud, more than in any other parts of the high 

northern latitudes. The Barents Sea also has a relatively high 

frequency of cyclonic storms in August, though the strength 

of these low-pressure systems is much less than those that 

develop later in the year. 

The graph in Figure 17 shows that the heaviest cloud cover 

of the entire track lies in the region surrounding Spitsbergen 

Island; in the surface station data, observing sites in Franz 

Josef Land have that dubious distinction. Ny Alesund, the only 

station in the area for which sunshine data are available, shows 

an average of 4.3h of sunshine each day, a figure that translates 

into just 18% of the maximum possible. According to satellite 

data (Figure 17), the cloudiness along the central line declines 

steadily after the eclipse track passes 30° E longitude, dropping 

below 75% on the coast of Novaya Zemlya. Cloudiness spikes 

upward briefly as the eclipse path crosses the high terrain of 

Novaya Zemlya, but then continues its downward trend—a 

trend that continues until the Chinese border. Surface observations (Table 18) are not quite so dramatic, showing a more 

muted cloud-cover trend that drops only about 10% between 

Viktoriya Island in Franz Josef Land and Malye Karmakuly 

on Novaya Zemlya. 

Novaya Zemlya and the islands that make up Svalbard 

and Franz Josef Land have prominent terrain that may provide some shielding from the endemic cloud cover of Arctic 

latitudes. Winds that blow downslope from higher ground or 

are diverted to flow around an island may carve holes in the 

cloud cover on the lee side of the terrain. It is a phenomenon 

that is usually very local in extent. The south side of Novaya 

Zemlya, being significantly larger and higher than the other 

islands and angled to block the prevailing northwesterly and 

northerly flows, is most likely to benefit from the lee side drying. It is not a major improvement, but brings mean cloudiness 

down to about 70%—a drop of nearly a fifth from the peak 

near Spitsbergen Island. 

Eclipse expeditions that hope to watch from Arctic wa-
F. Espenak and J. Anderson

11 

ters should head for the Kara Sea between Novaya Zemlya 

and the Yamal Peninsula (on the Russian mainland) in order 

to take advantage of the modest improvement in the cloud 

climatology.

While the Barents and Kara Seas lie in the path of cyclonic 

storms moving eastward from the Atlantic, the lows do not 

carry the punch of storms in the cold-weather season. Wind 

speeds around Novaya Zemlya average just over 15km/h in 

August and seldom reach above 50 km/h. Wind speeds at Viktoriya Island, between Spitsbergen and Franz Josef Islands, are 

slightly stronger on average, but also peak at the 50km/h mark. 

Wave heights reflect these lighter winds, being generally less 

than one meter and only occasionally above two.

Maximum temperatures all along the Arctic track rise 

only 5–10°C above the freezing point, reaching the warmest 

values on the bigger islands. Novaya Zemlya is warmer on 

the west side than on the east, as the west intercepts the Gulf 

Stream branch that reaches out from the Atlantic Ocean. This 

warmer air also carries a heavy moisture load and so the 

cloudiness on the windward side of the island is heavier than 

on the leeward side.

2.5 Siberia

As the path of the lunar shadow moves southward across 

central Russia, it encounters a moist landscape of rivers, 

bogs, and small lakes. The surface provides a ready supply 

of moisture to be incorporated into passing weather systems. 

Most of these weather systems track north of the 60th parallel, 

but their associated frontal systems can sweep much farther 

south, even into China. The weather in the north has a very 

different character than that in the south. Above the 60th 

parallel, large weather systems with extensive mid- and upper-level cloud shields and steady precipitation are a common 

feature of the mid-summer months. Farther south, nearer to 

Novosibirsk, the weather systems become more convective in 

nature, with showers and thundershowers bringing the majority of the rainfall. 

There is not a clear-cut distinction between the northern 

and southern cloud climates, but instead, a gradual transition 

as latitudes decline. In the satellite data, mean cloudiness 

diminishes steadily, from 65% along the north coast near 

Nadym to 47% near Barnaul (Figure 17). South of Barnaul 

cloud cover increases by nearly 10% over the rugged Altay 

Mountains that mark the boundary between Russia and China. 

Surface observations show the percent of possible sunshine 

climbing from 35% at Salekhard, to a more promising 54% at 

Novosibirsk and 57% at Barnaul.

The most likely eclipse destination in northern Siberia is 

Nadym, just below the Arctic Circle. A small community of 

50,000 composed of imposing bastions of apartments, Nadym 

owes its existence to huge reserves of natural gas. As climate 

statistics are not available for Nadym, Tako-Sale or Salekhard 

can be substituted. In either case, cloud cover statistics are not 

encouraging, in large part because of the frequent presence of 

migrating low-pressure systems with their large cloud shields 

and sustained precipitation. In Figure 17, Nadym looks promising only when compared with sites much farther north.

Much of the summer precipitation in the southern portion 

of the Siberian track is in the form of convective showers arising during the passage of weak frontal systems. These frontal 

disturbances pass relatively quickly and are easily followed in 

satellite imagery by noting the areas of mid- and high-level 

cloudiness that usually accompany them. Such systems can 

bring a day or more of cloudiness, in contrast to less organized 

forms of convection that may persist for only an afternoon 

and evening. Whatever its nature, most days with rain are 

supported by some form of upper disturbance and eclipse expeditions should keep an eye on numerical-computer models, 

as these are quite reliable at forecasting the movement of the 

upper systems. 

The Altay Mountains, with peaks rising above 4000m, 

impose a substantial barrier between Russia and China and 

separate two very different climate regimes. Their altitude 

brings a sharp increase in cloudiness as air is forced to rise 

and cool, but the spectacular beauty of the area, with brilliant 

glaciers and snow-capped peaks, provides a powerful temptation to go to the border for the eclipse. The climate in the 

Altay is highly variable, with high, steeply sloped mountains 

alternating with deep valleys. The rugged terrain breaks holes 

in all but the most persistent weather systems, but the difficulty 

of travel and the limited horizon view make the task of finding 

a sunny spot a difficult one. Given the challenges, the most 

promising weather would seem to lie on the south side of the 

Altay, close to the border with Mongolia, where the climate 

is much drier. 

Temperatures moderate significantly once the eclipse track 

leaves the Arctic coast for the interior of Siberia. August 1 is 

just past the warmest part of the year: maximum temperatures 

climb from an average of 13°C in the north to between 21 and 

23°C near Novosibirsk and Barnaul. Rainfall is infrequent in 

the afternoon—on average about 15% of the hours around 

the time of the eclipse have precipitation reported. It is not 

a particularly breezy time of year (maximum winds seldom 

exceed 40 km/h), but strong thunderstorms can bring damaging gusts just as in North America or Europe. The likelihood 

of a thunderstorm during the afternoon ranges from less than 

1% over the northern part of the track to between 3 and 5% 

south of Novosibirsk.

2.6 Local Conditions Around Novosibirsk

Novosibirsk is likely to be the staging point for eclipse 

expeditions to southern Siberia as it is a substantial metropolis 

(the third largest in Russia) with all of the services that come 

with a large population. The surrounding landscape is a mixture of forest and farmland, with good highways to the east, 

west, and south. Of particular interest is the highway that leads 

southward from the city toward Barnaul and the Mongolian 

border: it follows the central line very closely for the first 

300 km and then more loosely for the remaining distance. The 

central line of the eclipse shadow misses Novosibirsk to the 

west, passing directly over its airport near the town of Ob.

Open spaces for eclipse observing are at a bit of a pre-
Total Solar Eclipse of 2008 August 01

12

mium, but can be found with a little searching. The area is 

largely unpolluted, thanks to the vast Siberian wilderness, 

though occasional forest fires have been known to give a pink 

cast to the sky. The Novosibirsk Reservoir (informally, the Ob 

Sea), to the southwest of the city, is a large lake with a long 

dimension of over 100 km and a maximum width of nearly 

20 km. The size of the lake and its cool waters play havoc 

with convective clouds—small and medium-sized buildups 

dissipate rapidly as soon as they cross from land to water, often 

opening substantial holes in the cloud cover when conditions 

are right. Eclipse-viewing sites situated on the lee side (which 

changes with the wind direction) of the lake shore could derive 

a substantial benefit from this effect, especially as the central 

line crosses the lake only 20km from Novosibirsk. The suppression of cumulus cloudiness usually extends a short distance 

inland on the lee shore.

Examination of the hourly cloud-cover statistics for 

Novosibirsk shows a strong increase in broken cloudiness 

during the afternoon hours and a corresponding decrease in 

both scattered and overcast cloud cover. This pattern is almost 

certainly a climatological reflection of the buildup of cumulus 

cloud and suggests that a site on the lake should improve odds 

(i.e., the percent of possible sunshine) by 5% to 10% above 

the statistics for Novosibirsk airport, which lies 24 km to the 

north of the lake. Showery weather typically arrives with a 

southerly component to the wind, and so the north side of the 

lake is slightly more favored than the south.

The center of the eclipse track crosses the town of Leninskoye on the north side of the lake and Sosnovka on the south, 

both of which are easily accessible from Novosibirsk. Sosnovka 

is a tiny community located next to a creek of the same name. 

The terrain is open to the southwest and to the north across 

the lake, providing an excellent view of the oncoming shadow, 

and the surrounding countryside is largely made up of open 

farmland. There is no beach along the shore, but an open space 

next to the waterline affords an place for viewing the eclipse. 

Leninskoye, on the north side of the lake, has the attraction of 

a large beach that permits an excellent view southward. The 

beach, or the high ground that backs the beach, offers more 

space than appears available at Sosnovka. Leninskoye itself 

has limited facilities, but is undergoing rapid development as 

residents from Novosibirsk build dachas (country houses) in 

the community. 

Closer to Novosibirsk, the town of Ob—essentially an 

airport suburb—nearly straddles the central line, but there are 

few open spaces to catch a good view of the horizon and the 

ambiance is overly industrial with noisy traffic on the highway 

leading to Omsk. South of Ob lies a stretch of farmland with 

open pastures mixed with patches of forest. 

2.7 China

As the eclipse track crosses the Altay Mountains into 

China, there is an abrupt change in climatology, in part because 

of the blocking effects of the mountains. Northern China is 

bone-dry and much sunnier. The eclipse track passes between 

the Taklimakan and Gobi Deserts, following the track of the ancient Silk Road to Xi’an, and then settling into the sunset near 

Luohe. While over northern China the track skips along the 

Mongolia-China border, follows the gradually smaller peaks 

of the Altay Mountains, and then crosses onto a rocky plateau 

between mountain ranges as it passes Hami and Jiuquan. Here, 

at these latter stations, the influence of the deserts is felt most 

strongly, and the prospects for sunshine reach their peak. 

Mean cloud amount as measured by satellite (Figure 17) 

drops nearly 20% from the Altay Mountain maximum, to a 

minimum of 28% at a location on the center line to the southeast 

of Hami. Farther south, past Jiuquan, the track begins to feel the 

influence of the monsoon moisture that haunts central China 

in August, and the cloudiness rebounds to 50% at Xi’an. This 

quick variation in the cloud statistics, leaves eclipse watchers 

with an excellent location from which to view the spectacle. 

Surface-station reports mimic the conclusions of the 

satellite data. From Barnaul to Hami, the percent of possible 

sunshine rises by 20% to a maximum of 76% (Table 18). Precipitation for August drops to a very few millimeters (Table 19) 

and average daytime temperatures climb to the upper 20s (°C). 

Even winds are on our side, with peak values averaging only 

25 km/h along the Silk Road, and easing concerns about dust 

storms. For at least a short interval, the weather conditions for 

the eclipse seem almost perfect. 

In spite of its favorable average climatology, northern 

China is not without its weather systems and occasional heavy 

cloudiness in August. Most of the weather systems are small 

upper disturbances that move across the Altay Mountains from 

Kazakhstan or Russia. The dryness of the air over northern 

China usually means that these disturbances are stripped of 

their low-level cloud, but the remaining higher clouds are 

quite capable of masking the Sun and spoiling the eclipse. As 

with similar systems over Russia, high clouds can be readily detected in satellite imagery and predicted by computer 

models.

2.8 Local Conditions Around Hami

The city of Hami lies on the eastern fringes of the Tarim 

Pendi, the great basin that holds the Taklimakan Desert. To 

the east of Hami is a minor branch of the Tien Shan Mountains, the Karlik Shan, with peaks that reach nearly 5000m. 

While maps may barely show the range, from the city, it is a 

not-too-distant spectacle of snow-capped peaks, frequently 

topped with a fringe of convective cloud. The central line is 

some distance from Hami, on the far side of the Karlik peaks, 

on a pleasant grassland plateau at an altitude nearly 2000m 

above sea level. 

The road from Hami to the mountains is a ruler-straight 

highway that heads northeast from the city. The south limit of 

the eclipse is on the outskirts of Hami; the foot of the mountain 

range is 35 km distant. The mountains begin abruptly, first with 

a gentle climb into a gorge, and then with gradually increasing 

slopes and quick switch-back curves, but the paved highway 

is in excellent condition and after an hour or so of travel, 

emerges from the gorge to show a spectacular plateau—the 

Barkol grassland. As the highway turns southward toward 
F. Espenak and J. Anderson

13 

Yiwu, the largest community near the central line, the peaks 

of the Karlik guard the right-hand side. To the left is a line of 

lower hills, converging slowly toward the highway. The leftside eastern hills are mostly cloud free—the small amount of 

cumulus present will dissipate during the eclipse. The higher 

Karlik peaks in the west, however, are topped with towering 

convective clouds, some raining on the steep slopes above the 

grassland plateau. The winds of the day push the remnants of 

these mountain showers toward the highway, but the downslope 

run from the peaks causes them to dissipate on their journey 

and the day is scarcely interrupted by the leftover patches that 

finally reach the highway.

At Yiwu, a modern city of brightly colored apartments, 

the eastern hills finally pinch off the highway. The town is 

nestled against these dull-brown hills, and as the road turns 

from southeast to northeast toward the central line, it enters a 

winding gorge, at one moment open to a wide expanse of sky, 

and the next, confined between narrow hills and roadside trees. 

The central line is in the gorge: the sky is open to a good view 

of the eclipse, but the horizons are blocked in all directions and 

the space is very limited for a group of any size. Beyond the 

central line, several kilometers distant, the gorge opens onto 

a flat gravely plain allowing a view of the whole sky. 

The surface-station climatology at Hami (Table 18) is not 

representative of the conditions along the central line, as the 

mountain cloudiness is barely reflected in the observations 

from the city. The scattered-to-broken cloudiness encountered 

on the plateau is probably fairly common all along the eclipse 

track, at least wherever the track lies in the proximity of higher 

ground. Observations farther north near Urumqi seem to 

support this conclusion; however, the satellite-derived cloud 

statistics reflect the mountain cloud cover more accurately. 

While the statistics for Hami are more optimistic than is actually the case on the eclipse track, there seems little reason to 

dispute the satellite measurements that give a strong nod to the 

Hami-Jiuquan area. Perhaps the best location is northeast of 

Anxi, near the community of Gongpoquan where the terrain 

is lowest and the mountain-induced cloudiness at a minimum, 

but local information suggests that this is a military area with 

restricted access. 

Cloud conditions on the eclipse track cannot be easily 

viewed from Hami, though the cloud on the Karlik range is 

readily visible from the city. Only a trip to the plateau will permit the eclipse traveler to judge the conditions on eclipse day, 

but the cloud is so highly variable, unless a major disturbance 

is in the area, that it seems unlikely that the eclipse would 

not be visible somewhere on the Barkol grassland. The extent 

and direction of motion of the mountain cloud will depend on 

the weather on eclipse day and must be assessed at that time.

2.9 Local Conditions Near Xi’an

Xi’an lies on the edge of the eclipse path, in a region with 

a discomforting humidity, poorer prospects for cloudiness, and 

a disconcerting level of pollution and haze. The eclipse here 

will be very low—barely 4° above the horizon. Based on recent 

experience, the eclipse will not be visible from the city, as the 

Sun disappears into the smog while at a considerable altitude, 

perhaps as much as 10°. Outside the city, on the central line 

to the north, skies will be cleaner, but the view will still be 

severely limited by haze and humidity.

2.10 Getting Weather Information

The two main sources of weather information for shortrange planning (a few days to hours) are satellite imagery and 

numerical models of the atmosphere. Both of these can be 

found for nearly all parts of the eclipse track and links to a 

selection of distribution sites are given in the following subsections. The high latitude of much of the eclipse track limits 

the utility of geostationary images over Russian and Canada 

as the scene is wrapped over the curve of the Earth. Over the 

first half of the shadow track, downward-looking polar-orbiting satellites must be utilized to see the cloud patterns. Such 

satellites cannot provide the same frequency of coverage as 

their geostationary cousins and wide areas can only be shown 

by assembling strips of images side-by-side over a period of 

several hours, reducing the timeliness of the information.

Model data is even more limited over Russian and China 

even though most national meteorological centers configure 

their numerical models to run across the entire globe. Fortunately, a few sites do provide access to global output to help 

with the medium-range planning leading up to eclipse day. It 

is important to remember that numerical models have serious 

deficiencies, especially in data-sparse regions and the predictions should be backed up by a careful assessment of the real 

weather situation.

2.10.1 Sources of Satellite Imagery

1. https://afweather.afwa.af.mil/weather/satellite.html—A 

United States Air Force (USAF) weather site with satellite 

imagery over several sectors of the globe. High-latitude 

sectors include much of the eclipse track from Greenland 

to China. Images at higher latitudes are composites of 

several polar-orbiter passes and may be a few hours old. 

The sector labeled “IGM” covers most of China and is 

rectified to remove the effects of the Earth’s curvature. A 

low-resolution global sector shows the entire eclipse track 

over mainland Russian and China. A “North Atlantic” 

sector covers the track from the Canadian archipelago 

to Svalbard; the “Northern Europe” sector continues the 

coverage past Novaya Zemlya to China. Both still and 

animated imagery is available.

2. http://met.no/satellitt/index.html —Norwegian Meteorological Institute site with high-latitude imagery that extends to 

Svalberg (in Norwegian).

3. http://www.btinternet.com/~wokingham.weather/wwp2.

html—Wokingham Weather, a private site with high-resolution polar-orbiter imagery that occasionally extends beyond 

Novaya Zemlya.

4. http://www.sat.dundee.ac.uk/—Dundee University Satellite 

Receiving Station. One of the most comprehensive sites, 

Dundee has images from geostationary satellites around 

the globe at high resolution. Both Indian and Chinese 
Total Solar Eclipse of 2008 August 01

14

satellites provide an equatorial view of the eclipse track 

over China (and parts of Russia, with a stretch). Images are 

not rectified and have only minimal country outlines and 

latitude markings, so that finding a particular site requires 

considerable care. Registration (free) is required.

5. http://sputnik.infospace.ru/noaa/engl/noaa.htm—High-resolution polar-orbiter imagery of the Barents Sea. Look under 

“Sea Surface Temperature” and click on “Barents Sea.” The 

ensuing page will contain several satellite images over the 

region from Svalbard to Novaya Zemlya.

6. http://meteo.infospace.ru/main.htm—Russia’s “Weather 

Server.” Includes low-resolution composite satellite images 

of various sections of Russia under “Satellite Data.” 

2.10.2 Forecast Models

1. http://www.westwind.ch/—An omnibus site containing European model data from dozens of meteorological centers 

and many models. While most of the model output are 

for more southerly latitudes than the eclipse track, some 

provide cloud cover predictions for high latitudes. Try the 

University of Athens site “SKIRON” where three-day 

numerical forecasts extend north to Svalbard and Novaya 

Zemlya.

2. http://weatheroffice.ec.gc.ca/charts/index_e.html—Environment Canada’s site where numerical model forecasts for the 

Canadian Arctic islands are available. Use the “Regional” 

model for short-range (48 hours) detailed forecasts and 

the “Global” model for long-range (5-day) predictions. For 

more detail in cloud layers, look under “Vertical Motion.” 

The Global model extends across the pole to include areas 

as far as Novaya Zemlya.

3. http://ddb.kishou.go.jp/grads.html—A Japanese site with an 

interactive map server that allows you to pick out a region 

of interest anywhere in the world and display computer 

forecast fields for the area. The number of fields is limited, but “dew point depression” at several levels in the 

atmosphere (850, 700, 500mb) will give an indication of 

where the model is predicting high levels of atmospheric 

moisture.

4. http://weather.uwyo.edu/models/—A University of Wyoming 

site that allows you to select from several locations around 

the globe and obtain model data for that area. In particular, 

model output is available for China, the polar seas, and 

a large part of western Russia. While cloud cover is not 

one of the selectable elements, users can map the relative 

humidity at several atmospheric levels. Forecasts out to 

180 hours are available.

2.11 Summary

The weather options for the 2008 eclipse are limited: the 

best prospects are in southern Russia or northern China. By 

selecting a site along the shores of the Novosibirsk Reservoir 

or in the Altay Mountains near the Mongolian border, the 

climatological probability of seeing the eclipse may reach as 

high as 60% in Russia. In China, where a rugged terrain brings 

more cloudiness than suggested by the climate observing sites, 

the probability is likely in the 70% range. Elsewhere, eclipse 

chasers will have to trade grand Arctic and Siberian adventures 

and spectacular scenery for poorer weather prospects.

3. Observing the Eclipse

3.1 Eye Safety and Solar Eclipses

A total 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 the Earth ranges from ultraviolet (UV) 

radiation at wavelengths longer than 290nm, to radio waves in 

the meter range. The tissues in the eye transmit a substantial 

part of the radiation between 380–400nm 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 
F. Espenak and J. Anderson

15 

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 [unitless] 

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 transmittance of 1%, etc.). Figure 18 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 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 quite expensive 

in large sizes.

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. The metallic silver contained in the film emulsion is the protective filter; however, any 

black-and-white negative with images in it is not suitable for 
Total Solar Eclipse of 2008 August 01

16

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 the 

CD can be seen through in normal room lighting, 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 23). 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 

to react when other health-related advice about drugs, AIDS3, 

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. 3.1 was contributed by:

B. Ralph Chou, MSc, OD

Associate Professor, School of Optometry

University of Waterloo

Waterloo, Ontario, Canada N2L 3G1

3.2 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.

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.

Perceptor Telescopes TransCanada, Brownsville Junction 

Plaza, Box 38, Schomberg, Ontario, Canada L0G 1T0, 

(905) 939-2313.

Sources in Europe:

. Acquired Immunodeficiency Syndrome
F. Espenak and J. Anderson

17 

Baader Planetarium GmbH, Zur Sternwarte, 82291 Mammendorf, Germany, 0049 (8145) 8802.

3.3 Eclipse Photography

The eclipse may be safely photographed provided that 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 interchangable 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 19). 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 19). Another issue 

to consider is the lag time between digital frames required to 

write images to the DSLR’s memory 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 partial phases of the 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 totality, 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 19 

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 20).

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. 3.2, “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 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 1/1000 s to 1/4 s. 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 

the 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 (i.e., 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 International Organization for Standardizaion (ISO) speeds, apertures 

(f/number) and solar features (chromosphere, prominences, 

inner, middle, and outer corona) are summarized in Table 21. 

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 21. Keep in 

mind that these exposures are based on a clear sky and a corona 
Total Solar Eclipse of 2008 August 01

18

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 the camera 

on a wall or fence since slow shutter speeds will be needed. 

You should also disable or turn off your camera’s electronic 

flash so that it does not interfere with anyone else’s view of 

the eclipse.

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 on eclipse photography, observations, and eye 

safety, see the “Further Reading” sections in the Bibliography.

3.4 Sky at Totality

The total phase of an eclipse is accompanied by the onset of a rapidly darkening sky whose appearance resembles 

evening twilight about half an hour after sunset. The effect 

presents an excellent opportunity to view planets and bright 

stars in the daytime sky. Aside from the sheer novelty of it, such 

observations are useful in gauging the apparent sky brightness 

and transparency during totality. 

During the total solar eclipse of 2008, the Sun will be in 

Cancer. Four naked-eye planets and a number of bright stars 

will be above the horizon within the total eclipse path. Figure 

20 depicts the appearance of the sky during totality as seen 

from the central line at 11:00 UT. This corresponds to northern 

China near Altay.

All four planets lie east of the Sun in a string spanning 

39°. The most conspicuous of the planets will be Venus (mv= 

–3.8) located 15° from the Sun in Leo. Mercury (mv= –1.7) 

should also be easy to spot just 3° east of the Sun. Saturn is 

considerably fainter (mv= +1.1) and lies 28° from the Sun. Mars 

(mv= +1.7) is most distant from the Sun at 39°. It will also be the 

most challenging planet to find because it is over 5 magnitudes 

(~100×) fainter than Venus. 

The bright star Regulus (mv= +1.36) lies about half way 

between Venus and Saturn. A number of other bright stars will 

be scattered around the sky and may become visible during 

the eerie twilight of totality. They include Castor (mv= +1.94), 

Pollux (mv= +1.14), and Capella (mv= +0.08) to the northwest, 

Vega (mv=+0.03) to the east and Arcturus (mv=–0.05) high in 

the south. Star visibility requires a very dark and cloud free 

sky during the total phase.

At the bottom of Figure 20, a geocentric ephemeris (using 

Bretagnon and Simon 1986) gives the apparent positions of the 

naked eye planets during the eclipse. Delta is the distance of 

the planet from Earth (in Astronomical Units), App. Mag. is the 

apparent visual magnitude of the planet, and Solar Elong gives 

the elongation or angle between the Sun and planet.

For a map of the sky during totality from Canada, see 

NASA’s Web site for the 2008 total solar eclipse: http://sunearth.gsfc.nasa.gov/eclipse/SEmono/TSE2008/TSE2008.

html.

3.5 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 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-inch 

(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, www.

pfdsystems.com in order to link specific Baily’s bead events 

with lunar features.

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 arc-sec (~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 hand-held 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 
F. Espenak and J. Anderson

19 

accuracy requirement above. Some of these maps are available on Web sites such as www.topozone.com. 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, which provides 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 www.eclipsetours.com. For specific details 

on equipment and observing methods for observing at the 

eclipse path limits, refer to 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: david.dunham@jhuapl.edu

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.

3.6 Plotting the Path on Maps

To assist hand-plotting of high-resolution maps of the umbral path, the coordinates listed in Tables 7 and 8 are provided 

in longitude increments of 1°. The coordinates in Table 3 define 

a line of maximum eclipse at 3min increments. If observations are to be made near the limits, then the grazing eclipse 

zones tabulated in Table 8 should be used. A higher resolution table of graze zone coordinates at longitude increments 

of 7.5 ́ is available via the NASA 2008 total solar eclipse Web 

site: http://sunearth.gsfc.nasa.gov/eclipse/SEmono/TSE2008/

TSE2008.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 many maps available for immediate 

delivery.

4. ECLIPSE RESOURCES

4.1 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: http://www.totalsolareclipse.net, 

 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), and Michael Gill 

(UK). Yihua Yan (China), yyh@bao.ac.cn, is the director of the 

section of solar physics of the Beijing National Astronomical 

Observatory and has been added to the Working Group for the 

2008 and 2009 eclipses; he is in charge of the organization of 

the eclipse efforts in China.

4.2 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. 4.1). Information on safe solar 

filters can be obtained by contacting Program Group member 

Dr. B. Ralph Chou (bchou@sciborg.uwaterloo.ca).

4.3 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. 
Total Solar Eclipse of 2008 August 01

20

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). He maintains archives of past 

SEML messages through July 2004 on his Web site: http://

uk.geocities.com/solareclipsewebpages@btopenworld.com/

and http://www.mreclipse.com/SENL/SENLinde.htm.

4.4 The 2007 International Solar Eclipse 

Conference

An international conference on solar eclipses is being 

planned for 2007. The main objective of the gathering is to 

bring together professional eclipse researchers and amateur 

enthusiasts in a forum for the exchange of ideas, information, 

and plans for past and future eclipses. Previous conferences 

were held in Antwerp, Belgium (2000) and Milton Keynes, 

England (2004), the last of which had 115 delegates from 20 

different countries. 

The conferences are planned for years when no central 

eclipses occur, to avoid travel conflicts. The 2007 event is 

scheduled for August 24–26 at Griffith Observatory, Los Angeles, CA. The Web site for the conference (including registration 

information and speaker list) is: http://uk.geocities.com/solareclipsewebpages@btopenworld.com/SEC2007.html.

For more about the conference, contact the organizers 

(Joanne and Patrick Poitevin) at: solareclipsewebpages@

btopenworld.com.

4.5 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. This was made possible through the 

efforts and expertise of Dr. Joe Gurman (GSFC/Solar Physics 

Branch). 

NASA eclipse bulletins can be read, or downloaded via 

the Internet, using a Web browser (such as Netscape, Microsoft 

Explorer, etc.) from the GSFC Solar Data Analysis Center 

(SDAC) Eclipse Information home page, or from top-level 

Web addresses (URLs) for the currently available eclipse 

bulletins themselves:

Annular Solar Eclipse of 1994 May 10

— http://umbra.nascom.nasa.gov/eclipse/940510/rp.html

Total Solar Eclipse of 1994 Nov 03

— http://umbra.nascom.nasa.gov/eclipse/941103/rp.html

Total Solar Eclipse of 1995 Oct 24

— http://umbra.nascom.nasa.gov/eclipse/951024/rp.html

Total Solar Eclipse of 1997 Mar 09

— http://umbra.nascom.nasa.gov/eclipse/970309/rp.html

Total Solar Eclipse of 1998 Feb 26

— http://umbra.nascom.nasa.gov/eclipse/980226/rp.html

Total Solar Eclipse of 1999 Aug 11

— http://umbra.nascom.nasa.gov/eclipse/990811/rp.html

Total Solar Eclipse of 2001 Jun 21

— http://umbra.nascom.nasa.gov/eclipse/010621/rp.html

Total Solar Eclipse of 2002 Dec 04

— http://umbra.nascom.nasa.gov/eclipse/021204/rp.html

Solar Eclipses of 2003: May 31 & Nov 23 

— http://umbra.nascom.nasa.gov/eclipse/2003/rp.html

Total Solar Eclipse of 2006 Mar 29 

— http://umbra.nascom.nasa.gov/eclipse/060329/rp.html

Total Solar Eclipse of 2008 Aug 01 

— http://umbra.nascom.nasa.gov/eclipse/080801/rp.html

Recent bulletins are available in both “html” and “pdf” 

formats. All future NASA eclipse bulletins will be available 

over the Internet, at or before publication of each. The primary 

goal is to make the bulletins available to as large an audience 

as possible, thus, some figures or maps may not be at their 

optimum resolution or format. Comments and suggestions 

are actively solicited to fix problems and improve on compatibility and formats.

4.6 Future Eclipse Paths on the Internet

Presently, the NASA eclipse bulletins are published 18 

to 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 the demand, predictions 

have been generated for all central solar eclipses from 1991 

through 2030. All predictions are based on j=2 ephemerides for 

the Sun (Newcomb 1895) and Moon (Brown 1919, and Eckert 

et al. 1954). The value used for the Moon’s secular acceleration 

is n ̇=–26arcsec/cy2 as deduced by Morrison and Ward (1975). 

The path coordinates are calculated with respect to the Moon’s 

center of mass (no corrections for the Moon’s center of figure). 

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.

The umbral path characteristics have been predicted with 

a 1min 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. Global maps using an 

orthographic projection also present the regions of partial and 

total (or annular) eclipse. The index Web page for the path 

tables and maps is: http://sunearth.gsfc.nasa.gov/eclipse/SEpath/SEpath.html.

4.7 NASA Web Site for 2008 Total Solar Eclipse

A special Web site has been set up to supplement this bulletin with additional predictions, tables, and data for the total 

solar eclipse of 2008. Some of the data posted there include an 

expanded version of Tables 7 and 8 (Mapping Coordinates for 

the Zones of Grazing Eclipse), and local circumstance tables 

with additional cities, as well as for astronomical observatories. Also featured will be higher resolution maps of selected 

sections of the path of totality and limb profile figures for 

other locations/times along the path. The URL of the special 

TSE2008 Web site is: http://sunearth.gsfc.nasa.gov/eclipse/

SEmono/TSE2008/TSE2008.html.
F. Espenak and J. Anderson

21 

4.8 Predictions for Eclipse Experiments

This publication provides comprehensive information on 

the 2008 total solar eclipse 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 2008 eclipse, as well as 

for previous eclipses in which analysis is still in progress. To 

discuss individual needs and requirements, please contact Fred 

Espenak (espenak@gsfc.nasa.gov).

4.9 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 2006 to 2008, a value 

for ∆T of 65.3s was 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 iMac G4 800 MHz computer. All 

calculations, diagrams, and opinions presented in this publication are those of the authors and they assume full responsibility 

for their accuracy.

F. Espenak and J. Anderson

23 

 TABLES
Total Solar Eclipse of 2008 August 01

24

TABLE 1

ELEMENTS OF THE TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

Equatorial Conjunction: 09:48:26.72 TDT J.D. = 2454679.908643

(Sun & Moon in R.A.) (=09:47:21.40 UT)

Ecliptic Conjunction: 10:13:38.78 TDT J.D. = 2454679.926143

(Sun & Moon in Long.) (=10:12:33.46 UT)

Instant of 10:22:12.15 TDT J.D. = 2454679.932085

Greatest Eclipse: (=10:21:06.82 UT)

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

Sun: R.A. = 08h47m54.149s Moon: R.A. = 08h49m08.757s

Dec. =+17°51'56.39" Dec. =+18°38'01.54"

Semi-Diameter = 15'45.50" Semi-Diameter = 16'14.12"

Eq.Hor.Par. = 08.66" Eq.Hor.Par. = 0°59'34.82"

∆ R.A. = 9.694s/h ∆ R.A. = 142.347s/h

∆ Dec. = -38.19"/h ∆ Dec. = -762.64"/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 = 4.2° Brown Lun. No. = 1059

(Optical + Physical) b = -1.0° Saros Series = 126 (47/72)

c = 14.0° nDot = -26.00 "/cy**2

Eclipse Magnitude = 1.03942 Gamma = 0.83071 ∆T = 65.3 s

Polynomial Besselian Elements for: 2008 Aug 01 10:00:00.0 TDT (=t0)

n x y d l1 l2 μ

0 0.1017945 0.8506194 17.8675385 0.5382522 -0.0078656 328.422546

1 0.5285779 -0.2025230 -0.0101205 0.0001111 0.0001105 15.002012

2 -0.0000634 -0.0001512 -0.0000038 -0.0000120 -0.0000120 0.000002

3 -0.0000081 0.0000033 0.0000000 0.0000000 0.0000000 0.000000

Tan ƒ1 = 0.0046066 Tan ƒ2 = 0.0045836

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 = 10.000 TDT

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

calculated at five uniformly spaced times over a six hour period centered at

t0. Thus the Besselian elements are valid over the period 7.00 ≤ t1 ≤ 13.00

TDT.

Note that all times are expressed in Terrestrial Dynamical Time (TDT).

Saros Series 126: Member 47 of 72 eclipses in series.
F. Espenak and J. Anderson

25 

TABLE 2

SHADOW CONTACTS AND CIRCUMSTANCES

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

∆T = 65.3 s

= 000°16'22.6"

Terrestrial

Dynamical Ephemeris True

Time Latitude Longitude† Longitude*

h m s

External/Internal

Contacts of Penumbra: P1 08:05:11.4 50°12.6'N 052°30.9'W 052°14.5'W

P4 12:39:31.4 11°10.0'N 085°20.0'E 085°36.4'E

Extreme

North/South Limits

of Penumbral Path: N1 08:33:37.6 36°15.9'N 050°31.1'W 050°14.7'W

S1 12:10:58.3 03°34.5'S 087°40.7'E 087°57.0'E

External/Internal

Contacts of Umbra: U1 09:22:12.5 67°53.9'N 101°32.7'W 101°16.4'W

U2 09:25:15.5 68°39.8'N 105°22.9'W 105°06.5'W

U3 11:19:32.9 34°07.4'N 114°17.7'E 114°34.1'E

U4 11:22:31.0 32°52.7'N 112°57.7'E 113°14.1'E

Extreme

North/South Limits

of Umbral Path: N1 09:25:04.0 68°44.1'N 105°38.4'W 105°22.1'W

S1 09:22:24.7 67°49.1'N 101°17.9'W 101°01.5'W

N2 11:19:44.2 34°14.7'N 114°18.4'E 114°34.8'E

S2 11:22:19.1 32°45.1'N 112°57.2'E 113°13.5'E

Extreme Limits

of Central Line: C1 09:23:43.2 68°16.9'N 103°24.5'W 103°08.1'W

C2 11:21:02.8 33°29.4'N 113°37.1'E 113°53.5'E

Instant of

Greatest Eclipse: G0 10:22:12.1 65°39.2'N 072°01.7'E 072°18.0'E

Circumstances at

Greatest Eclipse: Sun’s Altitude = 33.5° Path Width = 236.9 km

Sun’s Azimuth = 235.2° Central Duration = 02m27.1s

_____________________________________________________________________________

† 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-2007 measurements. The actual value is expected

to fall within ±0.2 seconds of the estimated ∆T used here.
Total Solar Eclipse of 2008 August 01

26

TABLE 3

PATH OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

Universal Northern Limit Southern Limit Central Line Sun Path Central

Time Latitude Longitude Latitude Longitude Latitude Longitude Alt Width Durat.

° km

Limits 68°44.1'N 105°22.1'W 67°49.1'N 101°01.5'W 68°16.9'N 103°08.2'W 0 206 01m29.9s

09:24 69°20.0'N 104°20.4'W 75°41.1'N 082°13.1'W 73°56.9'N 091°31.6'W 7 213 01m40.5s

09:27 77°08.3'N 087°54.5'W 78°56.4'N 068°52.0'W 78°17.2'N 078°27.6'W 12 217 01m49.3s

09:30 80°32.0'N 075°34.7'W 81°02.4'N 053°57.7'W 80°58.4'N 064°37.5'W 16 219 01m55.3s

09:33 82°51.7'N 060°03.5'W 82°18.0'N 036°32.8'W 82°44.3'N 047°29.0'W 18 221 02m00.1s

09:36 84°18.5'N 038°58.1'W 82°47.2'N 017°38.7'W 83°38.8'N 026°44.8'W 21 222 02m04.2s

09:39 84°47.0'N 013°29.5'W 82°35.6'N 000°11.9'E 83°42.9'N 005°16.0'W 22 223 02m07.8s

09:42 84°20.7'N 009°52.7'E 81°53.8'N 014°59.8'E 83°06.6'N 012°59.5'E 24 224 02m10.9s

09:45 83°19.1'N 026°54.4'E 80°53.4'N 026°26.3'E 82°05.2'N 026°41.0'E 26 224 02m13.6s

09:48 82°00.4'N 038°27.5'E 79°42.3'N 035°08.7'E 80°50.6'N 036°36.7'E 27 225 02m16.0s

09:51 80°34.5'N 046°28.6'E 78°25.7'N 041°51.3'E 79°29.8'N 043°56.1'E 28 226 02m18.2s

09:54 79°06.1'N 052°19.1'E 77°06.3'N 047°09.1'E 78°06.2'N 049°31.0'E 29 227 02m20.1s

09:57 77°37.3'N 056°46.7'E 75°45.7'N 051°26.3'E 76°41.6'N 053°55.0'E 30 228 02m21.7s

10:00 76°08.8'N 060°19.7'E 74°24.7'N 054°59.7'E 75°17.1'N 057°29.8'E 31 229 02m23.1s

10:03 74°41.2'N 063°15.1'E 73°03.9'N 058°00.6'E 73°52.9'N 060°29.4'E 32 230 02m24.3s

10:06 73°14.7'N 065°43.6'E 71°43.4'N 060°36.9'E 72°29.5'N 063°03.1'E 32 231 02m25.3s

10:09 71°49.1'N 067°52.5'E 70°23.4'N 062°54.5'E 71°06.7'N 065°17.3'E 33 232 02m26.0s

10:12 70°24.5'N 069°46.5'E 69°03.8'N 064°57.4'E 69°44.7'N 067°16.6'E 33 233 02m26.6s

10:15 69°00.7'N 071°29.3'E 67°44.8'N 066°48.7'E 68°23.3'N 069°04.3'E 33 234 02m27.0s

10:18 67°37.7'N 073°03.5'E 66°26.2'N 068°30.9'E 67°02.5'N 070°43.0'E 33 236 02m27.1s

10:21 66°15.4'N 074°30.9'E 65°08.0'N 070°05.8'E 65°42.3'N 072°14.7'E 34 237 02m27.1s

10:24 64°53.5'N 075°53.2'E 63°50.1'N 071°34.9'E 64°22.4'N 073°40.7'E 33 238 02m26.9s

10:27 63°32.1'N 077°11.5'E 62°32.4'N 072°59.4'E 63°02.8'N 075°02.5'E 33 240 02m26.5s

10:30 62°10.9'N 078°27.0'E 61°14.8'N 074°20.5'E 61°43.5'N 076°21.0'E 33 241 02m25.9s

10:33 60°49.8'N 079°40.5'E 59°57.2'N 075°38.9'E 60°24.1'N 077°37.2'E 33 243 02m25.2s

10:36 59°28.7'N 080°52.8'E 58°39.5'N 076°55.6'E 59°04.7'N 078°51.9'E 32 244 02m24.2s

10:39 58°07.3'N 082°04.7'E 57°21.5'N 078°11.2'E 57°45.1'N 080°05.8'E 32 245 02m23.0s

10:42 56°45.6'N 083°16.9'E 56°03.2'N 079°26.5'E 56°25.1'N 081°19.7'E 31 247 02m21.7s

10:45 55°23.3'N 084°30.2'E 54°44.3'N 080°42.2'E 55°04.5'N 082°34.3'E 30 248 02m20.1s

10:48 54°00.2'N 085°45.3'E 53°24.7'N 081°59.0'E 53°43.1'N 083°50.3'E 29 249 02m18.3s

10:51 52°35.9'N 087°03.1'E 52°04.1'N 083°17.8'E 52°20.8'N 085°08.6'E 28 250 02m16.3s

10:54 51°10.3'N 088°24.8'E 50°42.2'N 084°39.4'E 50°57.1'N 086°30.2'E 27 251 02m14.1s

10:57 49°42.7'N 089°51.4'E 49°18.8'N 086°04.9'E 49°31.6'N 087°56.3'E 26 252 02m11.6s

11:00 48°12.8'N 091°24.8'E 47°53.4'N 087°35.7'E 48°04.0'N 089°28.2'E 25 252 02m08.8s

11:03 46°39.6'N 093°07.3'E 46°25.3'N 089°13.4'E 46°33.5'N 091°08.1'E 23 251 02m05.7s

11:06 45°02.0'N 095°02.1'E 44°53.9'N 091°00.7'E 44°59.2'N 092°58.8'E 21 250 02m02.2s

11:09 43°18.1'N 097°14.9'E 43°17.9'N 093°01.0'E 43°19.5'N 095°04.7'E 19 247 01m58.2s

11:12 41°24.4'N 099°55.9'E 41°35.2'N 095°20.5'E 41°31.9'N 097°33.5'E 16 243 01m53.6s

11:15 39°12.5'N 103°29.5'E 39°42.1'N 098°10.7'E 39°30.8'N 100°41.5'E 13 236 01m47.9s

11:18 36°03.7'N 109°50.0'E 37°28.8'N 101°59.9'E 36°59.6'N 105°18.3'E 8 224 01m40.2s

Limits 34°14.7'N 114°34.8'E 32°45.1'N 113°13.5'E 33°29.4'N 113°53.5'E 0 200 01m27.9s
F. Espenak and J. Anderson

27 

TABLE 4

PHYSICAL EPHEMERIS OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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

09:22.6 68°16.9'N 103°08.2'W 1.0299 1.0607 0.0 34.0 205.7 - 101.1 - 01m29.9s

09:24 73°56.9'N 091°31.6'W 1.0320 1.0650 6.8 45.3 213.4 924.4 108.0 4.654 01m40.5s

09:27 78°17.2'N 078°27.6'W 1.0336 1.0684 12.1 59.0 217.4 545.6 113.3 2.600 01m49.3s

09:30 80°58.4'N 064°37.5'W 1.0346 1.0705 15.5 73.7 219.4 437.6 116.6 2.017 01m55.3s

09:33 82°44.3'N 047°29.0'W 1.0354 1.0721 18.3 91.8 220.8 381.9 119.2 1.717 02m00.1s

09:36 83°38.8'N 026°44.8'W 1.0361 1.0735 20.5 113.7 221.8 347.0 121.3 1.528 02m04.2s

09:39 83°42.9'N 005°16.0'W 1.0366 1.0746 22.5 136.3 222.7 322.7 123.1 1.397 02m07.8s

09:42 83°06.6'N 012°59.5'E 1.0371 1.0756 24.2 155.9 223.5 304.8 124.7 1.299 02m10.9s

09:45 82°05.2'N 026°41.0'E 1.0375 1.0765 25.7 170.9 224.3 291.0 126.0 1.223 02m13.6s

09:48 80°50.6'N 036°36.7'E 1.0379 1.0772 27.0 182.2 225.1 280.2 127.1 1.163 02m16.0s

09:51 79°29.8'N 043°56.1'E 1.0382 1.0778 28.2 190.9 225.9 271.4 128.1 1.114 02m18.2s

09:54 78°06.2'N 049°31.0'E 1.0385 1.0784 29.2 198.0 226.8 264.3 129.0 1.073 02m20.1s

09:57 76°41.6'N 053°55.0'E 1.0387 1.0789 30.2 203.9 227.7 258.5 129.7 1.039 02m21.7s

10:00 75°17.1'N 057°29.8'E 1.0389 1.0793 30.9 209.0 228.7 253.7 130.4 1.010 02m23.1s

10:03 73°52.9'N 060°29.4'E 1.0390 1.0796 31.6 213.6 229.7 249.8 130.9 0.986 02m24.3s

10:06 72°29.5'N 063°03.1'E 1.0392 1.0799 32.2 217.7 230.7 246.6 131.3 0.966 02m25.3s

10:09 71°06.7'N 065°17.3'E 1.0393 1.0801 32.7 221.6 231.9 244.1 131.6 0.949 02m26.0s

10:12 69°44.7'N 067°16.6'E 1.0394 1.0803 33.0 225.2 233.0 242.1 131.9 0.935 02m26.6s

10:15 68°23.3'N 069°04.3'E 1.0394 1.0804 33.3 228.6 234.3 240.7 132.0 0.923 02m27.0s

10:18 67°02.5'N 070°43.0'E 1.0394 1.0804 33.4 231.9 235.5 239.8 132.1 0.914 02m27.1s

10:21 65°42.3'N 072°14.7'E 1.0394 1.0804 33.5 235.1 236.9 239.4 132.1 0.908 02m27.1s

10:24 64°22.4'N 073°40.7'E 1.0394 1.0803 33.5 238.1 238.2 239.5 132.0 0.903 02m26.9s

10:27 63°02.8'N 075°02.5'E 1.0393 1.0802 33.3 241.1 239.6 240.1 131.8 0.901 02m26.5s

10:30 61°43.5'N 076°21.0'E 1.0392 1.0800 33.1 244.0 241.1 241.1 131.5 0.902 02m25.9s

10:33 60°24.1'N 077°37.2'E 1.0391 1.0798 32.8 246.8 242.5 242.7 131.2 0.904 02m25.2s

10:36 59°04.7'N 078°51.9'E 1.0390 1.0795 32.3 249.5 244.0 244.8 130.8 0.910 02m24.2s

10:39 57°45.1'N 080°05.8'E 1.0388 1.0792 31.8 252.2 245.4 247.6 130.2 0.918 02m23.0s

10:42 56°25.1'N 081°19.7'E 1.0386 1.0788 31.1 254.8 246.8 251.0 129.6 0.930 02m21.7s

10:45 55°04.5'N 082°34.3'E 1.0384 1.0783 30.3 257.4 248.1 255.3 128.9 0.946 02m20.1s

10:48 53°43.1'N 083°50.3'E 1.0382 1.0778 29.5 260.0 249.3 260.6 128.0 0.967 02m18.3s

10:51 52°20.8'N 085°08.6'E 1.0379 1.0771 28.4 262.5 250.3 267.1 127.0 0.994 02m16.3s

10:54 50°57.1'N 086°30.2'E 1.0375 1.0764 27.3 264.9 251.1 275.0 125.9 1.029 02m14.1s

10:57 49°31.6'N 087°56.3'E 1.0371 1.0756 26.0 267.4 251.6 284.9 124.7 1.074 02m11.6s

11:00 48°04.0'N 089°28.2'E 1.0367 1.0747 24.5 269.8 251.6 297.5 123.3 1.132 02m08.8s

11:03 46°33.5'N 091°08.1'E 1.0362 1.0737 22.9 272.2 250.9 313.8 121.7 1.211 02m05.7s

11:06 44°59.2'N 092°58.8'E 1.0356 1.0725 21.0 274.7 249.5 335.7 119.8 1.319 02m02.2s

11:09 43°19.5'N 095°04.7'E 1.0350 1.0711 18.8 277.2 246.9 366.8 117.7 1.479 01m58.2s

11:12 41°31.9'N 097°33.5'E 1.0342 1.0695 16.1 279.8 242.6 415.3 115.0 1.734 01m53.6s

11:15 39°30.8'N 100°41.5'E 1.0331 1.0674 12.9 282.7 235.8 504.6 111.7 2.216 01m47.9s

11:18 36°59.6'N 105°18.3'E 1.0317 1.0644 8.1 286.3 223.6 760.8 107.0 3.632 01m40.2s

11:20.0 33°29.4'N 113°53.5'E 1.0292 1.0592 0.0 291.6 199.6 - 98.8 - 01m27.9s
Total Solar Eclipse of 2008 August 01

28

TABLE 5

LOCAL CIRCUMSTANCES ON THE CENTRAL LINE

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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

09:24 01m40.5s 7 08:31:20 288 297 5 09:23:10 108 120 09:24:50 288 300 10:17:47 108 122 10

09:27 01m49.3s 12 08:32:23 289 298 10 09:26:05 109 119 09:27:55 289 299 10:22:39 109 121 15

09:30 01m55.3s 16 08:34:02 289 298 14 09:29:02 109 119 09:30:58 289 299 10:26:54 110 119 18

09:33 02m00.1s 18 08:35:54 290 297 17 09:32:00 110 118 09:34:00 290 298 10:30:53 110 118 20

09:36 02m04.2s 21 08:37:56 290 297 19 09:34:58 111 117 09:37:02 291 297 10:34:41 111 116 22

09:39 02m07.8s 23 08:40:05 291 297 21 09:37:56 111 116 09:40:04 291 296 10:38:22 111 115 23

09:42 02m10.9s 24 08:42:19 291 296 23 09:40:55 112 115 09:43:05 292 295 10:41:56 112 113 25

09:45 02m13.6s 26 08:44:37 292 296 25 09:43:53 112 114 09:46:07 292 293 10:45:26 112 111 26

09:48 02m16.0s 27 08:46:59 292 295 27 09:46:52 113 112 09:49:08 293 292 10:48:51 113 110 27

09:51 02m18.2s 28 08:49:24 293 294 28 09:49:51 113 111 09:52:09 293 291 10:52:13 113 108 27

09:54 02m20.1s 29 08:51:53 293 293 30 09:52:50 114 110 09:55:10 294 290 10:55:31 114 107 28

09:57 02m21.7s 30 08:54:25 294 292 31 09:55:49 114 108 09:58:11 294 288 10:58:45 114 105 28

10:00 02m23.1s 31 08:56:59 294 291 32 09:58:48 114 107 10:01:12 294 287 11:01:57 114 103 29

10:03 02m24.3s 32 08:59:37 295 290 33 10:01:48 115 105 10:04:12 295 285 11:05:05 115 102 29

10:06 02m25.3s 32 09:02:17 295 289 35 10:04:47 115 104 10:07:13 295 284 11:08:11 115 100 29

10:09 02m26.0s 33 09:05:00 295 287 35 10:07:47 115 102 10:10:13 295 282 11:11:15 115 98 29

10:12 02m26.6s 33 09:07:45 296 286 36 10:10:47 116 101 10:13:13 296 281 11:14:16 116 97 29

10:15 02m27.0s 33 09:10:34 296 285 37 10:13:46 116 99 10:16:13 296 279 11:17:15 116 95 29

10:18 02m27.1s 33 09:13:24 296 283 38 10:16:46 116 97 10:19:13 296 277 11:20:11 116 94 28

10:21 02m27.1s 34 09:16:18 297 281 38 10:19:46 117 96 10:22:13 297 276 11:23:05 116 92 28

10:24 02m26.9s 33 09:19:14 297 280 39 10:22:46 117 94 10:25:13 297 274 11:25:57 116 90 27

10:27 02m26.5s 33 09:22:12 297 278 39 10:25:47 117 92 10:28:13 297 272 11:28:47 117 89 27

10:30 02m25.9s 33 09:25:13 298 276 39 10:28:47 117 91 10:31:13 297 270 11:31:35 117 87 26

10:33 02m25.2s 33 09:28:17 298 274 40 10:31:47 117 89 10:34:12 297 269 11:34:21 117 86 26

10:36 02m24.2s 32 09:31:24 298 272 40 10:34:48 118 87 10:37:12 298 267 11:37:04 117 84 25

10:39 02m23.0s 32 09:34:34 298 270 40 10:37:48 118 85 10:40:11 298 265 11:39:46 117 83 24

10:42 02m21.7s 31 09:37:46 298 268 39 10:40:49 118 84 10:43:11 298 264 11:42:25 117 82 23

10:45 02m20.1s 30 09:41:02 299 266 39 10:43:50 118 82 10:46:10 298 262 11:45:03 117 80 22

10:48 02m18.3s 29 09:44:21 299 264 38 10:46:51 118 80 10:49:09 298 260 11:47:38 117 79 21

10:51 02m16.3s 28 09:47:43 299 262 38 10:49:52 118 78 10:52:08 298 258 11:50:11 117 77 19

10:54 02m14.1s 27 09:51:08 299 260 37 10:52:53 118 77 10:55:07 298 257 11:52:41 117 76 18

10:57 02m11.6s 26 09:54:38 299 258 36 10:55:54 118 75 10:58:06 298 255 11:55:09 117 75 17

11:00 02m08.8s 25 09:58:11 299 255 35 10:58:55 118 73 11:01:04 298 253 11:57:33 117 73 15

11:03 02m05.7s 23 10:01:50 299 253 33 11:01:57 118 72 11:04:03 298 252 11:59:54 117 72 13

11:06 02m02.2s 21 10:05:34 299 251 32 11:04:59 118 70 11:07:01 298 250 12:02:11 117 71 11

11:09 01m58.2s 19 10:09:26 299 249 30 11:08:01 118 68 11:09:59 298 248 12:04:23 117 69 9

11:12 01m53.6s 16 10:13:27 298 246 27 11:11:03 117 66 11:12:57 297 246 12:06:28 116 68 6

11:15 01m47.9s 13 10:17:42 298 244 24 11:14:06 117 64 11:15:54 297 245 12:08:21 116 66 3

11:18 01m40.2s 8 10:22:28 297 241 19 11:17:10 116 62 11:18:50 296 242 - - - -
F. Espenak and J. Anderson

29 

TABLE 6

TOPOCENTRIC DATA AND PATH CORRECTIONS DUE TO LUNAR LIMB PROFILE

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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

09:24 3583.6 975.8 0.602 4.61 6.8 45.3 33.6 17.8 0.2 1.9 1.6 -8.1 0.2

09:27 3589.1 977.3 0.582 4.59 12.1 59.0 38.5 18.7 0.4 2.6 1.1 -5.9 0.1

09:30 3592.7 978.3 0.568 4.56 15.5 73.7 47.5 19.5 0.5 2.6 0.8 -5.1 -0.0

09:33 3595.5 979.0 0.558 4.54 18.3 91.8 61.0 20.1 0.6 2.3 0.5 -4.7 -0.1

09:36 3597.7 979.6 0.550 4.51 20.5 113.7 78.8 20.6 0.6 2.0 0.3 -4.4 -0.2

09:39 3599.7 980.2 0.542 4.48 22.5 136.3 97.9 21.2 0.7 2.0 0.2 -4.4 -0.5

09:42 3601.3 980.6 0.536 4.46 24.2 155.9 114.1 21.7 0.8 2.2 0.0 -4.6 -0.5

09:45 3602.7 981.0 0.531 4.43 25.7 170.9 125.9 22.2 1.0 2.3 -0.1 -4.9 -0.6

09:48 3604.0 981.3 0.527 4.41 27.0 182.2 134.2 22.6 1.2 2.3 -0.3 -5.9 -0.6

09:51 3605.1 981.6 0.523 4.38 28.2 190.9 140.0 23.1 1.4 2.8 -0.5 -7.2 -0.6

09:54 3606.0 981.9 0.519 4.36 29.2 198.0 144.2 23.5 1.6 3.2 -0.7 -8.5 -0.7

09:57 3606.8 982.1 0.516 4.33 30.2 203.9 147.3 23.9 1.8 3.5 -1.0 -9.7 -0.7

10:00 3607.5 982.3 0.514 4.31 30.9 209.0 149.5 24.3 1.9 3.7 -1.3-10.8 -0.7

10:03 3608.0 982.4 0.512 4.28 31.6 213.6 151.3 24.7 2.0 3.7 -1.7-11.7 -1.0

10:06 3608.5 982.6 0.510 4.25 32.2 217.7 152.6 25.0 2.1 3.6 -1.9-12.4 -1.0

10:09 3608.9 982.7 0.509 4.23 32.7 221.6 153.6 25.4 2.2 3.4 -1.9-12.9 -0.9

10:12 3609.1 982.7 0.508 4.20 33.0 225.2 154.4 25.7 2.2 3.3 -1.9-13.2 -0.9

10:15 3609.3 982.8 0.507 4.18 33.3 228.6 155.0 26.0 2.2 3.6 -1.9-13.3 -0.9

10:18 3609.4 982.8 0.507 4.15 33.4 231.9 155.3 26.3 2.2 3.7 -1.8-13.4 -0.9

10:21 3609.4 982.8 0.507 4.13 33.5 235.1 155.5 26.5 2.1 3.7 -1.8-13.8 -0.9

10:24 3609.3 982.8 0.507 4.10 33.5 238.1 155.6 26.8 2.0 4.0 -1.8-14.1 -0.9

10:27 3609.1 982.7 0.508 4.08 33.3 241.1 155.5 27.0 2.1 4.1 -1.7-14.1 -1.0

10:30 3608.8 982.6 0.509 4.05 33.1 244.0 155.3 27.2 2.0 4.4 -1.7-14.1 -1.0

10:33 3608.4 982.5 0.510 4.03 32.8 246.8 154.9 27.4 1.9 4.5 -1.7-14.0 -1.0

10:36 3607.9 982.4 0.512 4.00 32.3 249.5 154.4 27.6 1.9 4.6 -1.6-13.9 -0.9

10:39 3607.4 982.2 0.514 3.97 31.8 252.2 153.7 27.8 1.8 4.6 -1.6-13.6 -0.9

10:42 3606.7 982.1 0.516 3.95 31.1 254.8 152.9 27.9 1.7 4.6 -1.6-13.3 -0.9

10:45 3605.9 981.8 0.519 3.92 30.3 257.4 152.0 28.0 1.7 4.5 -1.5-12.9 -0.9

10:48 3605.0 981.6 0.522 3.90 29.5 260.0 150.9 28.1 1.6 4.2 -1.5-12.5 -0.6

10:51 3603.9 981.3 0.525 3.87 28.4 262.5 149.6 28.1 1.5 4.1 -1.5-12.1 -0.6

10:54 3602.7 981.0 0.529 3.85 27.3 264.9 148.1 28.1 1.5 4.0 -1.4-11.7 -0.6

10:57 3601.4 980.6 0.534 3.82 26.0 267.4 146.3 28.1 1.4 3.9 -1.3-11.3 -0.6

11:00 3599.9 980.2 0.539 3.80 24.5 269.8 144.3 28.1 1.4 3.7 -1.3-10.9 -0.6

11:03 3598.1 979.7 0.545 3.77 22.9 272.2 142.0 28.0 1.3 3.6 -1.2-10.5 -0.7

11:06 3596.1 979.2 0.551 3.75 21.0 274.7 139.4 27.8 1.3 3.4 -1.2-10.1 -0.7

11:09 3593.8 978.6 0.559 3.72 18.8 277.2 136.3 27.6 1.2 3.1 -1.1 -9.7 -0.7

11:12 3591.0 977.8 0.569 3.69 16.1 279.8 132.6 27.4 1.1 2.8 -1.1 -9.2 -0.6

11:15 3587.5 976.8 0.581 3.67 12.9 282.7 128.0 27.0 1.1 2.3 -1.1 -8.5 -0.6

11:18 3582.4 975.5 0.598 3.64 8.1 286.3 121.7 26.3 1.0 2.1 -1.0 -7.7 -0.7
Total Solar Eclipse of 2008 August 01

30

TABLE 7

MAPPING COORDINATES FOR THE UMBRAL PATH

TOTAL SOLAR ECLIPSE OF 2006 AUGUST 01

Longitude Latitude of: Circumstances on Central Line _

Northern Southern Central Universal Sun Sun Path Central

Limit Limit Line Time Alt Az. Width Durat.

h m s ° ° km

103°00.0'W 70°06.11'N - - - - - - -

102°00.0'W 70°39.82'N - 68°54.04'N 09:22:39 0.7 35.0 206.7 01m31.0s

101°00.0'W 71°12.86'N - 69°26.17'N 09:22:41 1.4 36.0 207.5 01m32.0s

100°00.0'W 71°45.18'N 68°20.79'N 69°57.71'N 09:22:45 2.0 36.9 208.3 01m33.0s

099°00.0'W 72°16.74'N 68°51.05'N 70°28.62'N 09:22:50 2.6 37.9 209.1 01m33.9s

098°00.0'W 72°47.49'N 69°20.76'N 70°58.87'N 09:22:57 3.2 38.9 209.8 01m34.9s

097°00.0'W 73°17.42'N 69°49.88'N 71°28.43'N 09:23:04 3.8 39.8 210.4 01m35.8s

096°00.0'W 73°46.47'N 70°18.38'N 71°57.27'N 09:23:12 4.4 40.8 211.1 01m36.7s

095°00.0'W 74°14.64'N 70°46.25'N 72°25.36'N 09:23:22 5.0 41.8 211.6 01m37.6s

094°00.0'W 74°41.91'N 71°13.45'N 72°52.68'N 09:23:32 5.5 42.8 212.2 01m38.5s

093°00.0'W 75°08.27'N 71°39.98'N 73°19.22'N 09:23:43 6.1 43.8 212.7 01m39.3s

092°00.0'W 75°33.70'N 72°05.81'N 73°44.96'N 09:23:54 6.6 44.8 213.2 01m40.2s

091°00.0'W 75°58.22'N 72°30.94'N 74°09.91'N 09:24:06 7.1 45.9 213.7 01m41.0s

090°00.0'W 76°21.82'N 72°55.36'N 74°34.05'N 09:24:19 7.5 46.9 214.1 01m41.8s

089°00.0'W 76°44.52'N 73°19.06'N 74°57.38'N 09:24:32 8.0 47.9 214.5 01m42.5s

088°00.0'W 77°06.33'N 73°42.04'N 75°19.92'N 09:24:46 8.5 49.0 214.8 01m43.3s

087°00.0'W 77°27.27'N 74°04.31'N 75°41.67'N 09:24:59 8.9 50.0 215.2 01m44.0s

086°00.0'W 77°47.35'N 74°25.86'N 76°02.63'N 09:25:13 9.3 51.0 215.5 01m44.7s

085°00.0'W 78°06.60'N 74°46.70'N 76°22.83'N 09:25:27 9.7 52.1 215.8 01m45.4s

084°00.0'W 78°25.04'N 75°06.85'N 76°42.27'N 09:25:41 10.1 53.1 216.1 01m46.0s

083°00.0'W 78°42.70'N 75°26.30'N 77°00.98'N 09:25:56 10.5 54.2 216.4 01m46.7s

082°00.0'W 78°59.61'N 75°45.08'N 77°18.96'N 09:26:10 10.9 55.2 216.6 01m47.3s

081°00.0'W 79°15.79'N 76°03.20'N 77°36.25'N 09:26:24 11.2 56.3 216.9 01m47.9s

080°00.0'W 79°31.27'N 76°20.67'N 77°52.87'N 09:26:38 11.6 57.3 217.1 01m48.4s

079°00.0'W 79°46.07'N 76°37.51'N 78°08.82'N 09:26:52 11.9 58.4 217.3 01m49.0s

078°00.0'W 80°00.23'N 76°53.73'N 78°24.14'N 09:27:06 12.2 59.5 217.5 01m49.5s

076°00.0'W 80°26.73'N 77°24.40'N 78°52.97'N 09:27:34 12.8 61.6 217.9 01m50.6s

074°00.0'W 80°50.96'N 77°52.81'N 79°19.52'N 09:28:01 13.4 63.7 218.2 01m51.5s

072°00.0'W 81°13.13'N 78°19.11'N 79°43.96'N 09:28:28 13.9 65.8 218.5 01m52.4s

070°00.0'W 81°33.41'N 78°43.45'N 80°06.45'N 09:28:54 14.4 68.0 218.8 01m53.3s

068°00.0'W 81°51.98'N 79°05.95'N 80°27.16'N 09:29:19 14.8 70.1 219.1 01m54.1s

066°00.0'W 82°09.00'N 79°26.75'N 80°46.21'N 09:29:44 15.3 72.2 219.3 01m54.8s

064°00.0'W 82°24.59'N 79°45.98'N 81°03.76'N 09:30:07 15.7 74.3 219.5 01m55.5s

062°00.0'W 82°38.89'N 80°03.74'N 81°19.91'N 09:30:30 16.0 76.5 219.7 01m56.2s

060°00.0'W 82°52.01'N 80°20.14'N 81°34.77'N 09:30:53 16.4 78.6 219.9 01m56.8s

058°00.0'W 83°04.05'N 80°35.28'N 81°48.46'N 09:31:15 16.7 80.7 220.0 01m57.4s

056°00.0'W 83°15.10'N 80°49.26'N 82°01.06'N 09:31:36 17.0 82.8 220.2 01m58.0s

054°00.0'W 83°25.25'N 81°02.14'N 82°12.65'N 09:31:56 17.4 84.9 220.3 01m58.5s

052°00.0'W 83°34.55'N 81°14.02'N 82°23.30'N 09:32:16 17.6 87.0 220.5 01m59.0s

050°00.0'W 83°43.08'N 81°24.95'N 82°33.09'N 09:32:36 17.9 89.2 220.6 01m59.5s

048°00.0'W 83°50.89'N 81°35.00'N 82°42.08'N 09:32:55 18.2 91.3 220.7 02m00.0s

046°00.0'W 83°58.04'N 81°44.22'N 82°50.31'N 09:33:14 18.4 93.4 220.9 02m00.5s

044°00.0'W 84°04.57'N 81°52.67'N 82°57.84'N 09:33:32 18.7 95.5 221.0 02m00.9s

042°00.0'W 84°10.52'N 82°00.38'N 83°04.72'N 09:33:50 18.9 97.6 221.1 02m01.3s

040°00.0'W 84°15.93'N 82°07.41'N 83°10.97'N 09:34:08 19.2 99.7 221.2 02m01.7s

038°00.0'W 84°20.82'N 82°13.78'N 83°16.63'N 09:34:25 19.4 101.8 221.3 02m02.1s

036°00.0'W 84°25.23'N 82°19.53'N 83°21.74'N 09:34:43 19.6 103.9 221.4 02m02.5s

034°00.0'W 84°29.18'N 82°24.69'N 83°26.32'N 09:35:00 19.8 106.0 221.5 02m02.9s

032°00.0'W 84°32.70'N 82°29.28'N 83°30.39'N 09:35:16 20.0 108.1 221.6 02m03.3s
F. Espenak and J. Anderson

31 

Table 7 (CONTINUED)

MAPPING COORDINATES FOR THE UMBRAL PATH

TOTAL SOLAR ECLIPSE OF 2006 AUGUST 01

Longitude Latitude of: Circumstances on Central Line _

Northern Southern Central Universal Sun Sun Path Central

Limit Limit Line Time Alt Az. Width Durat.

h m s ° ° km

030°00.0'W 84°35.80'N 82°33.32'N 83°33.98'N 09:35:33 20.2 110.2 221.7 02m03.6s

028°00.0'W 84°38.49'N 82°36.84'N 83°37.11'N 09:35:50 20.4 112.3 221.7 02m04.0s

026°00.0'W 84°40.80'N 82°39.85'N 83°39.78'N 09:36:06 20.6 114.4 221.8 02m04.3s

024°00.0'W 84°42.73'N 82°42.37'N 83°42.02'N 09:36:23 20.8 116.6 221.9 02m04.7s

022°00.0'W 84°44.30'N 82°44.40'N 83°43.83'N 09:36:39 21.0 118.7 222.0 02m05.0s

020°00.0'W 84°45.51'N 82°45.96'N 83°45.22'N 09:36:55 21.2 120.8 222.1 02m05.4s

018°00.0'W 84°46.37'N 82°47.05'N 83°46.20'N 09:37:12 21.3 122.9 222.2 02m05.7s

016°00.0'W 84°46.88'N 82°47.68'N 83°46.78'N 09:37:29 21.5 125.0 222.2 02m06.0s

014°00.0'W 84°47.04'N 82°47.85'N 83°46.95'N 09:37:45 21.7 127.1 222.3 02m06.3s

012°00.0'W 84°46.86'N 82°47.56'N 83°46.72'N 09:38:02 21.9 129.2 222.4 02m06.7s

010°00.0'W 84°46.33'N 82°46.81'N 83°46.08'N 09:38:19 22.1 131.3 222.5 02m07.0s

008°00.0'W 84°45.46'N 82°45.59'N 83°45.03'N 09:38:36 22.2 133.4 222.6 02m07.3s

006°00.0'W 84°44.23'N 82°43.90'N 83°43.57'N 09:38:54 22.4 135.6 222.7 02m07.6s

004°00.0'W 84°42.64'N 82°41.73'N 83°41.69'N 09:39:11 22.6 137.7 222.7 02m08.0s

002°00.0'W 84°40.68'N 82°39.06'N 83°39.37'N 09:39:29 22.8 139.8 222.8 02m08.3s

000°00.0'E 84°38.34'N 82°35.89'N 83°36.61'N 09:39:48 23.0 141.9 222.9 02m08.6s

002°00.0'E 84°35.61'N 82°32.20'N 83°33.40'N 09:40:07 23.1 144.1 223.0 02m09.0s

004°00.0'E 84°32.48'N 82°27.97'N 83°29.70'N 09:40:26 23.3 146.2 223.1 02m09.3s

006°00.0'E 84°28.92'N 82°23.17'N 83°25.52'N 09:40:46 23.5 148.3 223.2 02m09.6s

008°00.0'E 84°24.91'N 82°17.79'N 83°20.81'N 09:41:06 23.7 150.5 223.3 02m10.0s

010°00.0'E 84°20.44'N 82°11.78'N 83°15.55'N 09:41:27 23.9 152.6 223.4 02m10.3s

012°00.0'E 84°15.48'N 82°05.12'N 83°09.72'N 09:41:49 24.1 154.8 223.5 02m10.7s

014°00.0'E 84°09.98'N 81°57.77'N 83°03.28'N 09:42:11 24.3 156.9 223.6 02m11.1s

016°00.0'E 84°03.93'N 81°49.68'N 82°56.19'N 09:42:35 24.5 159.1 223.7 02m11.4s

018°00.0'E 83°57.28'N 81°40.81'N 82°48.41'N 09:42:59 24.7 161.3 223.8 02m11.8s

020°00.0'E 83°49.99'N 81°31.10'N 82°39.88'N 09:43:25 24.9 163.5 223.9 02m12.2s

022°00.0'E 83°42.00'N 81°20.48'N 82°30.55'N 09:43:52 25.1 165.7 224.0 02m12.6s

024°00.0'E 83°33.27'N 81°08.90'N 82°20.36'N 09:44:20 25.4 167.9 224.1 02m13.0s

026°00.0'E 83°23.72'N 80°56.27'N 82°09.23'N 09:44:50 25.6 170.1 224.3 02m13.5s

028°00.0'E 83°13.28'N 80°42.49'N 81°57.08'N 09:45:21 25.9 172.3 224.4 02m13.9s

030°00.0'E 83°01.87'N 80°27.48'N 81°43.82'N 09:45:54 26.1 174.6 224.5 02m14.4s

032°00.0'E 82°49.39'N 80°11.11'N 81°29.34'N 09:46:29 26.4 176.9 224.7 02m14.9s

034°00.0'E 82°35.73'N 79°53.26'N 81°13.53'N 09:47:07 26.6 179.1 224.9 02m15.4s

036°00.0'E 82°20.77'N 79°33.77'N 80°56.24'N 09:47:47 26.9 181.5 225.1 02m15.9s

038°00.0'E 82°04.37'N 79°12.50'N 80°37.33'N 09:48:30 27.2 183.8 225.2 02m16.4s

040°00.0'E 81°46.36'N 78°49.24'N 80°16.61'N 09:49:17 27.5 186.2 225.5 02m17.0s

042°00.0'E 81°26.56'N 78°23.78'N 79°53.89'N 09:50:07 27.9 188.6 225.7 02m17.6s

044°00.0'E 81°04.74'N 77°55.88'N 79°28.92'N 09:51:02 28.2 191.0 225.9 02m18.2s

046°00.0'E 80°40.65'N 77°25.27'N 79°01.45'N 09:52:01 28.6 193.5 226.2 02m18.9s

048°00.0'E 80°14.01'N 76°51.64'N 78°31.18'N 09:53:06 28.9 196.0 226.5 02m19.5s

050°00.0'E 79°44.49'N 76°14.63'N 77°57.76'N 09:54:18 29.3 198.6 226.9 02m20.3s

051°00.0'E 79°28.52'N 75°54.73'N 77°39.74'N 09:54:56 29.5 199.9 227.1 02m20.6s

052°00.0'E 79°11.68'N 75°33.84'N 77°20.79'N 09:55:37 29.7 201.3 227.3 02m21.0s

053°00.0'E 78°53.91'N 75°11.89'N 77°00.84'N 09:56:19 30.0 202.6 227.5 02m21.4s

054°00.0'E 78°35.16'N 74°48.84'N 76°39.83'N 09:57:04 30.2 204.0 227.7 02m21.7s

055°00.0'E 78°15.34'N 74°24.60'N 76°17.70'N 09:57:51 30.4 205.4 228.0 02m22.1s

056°00.0'E 77°54.40'N 73°59.12'N 75°54.37'N 09:58:41 30.6 206.8 228.2 02m22.5s

057°00.0'E 77°32.26'N 73°32.33'N 75°29.78'N 09:59:33 30.8 208.3 228.5 02m22.9s

058°00.0'E 77°08.83'N 73°04.16'N 75°03.86'N 10:00:28 31.1 209.8 228.8 02m23.3s

059°00.0'E 76°44.04'N 72°34.53'N 74°36.51'N 10:01:27 31.3 211.3 229.1 02m23.7s

060°00.0'E 76°17.80'N 72°03.37'N 74°07.66'N 10:02:28 31.5 212.8 229.5 02m24.1s
Total Solar Eclipse of 2008 August 01

32

Table 7 (CONTINUED)

MAPPING COORDINATES FOR THE UMBRAL PATH

TOTAL SOLAR ECLIPSE OF 2006 AUGUST 01

Longitude Latitude of: Circumstances on Central Line _

Northern Southern Central Universal Sun Sun Path Central

Limit Limit Line Time Alt Az. Width Durat.

h m s ° ° km

061°00.0'E 75°50.00'N 71°30.60'N 73°37.23'N 10:03:34 31.7 214.4 229.9 02m24.5s

062°00.0'E 75°20.56'N 70°56.16'N 73°05.13'N 10:04:43 32.0 216.0 230.3 02m24.9s

063°00.0'E 74°49.38'N 70°19.97'N 72°31.27'N 10:05:56 32.2 217.7 230.7 02m25.3s

064°00.0'E 74°16.36'N 69°41.95'N 71°55.57'N 10:07:14 32.4 219.4 231.2 02m25.6s

065°00.0'E 73°41.38'N 69°02.05'N 71°17.94'N 10:08:36 32.6 221.1 231.7 02m26.0s

066°00.0'E 73°04.35'N 68°20.22'N 70°38.30'N 10:10:02 32.8 222.9 232.3 02m26.3s

067°00.0'E 72°25.18'N 67°36.40'N 69°56.59'N 10:11:34 33.0 224.7 232.9 02m26.5s

068°00.0'E 71°43.77'N 66°50.58'N 69°12.75'N 10:13:10 33.1 226.6 233.5 02m26.8s

069°00.0'E 71°00.03'N 66°02.73'N 68°26.73'N 10:14:52 33.3 228.5 234.2 02m27.0s

070°00.0'E 70°13.91'N 65°12.88'N 67°38.50'N 10:16:40 33.4 230.5 235.0 02m27.1s

071°00.0'E 69°25.36'N 64°21.05'N 66°48.07'N 10:18:32 33.5 232.5 235.8 02m27.2s

072°00.0'E 68°34.35'N 63°27.33'N 65°55.46'N 10:20:30 33.5 234.6 236.6 02m27.1s

073°00.0'E 67°40.90'N 62°31.81'N 65°00.72'N 10:22:34 33.5 236.7 237.6 02m27.0s

074°00.0'E 66°45.05'N 61°34.62'N 64°03.96'N 10:24:42 33.4 238.8 238.6 02m26.8s

075°00.0'E 65°46.89'N 60°35.94'N 63°05.32'N 10:26:54 33.3 241.0 239.6 02m26.5s

076°00.0'E 64°46.56'N 59°35.97'N 62°04.97'N 10:29:11 33.2 243.2 240.7 02m26.1s

077°00.0'E 63°44.25'N 58°34.95'N 61°03.13'N 10:31:32 32.9 245.4 241.8 02m25.6s

078°00.0'E 62°40.19'N 57°33.14'N 60°00.05'N 10:33:55 32.6 247.6 243.0 02m24.9s

079°00.0'E 61°34.67'N 56°30.82'N 58°56.04'N 10:36:20 32.3 249.8 244.1 02m24.1s

080°00.0'E 60°28.00'N 55°28.28'N 57°51.38'N 10:38:46 31.8 252.0 245.3 02m23.1s

081°00.0'E 59°20.53'N 54°25.80'N 56°46.42'N 10:41:12 31.3 254.2 246.4 02m22.0s

082°00.0'E 58°12.65'N 53°23.67'N 55°41.47'N 10:43:38 30.7 256.3 247.5 02m20.8s

083°00.0'E 57°04.71'N 52°22.15'N 54°36.85'N 10:46:01 30.1 258.3 248.5 02m19.5s

084°00.0'E 55°57.08'N 51°21.48'N 53°32.85'N 10:48:23 29.3 260.3 249.5 02m18.1s

085°00.0'E 54°50.10'N 50°21.86'N 52°29.75'N 10:50:41 28.6 262.2 250.2 02m16.5s

086°00.0'E 53°44.08'N 49°23.49'N 51°27.78'N 10:52:54 27.7 264.0 250.9 02m14.9s

087°00.0'E 52°39.28'N 48°26.52'N 50°27.15'N 10:55:03 26.9 265.8 251.3 02m13.2s

088°00.0'E 51°35.94'N 47°31.05'N 49°28.02'N 10:57:08 25.9 267.5 251.6 02m11.5s

089°00.0'E 50°34.24'N 46°37.19'N 48°30.51'N 10:59:06 25.0 269.1 251.6 02m09.6s

090°00.0'E 49°34.31'N 45°44.99'N 47°34.72'N 11:00:59 24.0 270.6 251.4 02m07.8s

091°00.0'E 48°36.25'N 44°54.50'N 46°40.73'N 11:02:46 23.0 272.0 251.0 02m05.9s

092°00.0'E 47°40.14'N 44°05.73'N 45°48.56'N 11:04:27 22.0 273.4 250.4 02m04.0s

093°00.0'E 46°46.01'N 43°18.69'N 44°58.24'N 11:06:02 20.9 274.7 249.5 02m02.1s

094°00.0'E 45°53.88'N 42°33.38'N 44°09.76'N 11:07:31 19.9 275.9 248.4 02m00.2s

095°00.0'E 45°03.73'N 41°49.76'N 43°23.12'N 11:08:54 18.8 277.1 247.0 01m58.3s

096°00.0'E 44°15.55'N 41°07.82'N 42°38.27'N 11:10:11 17.8 278.2 245.5 01m56.5s

097°00.0'E 43°29.30'N 40°27.51'N 41°55.20'N 11:11:22 16.7 279.2 243.7 01m54.6s

098°00.0'E 42°44.93'N 39°48.81'N 41°13.86'N 11:12:28 15.7 280.2 241.8 01m52.8s

099°00.0'E 42°02.40'N 39°11.65'N 40°34.19'N 11:13:29 14.6 281.2 239.7 01m50.9s

100°00.0'E 41°21.65'N 38°36.00'N 39°56.16'N 11:14:25 13.6 282.1 237.4 01m49.2s

101°00.0'E 40°42.62'N 38°01.82'N 39°19.71'N 11:15:15 12.5 282.9 235.0 01m47.4s

102°00.0'E 40°05.25'N 37°29.05'N 38°44.79'N 11:16:01 11.5 283.8 232.5 01m45.7s

103°00.0'E 39°29.49'N 36°57.65'N 38°11.34'N 11:16:42 10.5 284.6 229.9 01m44.0s

104°00.0'E 38°55.28'N 36°27.57'N 37°39.32'N 11:17:19 9.5 285.3 227.2 01m42.3s

105°00.0'E 38°22.56'N 35°58.77'N 37°08.67'N 11:17:51 8.4 286.0 224.5 01m40.7s

106°00.0'E 37°51.27'N 35°31.21'N 36°39.35'N 11:18:19 7.5 286.7 221.7 01m39.1s

107°00.0'E 37°21.37'N 35°04.84'N 36°11.31'N 11:18:44 6.5 287.4 218.8 01m37.5s

108°00.0'E 36°52.79'N 34°39.62'N 35°44.51'N 11:19:04 5.5 288.1 216.0 01m36.0s

109°00.0'E 36°25.50'N 34°15.52'N 35°18.89'N 11:19:21 4.5 288.7 213.1 01m34.5s

110°00.0'E 35°59.43'N 33°52.49'N 34°54.43'N 11:19:35 3.6 289.3 210.2 01m33.1s

111°00.0'E 35°34.56'N 33°30.50'N 34°31.07'N 11:19:45 2.6 289.9 207.4 01m31.7s
F. Espenak and J. Anderson

33 

TABLE 8

MAPPING COORDINATES FOR THE ZONES OF GRAZING ECLIPSE

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

North Graze Zone Northern South Graze Zone Southern

Longitude Latitudes Limit Latitudes Limit .

Northern Southern Universal Northern Southern Universal Path Elev Scale

Limit Limit Time Limit Limit Time Azm Fact Fact

h m s h m s ° km/"

061°00.0'E 75°53.73'N 75°51.91'N 10:00:39 71°28.73'N 71°18.12'N 10:06:29 151.6 -1.44 3.12

062°00.0'E 75°24.29'N 75°22.52'N 10:01:39 70°54.28'N 70°43.45'N 10:07:46 152.1 -1.44 3.13

063°00.0'E 74°53.11'N 74°51.38'N 10:02:43 70°18.09'N 70°07.06'N 10:09:08 152.6 -1.44 3.13

064°00.0'E 74°20.05'N 74°18.40'N 10:03:52 69°40.08'N 69°28.88'N 10:10:34 153.1 -1.44 3.13

065°00.0'E 73°45.03'N 73°43.47'N 10:05:04 69°00.19'N 68°48.86'N 10:12:04 153.5 -1.45 3.13

066°00.0'E 73°07.93'N 73°06.48'N 10:06:22 68°18.36'N 68°06.94'N 10:13:39 153.9 -1.45 3.14

067°00.0'E 72°28.67'N 72°27.33'N 10:07:44 67°34.55'N 67°23.09'N 10:15:19 154.3 -1.45 3.14

068°00.0'E 71°47.13'N 71°45.95'N 10:09:11 66°48.74'N 66°37.29'N 10:17:04 154.6 -1.46 3.15

069°00.0'E 71°03.25'N 71°02.25'N 10:10:44 66°00.91'N 65°49.17'N 10:18:54 154.9 -1.46 3.16

070°00.0'E 70°17.27'N 70°16.15'N 10:12:23 65°11.07'N 64°59.08'N 10:20:49 155.2 -1.47 3.17

071°00.0'E 69°28.86'N 69°27.60'N 10:14:07 64°19.27'N 64°07.07'N 10:22:48 155.4 -1.47 3.18

072°00.0'E 68°37.96'N 68°36.56'N 10:15:57 63°25.57'N 63°13.35'N 10:24:53 155.5 -1.48 3.19

073°00.0'E 67°44.57'N 67°43.07'N 10:17:53 62°30.06'N 62°17.73'N 10:27:01 155.6 -1.49 3.21

074°00.0'E 66°48.74'N 66°47.18'N 10:19:55 61°32.90'N 61°20.51'N 10:29:14 155.6 -1.50 3.22

075°00.0'E 65°50.71'N 65°48.97'N 10:22:03 60°34.25'N 60°21.86'N 10:31:30 155.5 -1.52 3.24

076°00.0'E 64°50.60'N 64°48.61'N 10:24:15 59°34.31'N 59°21.99'N 10:33:49 155.3 -1.53 3.26

077°00.0'E 63°48.36'N 63°46.32'N 10:26:33 58°33.32'N 58°21.11'N 10:36:10 155.1 -1.54 3.28

078°00.0'E 62°44.47'N 62°42.20'N 10:28:55 57°31.54'N 57°19.50'N 10:38:33 154.7 -1.56 3.31

079°00.0'E 61°39.11'N 61°36.62'N 10:31:20 56°29.26'N 56°17.42'N 10:40:57 154.3 -1.58 3.33

080°00.0'E 60°32.54'N 60°29.90'N 10:33:48 55°26.75'N 55°15.14'N 10:43:20 153.8 -1.60 3.36

081°00.0'E 59°25.13'N 59°22.38'N 10:36:18 54°24.31'N 54°12.94'N 10:45:42 153.2 -1.61 3.39

082°00.0'E 58°17.26'N 58°14.44'N 10:38:48 53°22.17'N 53°11.19'N 10:48:02 152.4 -1.63 3.42

083°00.0'E 57°09.29'N 57°06.44'N 10:41:18 52°20.69'N 52°09.95'N 10:50:20 151.6 -1.66 3.45

084°00.0'E 56°01.61'N 55°58.76'N 10:43:46 51°20.05'N 51°09.56'N 10:52:34 150.7 -1.68 3.48

085°00.0'E 54°54.56'N 54°51.73'N 10:46:12 50°20.48'N 50°10.24'N 10:54:44 149.7 -1.70 3.52

086°00.0'E 53°48.30'N 53°45.63'N 10:48:35 49°22.14'N 49°12.14'N 10:56:50 148.6 -1.72 3.55

087°00.0'E 52°43.42'N 52°40.80'N 10:50:53 48°25.20'N 48°15.44'N 10:58:51 147.5 -1.74 3.58

088°00.0'E 51°39.98'N 51°37.42'N 10:53:06 47°29.77'N 47°20.22'N 11:00:46 146.2 -1.76 3.61

089°00.0'E 50°38.18'N 50°35.67'N 10:55:15 46°35.93'N 46°26.60'N 11:02:36 144.9 -1.78 3.64

090°00.0'E 49°38.15'N 49°35.70'N 10:57:17 45°43.77'N 45°34.62'N 11:04:20 143.6 -1.79 3.66

091°00.0'E 48°40.01'N 48°37.62'N 10:59:14 44°53.30'N 44°44.35'N 11:05:59 142.2 -1.81 3.69

092°00.0'E 47°43.81'N 47°41.48'N 11:01:04 44°04.56'N 43°55.80'N 11:07:32 140.8 -1.82 3.71

093°00.0'E 46°49.59'N 46°47.33'N 11:02:48 43°17.55'N 43°08.97'N 11:08:59 139.3 -1.84 3.73

094°00.0'E 45°57.36'N 45°55.17'N 11:04:26 42°32.25'N 42°23.87'N 11:10:20 137.8 -1.85 3.75

095°00.0'E 45°07.11'N 45°05.00'N 11:05:57 41°48.66'N 41°40.52'N 11:11:35 136.4 -1.86 3.76

096°00.0'E 44°18.83'N 44°16.80'N 11:07:22 41°06.73'N 40°58.79'N 11:12:46 134.9 -1.86 3.77

097°00.0'E 43°32.47'N 43°30.53'N 11:08:41 40°26.45'N 40°18.70'N 11:13:50 133.4 -1.87 3.78

098°00.0'E 42°48.00'N 42°46.15'N 11:09:55 39°47.75'N 39°40.21'N 11:14:50 131.9 -1.87 3.79

099°00.0'E 42°05.36'N 42°03.61'N 11:11:02 39°10.61'N 39°03.29'N 11:15:44 130.4 -1.87 3.79

100°00.0'E 41°24.39'N 41°22.73'N 11:12:04 38°34.97'N 38°27.89'N 11:16:34 129.0 -1.87 3.79

101°00.0'E 40°45.23'N 40°43.68'N 11:13:01 38°00.78'N 37°53.93'N 11:17:19 127.5 -1.87 3.79

102°00.0'E 40°07.73'N 40°06.30'N 11:13:52 37°27.67'N 37°21.01'N 11:18:00 126.1 -1.87 3.79

103°00.0'E 39°31.78'N 39°30.48'N 11:14:39 36°56.67'N 36°50.03'N 11:18:36 124.7 -1.87 3.78

104°00.0'E 38°57.55'N 38°56.36'N 11:15:21 36°26.60'N 36°20.02'N 11:19:08 123.4 -1.86 3.78

105°00.0'E 38°24.72'N 38°23.63'N 11:15:58 35°57.79'N 35°51.36'N 11:19:36 122.1 -1.86 3.77

106°00.0'E 37°53.42'N 37°52.34'N 11:16:31 35°35.45'N 35°35.45'N 11:19:56 120.8 -1.85 3.76

107°00.0'E 37°23.52'N 37°22.43'N 11:17:00 35°04.84'N 35°04.84'N 11:20:21 119.5 -1.85 3.75

108°00.0'E 36°54.92'N 36°53.84'N 11:17:24 34°39.62'N 34°39.62'N 11:20:38 118.3 -1.84 3.74

109°00.0'E 36°27.61'N 36°26.54'N 11:17:45 34°15.52'N 34°15.52'N 11:20:51 117.0 -1.83 3.72

110°00.0'E 36°01.53'N 36°00.48'N 11:18:03 33°52.49'N 33°52.49'N 11:21:01 115.8 -1.81 3.69

111°00.0'E 35°36.63'N 35°35.60'N 11:18:16 33°30.51'N 33°30.51'N 11:21:09 114.5 -1.74 3.59

112°00.0'E 35°12.88'N 35°11.87'N 11:18:27 33°09.54'N 33°09.54'N 11:21:13 113.3 -1.63 3.42

113°00.0'E 34°50.26'N 34°49.27'N 11:18:34 32°49.51'N 32°49.51'N 11:21:14 113.0 -2.46 4.74
Total Solar Eclipse of 2008 August 01

34

TABLE 9

LOCAL CIRCUMSTANCES FOR CANADA AND NORTH ATLANTIC

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

CANADAAlert, NT 82°31'N 062°20'W 29 08:36:11.2 289 296 15 09:32:06.3 41 49 09:32:48.8 358 6 10:29:31.1 111 119 18 09:32:27.6 200 207 16 77 1.035 1.000 0.069 00m43sCambridge Bay, * 69°03'N 105°05'W — — — — 10:15:34.5 108 123 3 09:24:05.8 197 209 1 32 0.999 1.000Charlottetown, * 46°14'N 063°08'W 55 — — — 09:26:01.3 65 107 4 08:58 Rise — — 0 63 0.319 0.207Chicoutimi, QC 48°26'N 071°04'W — — — — 09:34:25.0 73 112 2 09:23 Rise — — 0 62 0.174 0.086Fredericton, NB 45°58'N 066°39'W 9 — — — 09:27:28.5 66 108 2 09:13 Rise — — 0 63 0.198 0.104Grise Fiord, NU 76°25'N 082°54'W 37 08:31:13.5 289 298 8 09:24:17.8 131 143 09:25:55.7 266 277 10:20:07.1 108 121 13 09:25:06.8 18 30 10 54 1.033 1.000 0.614 01m38sHalifax, NS 44°39'N 063°36'W 25 — — — 09:22:59.2 62 106 3 09:05 Rise — — 0 64 0.223 0.123Iqaluit, NU 63°44'N 068°28'W 34 08:14:13.8 300 321 2 — — 09:58:44.6 92 119 12 09:05:27.3 16 41 6 61 0.767 0.713Moncton, NB 46°06'N 064°47'W 12 — — — 09:26:39.8 66 108 3 09:05 Rise — — 0 63 0.271 0.164Québec, QC 46°49'N 071°14'W 73 — — — 09:31:44.4 70 111 1 09:29 Rise — — 0 63 0.044 0.011Resolute, NT 74°41'N 094°54'W 67 08:33:06.9 287 295 5 — — 10:19:24.3 109 122 10 09:25:44.9 198 209 7 43 0.997 0.998Saint John, NB 45°16'N 066°03'W 36 — — — 09:25:45.0 65 107 2 09:13 Rise — — 0 64 0.177 0.088Saint John's, NF 47°34'N 052°43'W 64 — — — 09:24:20.0 61 105 11 08:43:23.2 15 56 5 68 0.317 0.205Sydney, NS 46°09'N 060°11'W 5 — — — 09:24:17.3 63 106 6 08:47 Rise — — 0 63 0.340 0.227FAEROE ISLANDSTorshavn 62°01'N 006°46'W — 08:20:34.6 320 349 28 — — 10:17:50.3 83 103 40 09:18:02.0 21 47 34 120 0.516 0.414GREENLANDGodthåb 64°11'N 051°44'W 20 08:11:20.9 306 330 8 — — 09:59:01.0 89 116 19 09:03:59.3 17 44 13 76 0.689 0.617ICELANDReykjavík 64°09'N 021°51'W 28 08:14:44.3 314 341 21 — — 10:09:19.6 85 109 32 09:10:45.0 19 46 27 104 0.585 0.493ST. PIERRE & MIQUELONSaint Pierre 46°47'N 056°11'W — — — — 09:23:49.3 62 105 9 08:43:13.4 14 56 2 66 0.325 0.213

TABLE 10

LOCAL CIRCUMSTANCES FOR UNITED KINGDOM

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

UNITED KINGDOMENGLANDBirmingham 52°30'N 001°50'W 163 08:29:39.7 340 19 35 — — 10:04:53.0 64 92 47 09:16:18.9 22 57 41 118 0.245 0.142Bristol 51°27'N 002°35'W — 08:30:47.9 343 23 35 — — 10:00:34.4 61 92 47 09:14:47.4 22 58 41 116 0.213 0.115Coventry 52°25'N 001°30'W — 08:30:06.5 341 19 35 — — 10:05:11.1 64 92 47 09:16:42.0 22 57 41 118 0.243 0.140Leeds 53°50'N 001°35'W — 08:27:59.7 337 14 34 — — 10:08:44.3 67 94 47 09:17:20.6 22 55 41 120 0.286 0.177Liverpool 53°25'N 002°55'W 60 08:27:21.5 338 15 33 — — 10:05:40.7 66 94 46 09:15:29.4 22 56 40 117 0.272 0.165London 51°30'N 000°10'W 45 08:33:01.1 343 22 36 — — 10:04:46.3 62 90 49 09:18:01.8 22 57 43 119 0.218 0.119Manchester 53°30'N 002°15'W — 08:27:50.2 338 15 34 — — 10:06:53.8 66 94 47 09:16:20.8 22 56 40 118 0.275 0.168Middlesbrough 54°35'N 001°14'W — 08:27:25.0 335 11 34 — — 10:11:01.2 69 94 47 09:18:10.4 22 54 41 121 0.309 0.198Newcastle 54°59'N 001°35'W — 08:26:42.1 334 10 34 — — 10:11:23.6 70 95 46 09:17:58.9 22 54 40 121 0.320 0.209Nottingham 52°58'N 001°10'W — 08:29:33.3 339 17 35 — — 10:07:12.2 65 93 47 09:17:24.3 22 56 41 119 0.260 0.155Sheffield 53°23'N 001°30'W — 08:28:39.6 338 15 34 — — 10:07:45.1 66 93 47 09:17:12.2 22 56 41 119 0.272 0.165IRELAND, NORTHBelfast 54°35'N 005°55'W 17 08:23:31.1 335 11 31 — — 10:04:25.7 68 96 44 09:12:50.8 21 55 38 114 0.304 0.194SCOTLANDEdinburgh 55°57'N 003°13'W 134 08:24:31.1 332 7 32 — — 10:11:10.8 71 96 45 09:16:43.6 22 53 39 119 0.346 0.234Glasgow 55°53'N 004°15'W — 08:23:45.5 332 7 31 — — 10:09:39.4 71 97 44 09:15:34.0 22 53 38 118 0.344 0.231WALESCardiff 51°29'N 003°13'W 62 08:30:07.8 343 23 34 — — 09:59:39.8 60 92 47 09:13:59.4 22 58 41 115 0.213 0.115
F. Espenak and J. Anderson

35 

TABLE 11

LOCAL CIRCUMSTANCES FOR EUROPE — ALBANIA TO ITALY

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 09:38:38.7 16 44 62 — — 10:18:12.4 43 57 66 09:58:27.0 29 51 64 152 0.027 0.006AUSTRIAVienna 48°13'N 016°20'E 202 08:57:54.5 350 23 51 — — 10:32:29.4 64 73 59 09:44:57.1 27 50 56 146 0.195 0.102BELARUSGomel' 52°25'N 031°00'E — 09:01:20.2 333 348 53 — — 11:07:10.9 85 68 53 10:04:51.5 29 28 55 181 0.438 0.329Minsk 53°54'N 027°34'E 225 08:55:17.1 332 350 51 — — 11:00:44.5 84 73 53 09:58:19.6 28 32 54 173 0.443 0.333BELGIUMAntwerpen 51°13'N 004°25'E — 08:38:04.1 344 21 40 — — 10:12:24.3 63 87 52 09:24:28.5 24 56 46 126 0.221 0.122Brussels 50°50'N 004°20'E — 08:38:51.3 345 23 40 — — 10:11:11.1 62 87 52 09:24:16.8 24 56 46 126 0.209 0.112Liège 50°38'N 005°34'E — 08:40:32.9 346 23 41 — — 10:13:06.7 62 86 53 09:26:07.8 24 56 47 127 0.207 0.111BOSNIA & HERZEGOWINASarajevo 43°52'N 018°25'E — 09:18:47.9 4 36 57 — — 10:26:24.9 53 64 63 09:52:34.4 28 51 61 149 0.087 0.031BULGARIASofia 42°41'N 023°19'E 550 09:26:53.4 3 29 62 — — 10:41:03.1 57 53 65 10:04:07.0 30 43 64 164 0.104 0.040CROATIAZagreb 45°48'N 015°58'E — 09:07:08.2 358 33 53 — — 10:25:04.5 57 70 61 09:45:56.6 27 53 58 144 0.122 0.051CZECH REPUBLICOstrava 49°50'N 018°17'E — 08:54:56.8 344 15 50 — — 10:40:02.5 70 74 58 09:47:17.4 27 46 55 152 0.257 0.152Praha 50°05'N 014°26'E 202 08:50:36.4 345 18 48 — — 10:31:25.1 67 78 57 09:40:37.0 26 50 53 143 0.236 0.134DENMARKCopenhagen 55°40'N 012°35'E 13 08:38:25.6 332 1 42 — — 10:35:16.5 77 87 51 09:36:14.6 25 46 48 143 0.385 0.273ESTONIATallinn 59°25'N 024°45'E — 08:45:26.6 322 340 45 — — 10:55:05.0 90 85 48 09:50:17.1 26 33 48 167 0.556 0.460FINLANDHelsinki 60°10'N 024°58'E 9 08:44:58.1 321 338 44 — — 10:55:09.1 91 86 47 09:50:05.0 26 33 47 167 0.576 0.483FRANCELille 50°38'N 003°04'E 43 08:38:04.4 346 24 39 — — 10:08:06.6 61 88 51 09:22:20.6 23 57 46 123 0.199 0.105Lyon 45°45'N 004°51'E 286 08:59:17.1 5 47 46 — — 09:50:29.5 43 78 53 09:24:40.8 24 63 49 122 0.054 0.015Paris 48°52'N 002°20'E 50 08:42:15.7 352 32 40 — — 10:00:32.6 55 86 51 09:20:48.1 23 60 46 121 0.143 0.064GERMANYAachen 50°47'N 006°05'E — 08:40:41.8 345 22 41 — — 10:14:34.7 63 86 53 09:26:56.4 24 56 48 128 0.214 0.116Berlin 52°30'N 013°22'E — 08:44:06.6 339 11 45 — — 10:32:58.0 72 82 55 09:38:01.3 26 48 51 143 0.300 0.190Bonn 50°44'N 007°05'E — 08:41:48.0 345 22 42 — — 10:16:31.3 63 85 53 09:28:29.4 24 55 48 130 0.216 0.118Bremen 53°04'N 008°49'E 16 08:38:42.8 339 12 42 — — 10:24:58.3 70 86 53 09:31:07.5 24 51 48 135 0.293 0.184Dortmund 51°31'N 007°28'E — 08:40:23.7 343 19 42 — — 10:19:12.4 66 86 53 09:29:05.9 24 54 48 131 0.241 0.139Dresden 51°03'N 013°44'E — 08:47:32.4 343 15 46 — — 10:31:31.0 69 80 56 09:39:04.2 26 50 52 143 0.260 0.154Duisburg 51°25'N 006°46'E — 08:39:55.7 343 19 41 — — 10:17:33.8 65 86 53 09:28:01.8 24 54 48 130 0.236 0.134Düsseldorf 51°12'N 006°47'E — 08:40:25.3 344 20 42 — — 10:17:04.4 64 86 53 09:28:02.6 24 55 48 130 0.229 0.128Frankfurt 50°07'N 008°40'E 103 08:44:55.1 347 23 44 — — 10:18:20.5 63 83 55 09:31:02.1 25 55 50 132 0.205 0.109Hamburg 53°33'N 009°59'E 20 08:39:00.7 337 10 42 — — 10:27:58.1 72 86 53 09:32:48.2 25 50 48 137 0.312 0.202Hannover 52°24'N 009°44'E — 08:40:48.0 340 14 43 — — 10:25:32.8 69 85 53 09:32:30.6 25 51 49 136 0.278 0.170Cologne 50°56'N 006°59'E — 08:41:13.7 345 21 42 — — 10:16:49.3 64 85 53 09:28:20.4 24 55 48 130 0.222 0.123Leipzig 51°19'N 012°20'E — 08:45:34.2 343 16 45 — — 10:28:56.7 68 82 55 09:36:43.9 25 51 51 140 0.259 0.154Mannheim 49°29'N 008°29'E — 08:46:30.6 349 26 44 — — 10:16:12.4 61 83 55 09:30:47.9 25 56 50 131 0.185 0.094München 48°08'N 011°34'E 530 08:53:49.7 352 29 48 — — 10:19:48.0 59 78 57 09:36:24.8 26 55 53 136 0.161 0.076Nürnberg 49°27'N 011°04'E 320 08:49:06.9 348 24 46 — — 10:22:08.9 63 80 56 09:35:08.5 25 54 52 136 0.197 0.103Stuttgart 48°46'N 009°11'E — 08:49:24.9 351 28 45 — — 10:15:44.1 59 81 56 09:32:04.8 25 56 51 132 0.167 0.080HUNGARYBudapest 47°30'N 019°05'E 120 09:02:45.4 351 21 53 — — 10:38:27.3 65 69 60 09:50:30.2 28 47 58 153 0.197 0.103IRELANDDublin 53°20'N 006°15'W 47 08:24:34.6 338 16 31 — — 10:00:41.6 65 95 44 09:11:33.8 21 57 38 113 0.267 0.161ITALYBologna 44°29'N 011°20'E — 09:12:27.8 8 46 52 — — 10:02:46.3 45 72 59 09:37:30.3 26 60 56 133 0.048 0.013Milan 45°28'N 009°12'E — 09:04:22.6 4 44 49 — — 10:01:48.7 47 76 57 09:32:53.5 25 61 53 129 0.066 0.020Turin 45°03'N 007°40'E — 09:06:24.7 7 48 49 — — 09:53:56.9 43 75 56 09:30:02.4 25 62 52 126 0.045 0.011
Total Solar Eclipse of 2008 August 01

36

TABLE 12

LOCAL CIRCUMSTANCES FOR EUROPE — LATVIA TO UKRAINE

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

LATVIARiga 56°57'N 024°06'E — 08:47:29.9 327 347 47 — — 10:54:37.0 86 81 51 09:51:04.8 27 35 50 165 0.491 0.386LIECHTENSTEINVaduz 47°09'N 009°31'E — 08:55:48.9 356 35 47 — — 10:10:56.8 54 79 57 09:33:00.9 25 58 52 131 0.119 0.049LITHUANIAVilnius 54°41'N 025°19'E — 08:51:49.6 331 352 49 — — 10:56:46.8 84 76 53 09:54:26.7 27 35 53 168 0.443 0.333LUXEMBOURGLuxembourg 49°36'N 006°09'E 334 08:43:51.4 349 27 42 — — 10:11:19.1 60 84 53 09:26:58.2 24 57 48 127 0.178 0.089MACEDONIASkopje 41°59'N 021°26'E 240 09:31:30.8 9 37 62 — — 10:30:34.2 51 55 66 10:01:06.1 30 47 64 158 0.063 0.019MOLDOVAKisin'ov 47°00'N 028°50'E — 09:12:36.3 345 5 59 — — 11:03:20.6 74 57 59 10:08:30.8 30 31 61 179 0.282 0.174NETHERLANDSAmsterdam 52°22'N 004°54'E 2 08:36:13.6 341 17 39 — — 10:16:11.4 66 88 51 09:25:23.8 24 54 46 128 0.257 0.152NORWAYOslo 59°55'N 010°45'E 94 08:33:09.1 324 350 38 — — 10:36:04.7 84 93 47 09:33:55.4 24 43 44 143 0.495 0.390POLANDGdansk 54°23'N 018°40'E 11 08:45:55.6 334 360 46 — — 10:44:58.0 79 80 53 09:45:10.5 26 42 51 154 0.386 0.273Katowice 50°16'N 019°00'E — 08:54:30.6 343 12 50 — — 10:42:14.0 71 74 58 09:48:11.8 27 45 55 153 0.274 0.167Krakow 50°03'N 019°58'E 220 08:55:58.4 343 12 51 — — 10:44:12.9 72 72 58 09:49:58.8 27 44 56 156 0.276 0.169Lodz 51°46'N 019°30'E — 08:51:31.7 339 7 49 — — 10:44:46.8 75 76 56 09:47:58.6 27 43 54 155 0.320 0.209Poznan 52°25'N 016°55'E — 08:47:42.1 339 8 47 — — 10:40:03.2 74 79 55 09:43:32.4 26 45 52 150 0.319 0.208Warsaw 52°15'N 021°00'E 90 08:51:58.8 338 4 49 — — 10:48:11.8 77 75 56 09:49:59.6 27 41 54 158 0.345 0.233Wroclaw 51°06'N 017°00'E 147 08:50:34.9 342 12 48 — — 10:38:45.0 71 77 57 09:44:21.7 27 46 54 149 0.283 0.175ROMANIABucharest 44°26'N 026°06'E 82 09:19:39.2 354 17 60 — — 10:54:03.0 66 53 63 10:07:11.2 30 36 63 172 0.184 0.093SERBIA AND MONTENEGROBeograd 44°50'N 020°30'E 138 09:14:35.9 358 28 57 — — 10:36:56.6 59 62 63 09:55:47.4 29 47 61 155 0.134 0.059SLOVAKIABratislava 48°09'N 017°07'E — 08:58:50.3 350 22 51 — — 10:34:24.7 65 72 59 09:46:24.8 27 49 56 148 0.200 0.105SLOVENIALjubljana 46°03'N 014°31'E — 09:04:54.9 358 34 52 — — 10:21:23.3 56 72 60 09:42:56.5 27 55 57 141 0.118 0.048SWEDENGoteborg 57°43'N 011°58'E 17 08:35:43.3 328 355 40 — — 10:36:08.5 81 90 49 09:35:17.1 25 44 46 144 0.440 0.330Stockholm 59°20'N 018°03'E 45 08:39:38.4 324 347 42 — — 10:45:52.4 86 88 49 09:42:24.6 25 39 47 155 0.514 0.411SWITZERLANDBasel 47°33'N 007°35'E — 08:52:20.7 356 35 45 — — 10:07:26.4 54 81 55 09:29:28.3 25 59 51 128 0.122 0.051Bern 46°57'N 007°26'E 572 08:54:49.1 358 38 46 — — 10:04:27.0 51 80 55 09:29:16.2 25 60 51 127 0.103 0.039Zurich 47°23'N 008°32'E 493 08:53:54.7 356 35 46 — — 10:09:14.5 54 80 56 09:31:10.8 25 58 52 130 0.121 0.050UKRAINEChar'kov 50°00'N 036°15'E — 09:11:28.6 334 343 57 — — 11:17:47.2 86 60 53 10:15:41.8 30 20 57 195 0.439 0.329Dnepropetrovsk 48°27'N 034°59'E 79 09:13:59.9 338 348 59 — — 11:16:27.7 83 57 54 10:16:14.3 30 21 59 194 0.389 0.277Doneck 48°00'N 037°48'E — 09:17:41.6 337 343 60 — — 11:22:02.6 85 55 53 10:21:06.5 31 16 58 201 0.413 0.302Horlivka 48°18'N 038°03'E — 09:17:10.3 336 342 59 — — 11:22:15.6 85 55 52 10:20:58.0 31 16 58 201 0.423 0.312Kharkov 50°00'N 036°15'E — 09:11:28.6 334 343 57 — — 11:17:47.2 86 60 53 10:15:41.8 30 20 57 195 0.439 0.329Kiev 50°26'N 030°31'E — 09:05:03.3 337 354 55 — — 11:06:58.2 82 64 55 10:06:37.7 29 29 57 181 0.386 0.273Kramatorsk 48°43'N 037°32'E — 09:15:40.8 336 342 59 — — 11:21:00.8 85 57 53 10:19:32.8 31 17 58 200 0.425 0.315Krivoj Rog 47°55'N 033°21'E — 09:13:54.6 340 353 59 — — 11:13:26.0 80 56 56 10:14:33.6 30 23 60 190 0.357 0.245Lugansk 48°34'N 039°20'E — 09:17:42.0 335 338 59 — — 11:24:16.0 87 56 51 10:22:19.4 31 14 57 204 0.444 0.335L'vov 49°50'N 024°00'E 298 09:00:19.7 342 6 53 — — 10:53:13.2 75 68 58 09:56:55.3 28 38 57 165 0.306 0.195Mariupol' 47°06'N 037°33'E — 09:19:48.0 339 344 61 — — 11:22:13.9 83 52 54 10:22:15.4 31 16 59 202 0.390 0.278Nikolajev 46°58'N 032°00'E — 09:15:22.7 343 358 60 — — 11:10:44.8 78 54 57 10:13:51.3 31 25 61 188 0.318 0.207Odessa 46°28'N 030°44'E 65 09:15:49.1 345 2 60 — — 11:07:49.0 75 54 58 10:12:30.7 30 27 61 185 0.290 0.182Stachanov 48°34'N 038°40'E — 09:17:05.2 335 340 59 — — 11:23:07.5 86 56 52 10:21:23.7 31 15 58 203 0.436 0.326Zaporozje 47°50'N 035°10'E — 09:15:45.2 339 349 59 — — 11:17:08.9 82 55 55 10:17:29.2 31 20 59 195 0.377 0.264
F. Espenak and J. Anderson

37 

TABLE 13

LOCAL CIRCUMSTANCES FOR RUSSIA

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

RUSSIAAngarsk 52°34'N 103°54'E — 09:55:06.3 289 249 26 — — 11:46:41.5 123 86 9 10:52:31.5 206 167 17 278 0.874 0.849Arkangel'sk 64°30'N 040°25'E 7 08:54:24.3 310 314 43 — — 11:07:58.0 103 89 40 10:01:50.3 27 21 43 192 0.774 0.724Astrachan 46°21'N 048°03'E — 09:30:56.2 331 318 61 — — 11:40:05.9 92 51 46 10:37:30.4 32 0 54 225 0.514 0.411Barnaul 53°22'N 083°45'E — 09:44:57.3 299 264 39 10:47:31.0 129 91 10:49:46.6 287 248 11:48:16.7 117 78 21 10:48:38.9 28 350 30 260 1.038 1.000 0.804 02m16sBelgorod 50°36'N 036°35'E — 09:10:28.0 333 342 57 — — 11:17:54.1 87 61 52 10:15:15.2 30 20 57 195 0.456 0.348Berdsk 54°47'N 083°02'E — 09:41:51.5 298 266 39 10:44:33.0 113 76 10:46:51.9 303 266 11:45:37.1 117 80 21 10:45:42.6 208 171 30 258 1.038 1.000 0.913 02m19sBijsk 52°34'N 085°15'E — 09:47:21.1 299 262 38 10:49:29.0 110 70 10:51:43.7 307 267 11:49:46.5 117 78 19 10:50:36.5 208 169 28 262 1.038 1.000 0.852 02m15sBratsk 56°05'N 101°48'E — 09:48:04.8 288 253 27 — — 11:41:18.5 124 89 12 10:46:15.6 206 170 19 274 0.868 0.841Chabarovsk 48°27'N 135°06'E — 10:00:26.4 279 239 5 — — — 10:33 Set — — 0 298 0.603 0.513Chelyabinsk 55°10'N 061°24'E — 09:24:58.0 311 293 49 — — 11:38:13.7 107 73 35 10:33:33.2 29 0 43 233 0.815 0.776Cita 52°03'N 113°30'E — 09:57:35.3 285 244 19 — — 11:43:55.3 125 89 4 10:52:09.8 205 166 11 285 0.823 0.784Dzerzinsk 56°15'N 043°24'E — 09:06:43.9 320 321 52 — — 11:21:11.8 98 73 45 10:15:12.0 29 15 50 203 0.646 0.565Ekaterinburg 48°05'N 039°40'E 272 09:19:10.5 335 338 60 — — 11:25:16.4 86 55 51 10:23:36.2 31 13 58 206 0.438 0.328Gorno-Altajsk 51°58'N 085°58'E — 09:48:53.9 299 261 37 10:50:50.2 106 65 10:53:02.2 310 270 11:50:51.7 118 77 19 10:51:56.3 208 168 28 264 1.038 1.000 0.786 02m12sIrkutsk 52°16'N 104°20'E 467 09:55:45.4 289 248 25 — — 11:47:03.3 123 86 8 10:53:01.8 206 166 16 278 0.873 0.847Iskitim 54°38'N 083°18'E — 09:42:18.0 298 265 39 10:44:55.9 110 73 10:47:13.6 306 269 11:45:54.7 117 80 21 10:46:04.9 208 171 30 259 1.038 1.000 0.855 02m18sIzevsk 56°51'N 053°14'E — 09:14:53.9 314 305 50 — — 11:29:39.3 104 74 39 10:23:54.1 29 8 46 219 0.755 0.700Jaroslavl' 57°37'N 039°52'E — 09:01:24.8 320 325 50 — — 11:15:31.8 97 76 45 10:09:26.3 28 20 49 196 0.638 0.557Kazan 55°49'N 049°08'E — 09:12:48.1 318 312 52 — — 11:27:43.0 101 72 42 10:21:47.9 29 10 48 214 0.696 0.627Kemerovo 55°20'N 086°05'E — 09:42:37.1 296 263 37 — — 11:44:41.1 119 82 20 10:45:32.9 208 171 28 261 0.987 0.990Kirov 58°38'N 049°42'E — 09:09:00.7 314 309 49 — — 11:23:54.9 103 77 40 10:17:50.2 29 12 46 212 0.749 0.692Kirovograd 57°26'N 060°04'E — 09:19:57.9 310 295 48 — — 11:33:23.3 108 77 35 10:28:26.6 29 4 42 229 0.832 0.797Kogalym 62°02'N 074°30'E — 09:23:30.3 298 278 40 10:27:39.3 155 129 10:29:35.8 259 233 11:30:35.8 116 87 27 10:28:37.6 27 1 34 242 1.039 1.000 0.386 01m56sKosh Agach 50°01'N 088°44'E — 09:54:05.9 298 257 35 10:55:22.4 80 37 10:57:05.6 336 293 11:54:13.0 118 76 16 10:56:14.1 208 165 26 268 1.037 1.000 0.386 01m43sKrasnodar 45°02'N 039°00'E — 09:26:47.7 341 343 63 — — 11:26:29.6 82 46 54 10:28:01.8 32 11 60 209 0.363 0.251Krasnojarsk 56°01'N 092°50'E 152 09:44:46.9 293 258 33 — — 11:43:02.7 121 85 16 10:45:39.7 207 171 24 266 0.929 0.920Kurgan 55°26'N 065°18'E — 09:27:47.4 308 287 48 — — 11:39:49.3 110 74 32 10:35:47.9 29 359 41 238 0.859 0.831Langepas 61°10'N 075°23'E — 09:25:31.3 298 277 40 10:29:38.3 155 128 10:31:35.3 260 233 11:32:26.2 116 86 27 10:30:36.9 27 0 34 243 1.039 1.000 0.394 01m57sMagnitogorsk 53°27'N 059°04'E — 09:26:00.9 314 296 52 — — 11:39:46.6 105 69 36 10:34:55.4 30 360 45 232 0.767 0.715Megion 61°03'N 076°06'E — 09:26:11.6 298 276 40 10:30:00.6 139 111 10:32:16.9 276 248 11:32:48.9 117 86 26 10:31:08.9 27 360 33 244 1.039 1.000 0.634 02m16sMoscow 55°45'N 037°35'E 154 09:01:57.8 324 331 52 — — 11:14:44.2 93 73 48 10:09:16.5 29 21 52 193 0.578 0.485Muravlenko 63°47'N 073°30'E — 09:20:02.4 297 280 39 10:23:48.8 134 111 10:26:09.5 279 256 11:27:02.0 116 90 28 10:24:59.3 27 3 34 239 1.039 1.000 0.700 02m21sNabereznyje Cel... 55°42'N 052°19'E — 09:15:56.4 316 307 51 — — 11:30:46.1 103 72 40 10:25:01.6 29 7 47 219 0.728 0.666Nadym 65°35'N 072°42'E — 09:16:45.6 297 281 38 10:20:11.9 110 89 10:22:37.8 303 282 11:23:25.7 116 92 28 10:21:24.9 207 185 33 236 1.039 1.000 0.886 02m26sGorki 56°20'N 044°00'E — 09:07:10.2 320 320 52 — — 11:21:44.8 98 73 44 10:15:43.2 29 15 50 204 0.653 0.575Niznevartovsk 60°56'N 076°31'E — 09:26:39.8 298 276 40 10:30:21.7 131 104 10:32:43.4 283 256 11:33:07.3 117 86 26 10:31:32.6 27 360 33 245 1.039 1.000 0.757 02m22sNiznij Tagil 57°55'N 059°57'E — 09:19:04.8 309 295 48 — — 11:32:27.5 108 77 35 10:27:30.0 29 4 42 228 0.837 0.803Novoaltajsk 53°24'N 083°58'E — 09:45:01.3 299 264 38 10:47:30.1 123 84 10:49:47.7 293 255 11:48:13.4 117 78 21 10:48:39.0 28 350 29 260 1.038 1.000 0.920 02m18sNovokuzneck 53°45'N 087°06'E — 09:46:09.0 297 261 36 — — 11:47:35.2 119 80 19 10:48:49.5 208 169 27 263 0.990 0.993Novosibirsk 55°02'N 082°55'E — 09:41:19.2 298 266 39 10:44:02.3 110 74 10:46:20.6 306 270 11:45:08.7 117 80 22 10:45:11.6 208 172 30 258 1.038 1.000 0.861 02m18sNoyabrsk 63°10'N 075°37'E — 09:22:22.5 297 278 39 10:25:51.1 101 77 10:28:11.6 313 288 11:28:40.4 117 89 27 10:27:01.4 207 182 33 242 1.039 1.000 0.731 02m21sOmsk 55°00'N 073°24'E 85 09:34:56.1 304 276 44 — — 11:43:39.1 113 77 27 10:41:20.4 29 355 36 248 0.935 0.927Onguday 50°45'N 086°09'E — 09:51:19.5 299 260 37 10:53:12.8 133 92 10:55:22.5 283 241 11:53:03.3 117 76 18 10:54:17.8 28 347 28 265 1.038 1.000 0.737 02m10sOrenburg 51°54'N 055°06'E — 09:25:21.0 319 303 54 — — 11:39:21.8 102 65 39 10:34:22.7 30 1 48 229 0.698 0.630Penza 53°13'N 045°00'E — 09:13:22.4 323 322 55 — — 11:27:02.2 96 66 45 10:21:42.0 30 12 52 210 0.605 0.517Perm 58°00'N 056°15'E — 09:15:45.7 311 300 49 — — 11:29:57.4 106 77 37 10:24:29.7 29 6 44 223 0.802 0.759Prokopjevsk 53°53'N 086°45'E — 09:45:42.4 297 262 37 — — 11:47:21.1 118 80 19 10:48:29.1 208 170 28 262 0.992 0.995R'azan' 54°38'N 039°44'E — 09:05:49.5 324 330 53 — — 11:18:43.3 94 70 48 10:13:23.1 29 18 52 198 0.576 0.483Rostov-na-Donu 47°14'N 039°42'E — 09:21:20.8 337 339 61 — — 11:26:05.0 85 52 52 10:25:07.1 31 12 58 207 0.420 0.309St. Petersburg 59°55'N 030°15'E 5 08:49:51.8 320 334 46 — — 11:01:55.8 94 83 47 09:56:13.4 27 29 48 177 0.607 0.519Samara 53°12'N 050°09'E — 09:18:17.7 320 312 54 — — 11:32:41.7 99 67 42 10:27:14.7 30 7 50 219 0.663 0.586Saratov 51°34'N 046°02'E 60 09:17:30.3 325 321 56 — — 11:30:30.0 95 63 45 10:25:38.7 30 9 52 214 0.586 0.494Strezhevoy 60°44'N 077°35'E — 09:27:42.5 298 275 39 10:31:10.2 111 83 10:33:34.3 304 276 11:33:42.7 117 86 26 10:32:22.3 207 179 33 246 1.039 1.000 0.885 02m24sToljatti 53°31'N 049°26'E — 09:17:02.5 320 313 54 — — 11:31:29.5 99 67 42 10:25:57.9 30 8 50 217 0.660 0.583Tomsk 56°30'N 084°58'E — 09:39:49.0 296 265 37 — — 11:42:29.8 119 83 21 10:43:00.6 208 173 29 258 0.988 0.991T'umen' 57°09'N 065°32'E — 09:24:59.5 307 287 46 — — 11:36:46.0 111 77 32 10:32:45.1 29 0 40 236 0.882 0.860Ufa 54°44'N 055°56'E 174 09:20:53.4 315 301 51 — — 11:35:17.7 104 71 38 10:29:57.1 30 4 46 226 0.751 0.695Ulan-Ude 51°50'N 107°37'E — 09:57:13.3 287 247 23 — — 11:46:37.9 124 86 7 10:53:28.9 206 166 14 281 0.856 0.826Uljanovsk 54°20'N 048°24'E — 09:14:36.9 320 315 53 — — 11:29:13.0 99 69 43 10:23:31.0 30 9 50 214 0.663 0.586Vladimir 56°10'N 040°25'E — 09:04:01.9 322 326 52 — — 11:17:50.9 96 73 46 10:12:00.8 29 18 51 198 0.614 0.528Vladivostok 43°10'N 131°56'E 29 10:08:47.2 283 237 4 — — — 10:31 Set — — 0 295 0.424 0.312Volgograd 48°44'N 044°25'E — 09:22:00.5 331 326 59 — — 11:32:01.0 91 56 48 10:28:41.7 31 8 55 215 0.512 0.409Vologda 59°12'N 039°55'E — 08:59:23.7 317 323 48 — — 11:13:45.4 98 79 44 10:07:27.9 28 20 48 195 0.670 0.595Voronez 51°40'N 039°10'E — 09:10:43.3 329 335 56 — — 11:21:02.9 90 63 50 10:17:05.8 30 17 55 200 0.508 0.405
Total Solar Eclipse of 2008 August 01

38

TABLE 14

LOCAL CIRCUMSTANCES FOR ASIA MINOR

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

ARMENIAJerevan 40°11'N 044°30'E — 09:45:46.3 345 327 66 — — 11:41:09.8 82 34 50 10:45:15.9 33 355 59 230 0.341 0.229AZERBAIJANBaku 40°23'N 049°51'E — 09:48:28.2 339 311 64 — — 11:50:10.1 87 37 45 10:51:30.1 33 350 55 239 0.428 0.317BAHRAINAl-Manamah 26°13'N 050°35'E — 10:40:19.9 3 295 62 — — 12:00:57.6 68 357 44 11:21:51.9 36 325 53 265 0.164 0.078GEORGIATbilisi 41°43'N 044°49'E — 09:41:05.0 342 327 65 — — 11:40:23.2 84 38 50 10:42:34.8 33 357 59 228 0.377 0.265IRANBakhtaran 34°19'N 047°04'E 1320 10:07:38.4 353 312 67 — — 11:50:40.3 77 18 48 11:00:53.4 35 341 58 247 0.265 0.159Esfahan 32°40'N 051°38'E 1597 10:14:18.5 349 298 64 — — 12:00:48.6 80 18 43 11:09:34.1 35 335 53 255 0.311 0.200Mashhad 36°18'N 059°36'E — 10:06:09.3 334 285 58 — — 12:07:24.0 92 34 35 11:09:21.9 33 337 46 258 0.505 0.402Qom 34°39'N 050°54'E — 10:07:14.7 347 302 65 — — 11:57:50.6 82 23 44 11:04:37.2 34 339 54 251 0.336 0.224Tabriz 38°05'N 046°18'E — 09:53:45.2 347 319 67 — — 11:46:25.4 81 29 49 10:51:58.1 34 349 58 238 0.327 0.216Tehran 35°40'N 051°26'E 1200 10:04:01.1 344 302 64 — — 11:57:47.7 84 26 43 11:03:04.4 34 341 54 250 0.364 0.252IRAQBasrah 30°30'N 047°50'E — 10:23:04.7 359 305 66 — — 11:53:52.6 72 7 48 11:09:55.4 35 334 57 255 0.201 0.106Mosul 36°20'N 043°08'E 223 09:59:16.2 354 328 69 — — 11:40:31.1 74 21 53 10:51:23.5 34 350 62 236 0.240 0.137Baghdad 33°21'N 044°25'E 34 10:11:45.6 359 319 69 — — 11:44:33.0 71 13 52 10:59:31.7 35 342 61 245 0.199 0.105ISRAELHaifa 32°49'N 034°59'E — 10:28:29.1 23 352 72 — — 11:02:57.6 47 1 67 10:45:49.1 35 356 70 225 0.022 0.004JORDAN'Amman 31°57'N 035°56'E 776 10:33:43.5 24 347 72 — — 11:04:58.6 46 357 67 10:49:25.1 35 351 69 231 0.018 0.003KUWAITKuwait City 29°20'N 047°59'E 5 10:28:07.9 1 303 66 — — 11:54:22.3 70 4 47 11:12:34.6 36 332 56 258 0.180 0.090LEBANONBeirut 33°53'N 035°30'E — 10:16:56.9 16 352 72 — — 11:11:16.1 54 7 65 10:44:27.0 35 357 69 224 0.056 0.016OMANMasqat 23°37'N 058°35'E — 10:46:09.7 354 280 54 — — 12:17:35.1 75 2 33 11:33:33.6 35 320 43 273 0.253 0.149SAUDI ARABIARiyadh 24°38'N 046°43'E 591 10:55:04.9 17 306 62 — — 11:46:08.3 56 343 51 11:21:01.6 36 324 56 265 0.059 0.017SYRIADamascus 33°30'N 036°18'E 720 10:18:08.6 15 348 72 — — 11:14:28.5 55 6 64 10:46:41.7 35 354 69 227 0.060 0.018Halab 36°12'N 037°10'E 390 10:00:32.8 4 349 71 — — 11:22:39.5 64 18 60 10:42:26.6 34 359 67 222 0.137 0.061TURKEYAdana 37°01'N 035°18'E 25 09:57:00.7 5 357 71 — — 11:16:35.5 63 21 62 10:37:31.3 34 5 68 215 0.126 0.053Ankara 39°56'N 032°52'E 861 09:42:22.9 360 6 68 — — 11:10:57.3 65 32 62 10:27:23.1 33 17 67 200 0.158 0.075Antalya 36°53'N 030°43'E — 10:02:27.3 15 15 71 — — 10:55:18.7 52 23 68 10:29:07.2 33 18 70 198 0.050 0.014Bursa 40°11'N 029°04'E — 09:41:14.4 5 19 67 — — 10:57:21.2 59 37 65 10:19:41.9 32 27 68 186 0.110 0.044Gaziantep 37°05'N 037°22'E — 09:56:01.6 1 349 70 — — 11:23:57.2 67 21 60 10:40:56.4 34 1 66 221 0.161 0.076Istanbul 41°01'N 028°58'E 18 09:36:39.5 2 18 66 — — 10:58:34.0 62 40 65 10:18:03.3 32 28 67 185 0.130 0.056Izmir 38°25'N 027°09'E 28 09:55:43.5 16 28 69 — — 10:41:49.4 48 35 69 10:18:54.0 32 31 69 181 0.037 0.009Konya 37°52'N 032°31'E — 09:53:35.4 7 8 70 — — 11:06:48.3 59 25 65 10:30:42.9 33 14 69 203 0.102 0.039UNITED ARAB EMIRATESAbu Dhabi 24°28'N 054°22'E — 10:45:02.7 360 287 58 — — 12:09:45.4 71 358 38 11:28:48.5 35 322 48 270 0.197 0.103Dubai 25°16'N 055°20'E — 10:41:18.0 357 286 58 — — 12:11:31.9 74 2 37 11:28:01.1 35 323 47 269 0.230 0.129
F. Espenak and J. Anderson

39 

TABLE 15

LOCAL CIRCUMSTANCES FOR ASIA

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 10:16:00.8 326 269 49 — — 12:16:43.1 98 38 25 11:19:04.6 32 332 37 267 0.616 0.530BANGLADESHChittagong 22°20'N 091°50'E — 10:48:15.3 320 247 23 — — — 11:42:11.1 28 319 11 285 0.666 0.588Dacca 23°43'N 090°25'E — 10:45:36.7 319 248 25 — — 12:31:10.8 98 33 2 11:40:31.3 29 320 12 284 0.679 0.605Khulna 22°48'N 089°33'E — 10:47:26.3 321 248 25 — — 12:32:12.6 97 30 2 11:41:56.1 29 319 13 284 0.653 0.573Rajshahi 24°22'N 088°36'E — 10:44:17.8 320 249 27 — — 12:30:58.9 98 33 3 11:39:49.6 29 320 14 283 0.674 0.598BHUTANThimbu 27°28'N 089°39'E — 10:38:13.1 316 248 28 — — 12:27:34.3 102 39 4 11:35:08.9 29 323 15 283 0.741 0.681INDIAAhmadabad 23°02'N 072°37'E 55 10:46:22.3 337 262 41 — — 12:30:50.9 88 17 17 11:40:50.6 32 319 28 279 0.459 0.350Bangalore 12°59'N 077°35'E 895 11:12:20.6 346 262 28 — — 12:36:58.3 76 357 8 11:56:07.1 31 309 18 285 0.311 0.200Bombay 18°58'N 072°50'E 8 10:57:20.4 342 263 37 — — 12:33:28.7 82 8 15 11:47:19.3 32 315 26 281 0.380 0.267Calcutta 22°32'N 088°22'E 6 10:48:00.0 322 249 26 — — 12:32:41.3 96 29 3 11:42:28.0 29 319 14 284 0.636 0.553Delhi 28°40'N 077°13'E — 10:33:13.3 325 258 40 — — 12:26:42.2 97 33 15 11:32:29.2 31 325 27 277 0.624 0.538Hyderabad 17°23'N 078°29'E 531 11:00:26.7 338 258 31 — — 12:36:13.5 84 9 9 11:50:12.7 31 313 20 283 0.420 0.308Kanpur 26°28'N 080°21'E — 10:38:57.1 325 255 36 — — 12:29:29.2 97 31 11 11:36:37.6 31 322 23 279 0.623 0.537Lucknow 26°51'N 080°55'E 122 10:38:11.9 324 254 35 — — 12:29:06.7 97 32 11 11:36:04.1 30 323 22 279 0.636 0.553Madras 13°05'N 080°17'E 16 11:10:53.7 343 259 26 — — 12:37:45.3 78 0 6 11:55:51.1 31 310 16 285 0.346 0.234New Delhi 28°36'N 077°12'E 212 10:33:22.4 325 258 40 — — 12:26:46.8 97 33 15 11:32:35.9 31 325 27 277 0.622 0.537Pune 18°32'N 073°52'E — 10:58:19.9 342 262 36 — — 12:34:09.9 82 8 14 11:48:08.9 32 314 25 282 0.385 0.272KAZAKHSTANAlma-Ata 43°15'N 076°57'E 775 10:00:46.3 311 265 44 — — 12:05:36.0 109 59 22 11:05:44.7 30 340 33 264 0.840 0.806Karaganda 49°50'N 073°10'E — 09:44:38.2 308 273 46 — — 11:53:09.2 111 68 26 10:51:14.5 30 349 36 254 0.877 0.854KYRGYZSTANBishkek (Frunze) 42°54'N 074°36'E — 09:59:59.8 313 267 46 — — 12:05:41.4 108 57 23 11:05:26.9 31 341 34 263 0.808 0.766LAOSVientiane 17°58'N 102°36'E 170 10:54:08.2 318 244 10 — — — 11:41 Set — — 0 289 0.657 0.577MACAUMacau 22°14'N 113°35'E — 10:43:48.1 307 239 4 — — — 11:04 Set — — 0 289 0.374 0.261MONGOLIADarchan 49°29'N 105°55'E — 10:01:04.9 289 246 23 — — 11:51:02.3 123 83 6 10:57:42.8 206 164 14 281 0.882 0.859Hovd 48°08'N 091°23'E — 09:58:56.9 298 254 33 10:59:48.0 47 2 11:00:29.2 9 324 11:57:11.3 118 74 14 11:00:08.7 208 163 23 271 1.036 1.000 0.055 00m41sOlgij 48°56'N 089°57'E — 09:56:45.8 298 256 35 10:57:39.9 76 32 10:59:15.9 340 296 11:55:59.7 118 75 15 10:58:28.0 208 164 24 269 1.037 1.000 0.334 01m36sUlaanbaatar 47°55'N 106°53'E 1307 10:04:00.9 289 245 22 — — 11:53:08.8 122 81 5 11:00:14.4 206 162 13 282 0.888 0.867NEPALKathmandu 27°43'N 085°19'E 1348 10:37:07.4 319 251 32 — — 12:28:02.0 100 37 8 11:34:56.4 30 323 19 281 0.701 0.632NORTH KOREAP'yongyang 39°01'N 125°45'E 29 10:16:29.1 287 237 5 — — — 10:46 Set — — 0 294 0.564 0.467PAKISTANIslamabad 33°42'N 073°10'E — 10:19:54.8 324 264 46 — — 12:19:23.2 100 40 21 11:22:20.0 32 330 33 271 0.656 0.577Karachi 24°52'N 067°03'E 4 10:41:03.7 341 268 47 — — 12:26:10.1 86 16 23 11:35:51.8 33 321 35 275 0.414 0.302Lahore 31°35'N 074°18'E — 10:25:24.6 325 261 44 — — 12:22:30.8 98 36 19 11:26:35.8 32 328 31 273 0.636 0.553SOUTH KOREASeoul 37°33'N 126°58'E 10 10:18:04.2 288 236 3 — — — 10:37 Set — — 0 293 0.381 0.268SRI LANKAColombo 06°56'N 079°51'E 7 11:28:40.6 355 266 21 — — 12:35:38.6 66 341 5 12:03:01.6 30 304 13 287 0.194 0.101TAJIKISTANDusanbe 38°35'N 068°48'E — 10:05:55.6 322 272 51 — — 12:10:35.3 101 46 27 11:10:59.1 32 337 38 263 0.674 0.599TURKMENISTANAschabad 37°57'N 058°23'E — 10:00:53.4 333 289 59 — — 12:03:58.9 93 37 36 11:05:00.4 33 340 47 254 0.515 0.413UZBEKISTANTaskent 41°20'N 069°18'E — 09:59:52.1 319 273 50 — — 12:06:29.0 103 51 27 11:05:51.9 31 340 38 260 0.721 0.657
Total Solar Eclipse of 2008 August 01

40

TABLE 16

LOCAL CIRCUMSTANCES FOR CHINA

TOTAL SOLAR ECLIPSE OF 2008 AUGUST 01

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 ° ° ° °

CHINAAltay 47°52'N 088°07'E — 09:57:54.6 300 256 36 10:59:25.9 167 122 11:00:51.0 249 204 11:58:02.2 117 72 16 11:00:08.5 28 343 25 269 1.037 1.000 0.242 01m25sAnshan 41°08'N 122°59'E — 10:14:15.1 287 237 8 — — — 11:02 Set — — 0 294 0.854 0.822Baiyin 36°47'N 104°07'E — 10:22:45.7 298 242 20 11:17:59.4 159 105 11:19:14.2 254 200 — 11:18:36.9 26 332 9 286 1.032 1.000 0.325 01m15sBaotou 40°40'N 109°59'E — 10:16:29.9 292 240 17 — — — 11:11:09.2 206 156 7 288 0.941 0.933Beijing 39°55'N 116°25'E — 10:17:15.1 290 238 12 — — — 11:10:02.7 205 156 3 291 0.916 0.901Binxian 35°00'N 108°08'E — 10:25:40.8 298 240 16 11:19:28.8 155 100 11:20:42.8 257 202 — 11:20:05.9 26 331 5 288 1.031 1.000 0.371 01m14sChangsha 28°12'N 112°58'E 49 10:35:20.0 301 238 8 — — — 11:16 Set — — 0 291 0.768 0.713Chengdu 30°39'N 104°04'E — 10:32:57.1 303 241 17 — — — 11:27:34.2 26 327 6 288 0.913 0.898Chongqing 29°34'N 106°35'E 261 10:34:28.4 303 240 14 — — — 11:28:10.9 26 326 3 289 0.912 0.896Datong 46°03'N 124°50'E — 10:06:37.7 283 239 10 — — — 10:57:48.7 204 162 2 295 0.819 0.778Fushun 41°52'N 123°53'E — 10:12:58.9 286 237 8 — — — 11:00 Set — — 0 295 0.840 0.804Guangzhou 23°06'N 113°16'E 18 10:42:39.9 307 239 5 — — — 11:06 Set — — 0 290 0.445 0.334Guiyang 26°35'N 106°43'E — 10:39:10.3 306 240 12 — — — 11:32:01.1 26 324 1 290 0.860 0.830Hami 42°48'N 093°27'E — 10:09:51.6 300 249 31 — — 12:05:37.4 116 68 10 11:09:53.6 28 338 20 276 0.998 0.999Handan 36°37'N 114°29'E — 10:22:31.6 293 238 12 — — — 11:15:27.6 205 153 2 291 0.967 0.966Hangzhou 30°15'N 120°10'E — 10:30:15.4 296 237 4 — — — 10:50 Set — — 0 291 0.397 0.284Harbin 45°45'N 126°41'E 145 10:06:40.8 283 238 8 — — — 10:57:24.6 203 162 0 296 0.816 0.774Heze 35°17'N 115°27'E — 10:24:21.7 294 238 10 — — — 11:16:52.2 205 152 1 292 0.981 0.982Huainan 32°40'N 117°00'E — 10:27:50.0 295 237 8 — — — 11:08 Set — — 0 292 0.773 0.719Jilin 43°51'N 126°33'E — 10:09:28.2 284 238 7 — — — 10:54 Set — — 0 295 0.797 0.750Jinan 36°40'N 116°57'E — 10:22:02.1 292 238 10 — — — 11:14:20.2 205 153 1 293 0.955 0.950Jiuquan 39°45'N 098°34'E — 10:16:53.3 299 245 26 11:14:18.5 169 116 11:15:27.0 245 193 12:08:48.0 115 66 5 11:14:52.9 27 335 15 281 1.034 1.000 0.214 01m08sKunming 25°05'N 102°40'E 1893 10:42:16.7 310 242 15 — — — 11:35:31.4 27 322 3 288 0.806 0.762Laiwu 36°12'N 117°42'E — 10:22:34.1 292 237 9 — — — 11:12 Set — — 0 293 0.933 0.922Lanzhou 36°03'N 103°41'E 1556 10:23:59.2 299 242 20 — — — 11:19:50.5 27 332 9 286 0.993 0.995Lüda 38°53'N 121°35'E — 10:17:49.0 289 237 8 — — — 11:02 Set — — 0 293 0.833 0.795Luohe 33°35'N 114°01'E — 10:27:09.2 296 238 10 11:19:03.2 107 52 11:20:30.1 303 248 — 11:19:46.8 205 150 1 292 1.029 1.000 0.862 01m27sLuoyang 34°41'N 112°28'E — 10:25:45.0 296 238 12 11:18:24.3 71 17 11:19:29.3 339 285 — 11:18:56.9 205 151 2 291 1.030 1.000 0.307 01m05sNanjing 32°03'N 118°47'E — 10:28:13.0 295 237 6 — — — 10:59 Set — — 0 291 0.607 0.517Nanyang 33°00'N 112°32'E — 10:28:17.5 297 238 11 11:21:02.7 193 138 11:21:21.3 217 162 — 11:21:12.1 25 330 1 291 1.029 1.000 0.022 00m19sPingdingshan 33°45'N 113°17'E — 10:27:02.1 296 238 11 11:19:08.2 112 57 11:20:36.7 298 244 — 11:19:52.5 205 150 1 291 1.029 1.000 0.944 01m28sPingliang 35°27'N 107°10'E — 10:24:59.8 298 240 17 11:19:06.5 152 98 11:20:24.3 259 205 — 11:19:45.5 26 331 6 288 1.031 1.000 0.405 01m18sPingxiang 27°38'N 113°50'E — 10:35:55.5 301 238 7 — — — 11:11 Set — — 0 290 0.676 0.600Puyang 35°42'N 114°59'E — 10:23:49.5 294 238 11 — — — 11:16:30.6 205 152 1 292 0.977 0.978Qingdao 36°06'N 120°19'E — 10:22:05.8 291 237 7 — — — 11:01 Set — — 0 293 0.754 0.697Qiqihar 47°19'N 123°55'E — 10:04:52.5 283 239 11 — — — 10:56:22.4 204 163 3 294 0.812 0.769Sanmenxia 34°45'N 111°05'E — 10:25:49.4 296 239 13 11:18:39.5 101 46 11:20:08.2 310 256 — 11:19:24.0 205 151 3 290 1.030 1.000 0.746 01m29sShanghai 31°14'N 121°28'E 5 10:28:28.1 295 237 4 — — — 10:47 Set — — 0 291 0.366 0.252Shenyang 41°48'N 123°27'E 42 10:13:10.8 286 238 8 — — — 11:01 Set — — 0 295 0.853 0.821Shijiazhuang 38°03'N 114°28'E — 10:20:20.9 292 238 13 — — — 11:13:27.7 205 154 3 291 0.949 0.942Suining 30°31'N 105°34'E — 10:33:03.5 303 240 15 — — — 11:27:15.4 26 327 4 288 0.921 0.907Tai'an 36°12'N 117°07'E — 10:22:41.3 293 237 10 — — — 11:14 Set — — 0 293 0.958 0.954Taiyuan 37°55'N 112°30'E — 10:20:45.9 293 239 14 — — — 11:14:23.7 205 154 4 290 0.960 0.957Tangshan 39°38'N 118°11'E — 10:17:24.9 290 238 11 — — — 11:09:43.1 204 156 1 293 0.912 0.895Tianjin 39°08'N 117°12'E 4 10:18:19.4 290 238 11 — — — 11:10:49.9 205 155 2 292 0.922 0.909Tongchuan 35°01'N 109°01'E — 10:25:35.9 297 239 15 11:19:01.1 131 77 11:20:31.8 280 225 — 11:19:46.5 26 331 5 289 1.030 1.000 0.729 01m31sUrumqi 43°48'N 087°35'E 906 10:05:32.8 303 254 36 — — 12:04:59.5 114 66 14 11:07:34.1 29 339 25 272 0.957 0.954Weifang 36°42'N 119°04'E — 10:21:32.6 291 237 8 — — — 11:07 Set — — 0 293 0.875 0.848Weinan 34°29'N 109°29'E — 10:26:24.1 297 239 14 11:19:44.5 152 97 11:20:59.1 259 204 — 11:20:21.9 26 331 4 289 1.030 1.000 0.400 01m15sWuhan 30°36'N 114°17'E 23 10:31:29.6 298 238 9 — — — 11:15 Set — — 0 291 0.831 0.793Xi'an (Sian) 34°15'N 108°52'E — 10:26:49.4 298 239 15 — — — 11:20:54.8 26 330 4 289 0.999 1.000Xianyang 34°22'N 108°42'E — 10:26:39.1 298 239 15 — — — 11:20:48.4 26 330 4 289 1.000 1.000Xiaogan 30°55'N 113°54'E — 10:31:07.2 298 238 9 — — — 11:17 Set — — 0 291 0.877 0.851Xintai 35°54'N 117°44'E — 10:22:59.9 293 237 9 — — — 11:11 Set — — 0 292 0.917 0.903Xuchang 34°03'N 113°49'E — 10:26:29.6 296 238 11 11:18:37.4 82 28 11:19:51.5 328 274 — 11:19:14.6 205 151 1 291 1.029 1.000 0.456 01m14sYancheng 33°24'N 120°09'E — 10:25:55.8 294 237 6 — — — 10:56 Set — — 0 292 0.595 0.503Yiwu 43°15'N 094°45'E — 10:09:27.6 299 249 30 11:08:09.6 129 80 11:10:05.7 286 236 12:04:35.5 117 69 9 11:09:07.8 28 338 19 277 1.035 1.000 0.797 01m56sYulin 22°36'N 110°07'E — 10:44:27.4 309 240 7 — — — 11:18 Set — — 0 290 0.611 0.522Yumen 39°56'N 097°51'E — 10:16:24.3 299 246 26 11:14:28.3 196 144 11:14:49.4 218 166 12:08:46.6 115 66 5 11:14:38.9 27 335 15 281 1.034 1.000 0.018 00m21sYuncheng 35°00'N 110°59'E — 10:25:26.9 296 239 14 11:18:24.2 88 34 11:19:46.2 323 268 — 11:19:05.3 205 151 3 290 1.030 1.000 0.545 01m22sZaozhuang 34°53'N 117°34'E — 10:24:30.5 293 237 9 — — — 11:10 Set — — 0 292 0.872 0.844Zhangye 38°56'N 100°27'E — 10:18:40.9 299 244 24 11:15:12.8 150 97 11:16:43.3 264 211 12:09:17.3 115 65 3 11:15:58.2 27 334 13 283 1.033 1.000 0.457 01m30sZhengzhou 34°48'N 113°39'E — 10:25:23.7 295 238 11 — — — 11:18:18.0 205 151 1 291 0.997 0.998Zhumadian 32°58'N 114°03'E — 10:28:03.8 296 238 10 — — — 11:20 Set — — 0 292 0.999 1.000Zibo 36°47'N 118°01'E — 10:21:39.1 292 237 9 — — — 11:12 Set — — 0 293 0.937 0.927
F. Espenak and J. Anderson

41 

TABLE 17

SOLAR ECLIPSES OF SAROS SERIES 126

First Eclipse: 1179 Mar 10 Duration of Series: 1280.1 yrs.

Last Eclipse: 2459 May 03 Number of Eclipses: 72

Saros Summary: Partial: 31 Annular: 28 Total: 10 Hybrid: 3

___________________________________________________________________________________

Eclipse Mag./

Date Type Gamma Width Durat.

1179 Mar 10 Pb -1.5347 0.0551

1197 Mar 20 P -1.4871 0.1342

1215 Mar 31 P -1.4336 0.2236

1233 Apr 11 P -1.3709 0.3292

1251 Apr 22 P -1.3034 0.4436

1269 May 02 P -1.2283 0.5712

1287 May 14 P -1.1492 0.7065

1305 May 24 P -1.0651 0.8508

1323 Jun 04 As -0.9793 - 05m59s

1341 Jun 14 A -0.8916 464 06m25s

1359 Jun 26 A -0.8033 330 06m30s

1377 Jul 06 A -0.7162 269 06m24s

1395 Jul 17 A -0.6311 234 06m12s

1413 Jul 27 A -0.5499 213 05m58s

1431 Aug 08 A -0.4732 201 05m45s

1449 Aug 18 A -0.4025 194 05m35s

1467 Aug 29 A -0.3385 191 05m29s

1485 Sep 09 A -0.2805 190 05m26s

1503 Sep 20 A -0.2309 190 05m27s

1521 Sep 30 A -0.1887 191 05m30s

1539 Oct 12 A -0.1546 192 05m35s

1557 Oct 22 A -0.1261 192 05m40s

1575 Nov 02 A -0.1056 191 05m44s

1593 Nov 22 A -0.0901 189 05m47s

1611 Dec 04 A -0.0799 185 05m45s

1629 Dec 14 A -0.0721 179 05m38s

1647 Dec 26 A -0.0671 170 05m26s

1666 Jan 05 A -0.0620 160 05m07s

1684 Jan 16 A -0.0561 147 04m43s

1702 Jan 28 A -0.0481 132 04m14s

1720 Feb 08 A -0.0372 115 03m40s

1738 Feb 18 A -0.0208 96 03m03s

1756 Mar 01 A 0.0009 76 02m24s

1774 Mar 12 A 0.0287 55 01m43s

1792 Mar 22 A 0.0620 33 01m02s

1810 Apr 04 A 0.1033 12 00m21s

1828 Apr 14 Hm 0.1500 10 00m18s

1846 Apr 25 H 0.2039 31 00m53s

1864 May 06 H 0.2622 52 01m25s

1882 May 17 T 0.3269 72 01m50s

Eclipse Mag./

Date Type Gamma Width Durat.

1900 May 28 T 0.3943 92 02m10s

1918 Jun 08 T 0.4658 112 02m23s

1936 Jun 19 T 0.5389 132 02m31s

1954 Jun 30 T 0.6135 153 02m35s

1972 Jul 10 T 0.6871 175 02m36s

1990 Jul 22 T 0.7595 201 02m33s

2008 Aug 01 T 0.8306 237 02m27s

2026 Aug 12 T 0.8976 294 02m18s

2044 Aug 23 T 0.9612 452 02m04s

2062 Sep 03 P 1.0189 0.9754

2080 Sep 13 P 1.0721 0.8748

2098 Sep 25 P 1.1181 0.7877

2116 Oct 06 P 1.1587 0.7109

2134 Oct 17 P 1.1929 0.6463

2152 Oct 28 P 1.2211 0.5930

2170 Nov 08 P 1.2423 0.5529

2188 Nov 18 P 1.2589 0.5216

2206 Dec 01 P 1.2709 0.4990

2224 Dec 11 P 1.2789 0.4838

2242 Dec 22 P 1.2833 0.4756

2261 Jan 02 P 1.2870 0.4684

2279 Jan 13 P 1.2895 0.4637

2297 Jan 23 P 1.2937 0.4556

2315 Feb 05 P 1.2987 0.4461

2333 Feb 15 P 1.3084 0.4276

2351 Feb 27 P 1.3204 0.4046

2369 Mar 09 P 1.3388 0.3694

2387 Mar 20 P 1.3619 0.3250

2405 Mar 31 P 1.3925 0.2661

2423 Apr 11 P 1.4278 0.1979

2441 Apr 21 P 1.4702 0.1158

2459 May 03 Pe 1.5184 0.0223

_________________________________________________________________________________

Eclipse P - Partial Pb - Partial Eclipse (Saros Series Begins)

Type: A - Annular Pe - Partial Eclipse (Saros Series Ends)

T - Total Hm - Middle eclipse of Saros series

H - Hybrid (Annular/Total) As - Annular Eclipse (no southern limit)

Note: Mag./Width column gives either the eclipse magnitude (for partial eclipses)

or the umbral path width in kilometers (for total and annular eclipses).
Total Solar Eclipse of 2008 August 01

42

Table 18: Cloud Cover Statistics for August along the Eclipse Path

Location

Percent of 

possible

sunshine Clear Scattered Broken Overcast Obscured

Alert* 32 2.3 19.1 31.3 41.1 6.2

Resolute 22 0.8 16.6 27.3 44.2 11

Eureka 32 2.7 19.2 42.3 34.7 1.1

Cambridge Bay 34

Thule 6.3 25.1 31.7 29.9 7.0

Danmarkshavn 13.3 31.8 21 28.8 5.1

Longyearbyen, Spitsbergen 0.2 15.0 54.8 29.0 1.1

Ny-Alesund, Spitsbergen 18 2.7 15.4 35.8 44.7 1.4

Bear Island (Bjornoya) 0.3 11.0 36.4 37.0 15.3

Hopen Island 1 13.2 26.5 40.3 19

Jan Mayen Island 0.2 11.2 34.9 40.9 12.8

Barentsburg, Spitsbergen 3.3 12.4 47.8 35.5 1

Nagurskoye, Franz Josef Land 1.3 8.1 49.7 37.6 3.4

Krenkel Polar, Franz Josef Land 1.7 6.1 53.2 35 4.9

Viktoriya Island, Franz Josef Land* 4.2 4.9 37.9 34.1 19.2

Russkaya Gavan', Novaya Zemlya 6.8 9.1 45.2 36.8 2.1

Belyy Island 5.4 11.2 35.5 41.1 6.8

Malye Karmakuly, Novaya Zemlya 23 7.1 16.3 40.9 33.1 2.7

Novy Port* 4.7 15.9 49.2 29.3 0.9

Vorkuta 3.6 10.7 37.2 48.5 0

Yar Sale* 3 12.7 47.7 36.6 0

Salekhard 35 3.3 12.2 41.5 42.6 0.4

Tarko-Sale 36

Surgut 42

Khanty-Mansiysk 45 3 17.1 48.2 31.7 0

Kolpashevo 43

Tara 49

Barabinsk 52

Novosibirsk* 53 7.2 25 34 33.8 0

Novokuznetsk 7.8 17.9 44.4 30 0

Barnaul* 57

Hovd* 67

Kazakhstan

Leninogorsk 63

Zaysan 70

Semey 68

Urumqi 71 7.4 41 43.1 8.6 0

Altay* 73

Hami* 76

Jiuquan* 67

Yinchuan 66 5.2 45.1 36.8 12.6 0.3

Xi'an* 54 7.1 35.1 32.4 25.2 0.2

Zhengzhou 51

Beijing 54 5.6 34.7 36.8 22.9 0

 * = within the eclipse track

Percent of possible sunshine: the percent of time from sunrise to sunset represented by the hourly sunshine in the previous 

column. This statistic is probably the best for determining the probability of seeing the eclipse. Data from various sources.

Percent frequency of clear, scattered, broken, overcast, and obscured cloud conditions: Clear skies are those with less 

than 1/10th sky cover; scattered, 1-5 tenths; broken, 6-9 tenths; and overcast, 10-tenths. Data are for the time of day closest to 

totality, broken into three-hour intervals (0, 3, 6, 12...). Data from the International Station Meteorological Climate Summary.

Russia

Mongolia

China

Percent Frequency of (cloud cover) at eclipse time

Canada

Greenland

Norway
F. Espenak and J. Anderson

43 

Table 19: Climate Statistics for August along the Eclipse Path

Location

Pcpn

Amount

(mm)

Days with

rain

% obs with

t-storms at

eclipse

time

% obs with

pcpn at

eclipse

time

% obs with

fog

% obs with

smoke or

haze at

eclipse time

% obs with

dust or

sand

% of obs

with

obstructions

to vision

Tmax

(°C)

Tmin

(°C)

Alert* 21.2 10.1 0 21.6 20.7 0 0 21 3 -2

Resolute 34.3 13.4 0 28.7 27.4 0 0 27.4 4 -1

Eureka 14.9 8.2 0 17.1 2.2 0 0 2.2 5 0

Cambridge Bay 26.7 13.1 9 3

Thule 16.7 2 0 20.1 14.9 0.2 0.2 15.2 6 1

Danmarkshavn 1 5 0 20.9 23.6 0 0 23.6

Longyearbyen, Spitsbergen 24.8 0 19.6 5 0 0 5 7 3

Ny-Alesund, Spitsbergen 13.6 0 18.8 3.8 0 0 3.8 6 3

Bear Island (Bjornoya) 36.4 18.6 0 13.5 30.6 0.2 0 30.7 6 4

Hopen Island 20 0 18.1 35.9 0 0 35.9 4 2

Jan Mayen Island 74 0 26.9 25 0 0 25 7 4

Barentsburg, Spitsbergen 21 0 23.1 2.8 0 0 2.8 6 3

Nagurskoye, Franz Josef Land 16 0 18.3 20.2 0 0 22.3 1 -1

Krenkel Polar, Franz Josef Land 23 15 0 21.3 11.1 0 0 12.8 1 -1

Viktoriya Island, Franz Josef Land* 0.2 14.6 38.4 0 0 39.5 1 -1

Russkaya Gavan', Novaya Zemlya 18 0 20.3 9.2 0.4 0 9.8 5 2

Belyy Island 0 15.9 14 0.2 0 14.2 7 2

Malye Karmakuly, Novaya Zemlya 50 9.2 0 10.7 14.5 0 0 14.5 8 5

Novy Port* 0.2 11.6 1.1 1.3 0 2.4 13 8

Vorkuta 0.6 25.6 1.9 0.4 0 2.3 13 6

Yar Sale* 0 13.2 0.4 3 0 3.4 5 2

Salekhard 62 9.6 1 15.4 1 1.2 0 2.4 15 7

Tarko-Sale 64 9.4

Khanty-Mansiysk 66 9.5 1.2 16.1 1.8 4.4 0.2 6.3 19 10

Tara 66 9.5

Barabinsk 53 8.5

Novosibirsk* 60 3.1 15.2 0.8 1.2 0 1.9 22 12

Novokuznetsk 5.3 15.2 0 0 0 0 21 11

Barnaul* 50 8 23 11

Hovd* 23 4 23 10

Leninogorsk 76 9.4

Zaysan 4.3 24

Urumqi 31 6 0.2 9.8 0 0 0.5 0.5 30 18

Altay* 22 4.1 28 15

Hami* 7 1.5 34 19

Jiuquan* 17 3.1 28 14

Yinchuan 52 5.5 2.4 10.1 0 0 1.8 1.8 28 16

Xi'an* 67 6.6 1.4 14.7 9.4 4.5 0.5 14.5 31 21

Zhengzhou 117 7.1 31 22

Beijing 182 9.4 6.8 16 22.7 5.7 0.2 33.3 30 20

* = within the eclipse track

Description of elements:

Tmax, Tmin: average maximum and minimum temperatures. Data from various sources.

Canada

Greenland

Norway

Russia

Table 19: Climatological statistics along the eclipse path. Data are for the time of day closest to totality, broken into three-hour intervals (0, 3, 6, 12...). Data

from the International Station Meteorological Climate Summary (NCDC).

% obs with...: Percent of observations with the indicated element. “Obstructions to vision” includes fog, haze, and blowing snow, dust, or sand. Data are for

the time of day closest to totality, broken into three-hour intervals (0, 3, 6, 12...). Data from the International Station Meteorological Climate Summary

(NCDC).

Mongolia

Kazakhstan

China
Total Solar Eclipse of 2008 August 01

44

TABLE 20

F I E L D O F V I E W A N D S I Z E O F S U N ' S I M A G E

F O R V A R I O U S P H O T O G R A P H I C F O C A L L E N G T H S

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 21

S O L A R E C L I P S E E X P O S U R E G U I D E

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
F. Espenak and J. Anderson

45 

 FIGURES
Total Solar Eclipse of 2008 August 01

46

¬

N

S

W E

sunearth.gsfc.nasa.gov/eclipse/eclipse.html

Total Solar Eclipse of 2008 Aug 01

Equatorial Conjunction = 09:47:21.4 UT J.D. = 2454679.907887

Ecliptic Conjunction = 10:12:33.5 UT J.D. = 2454679.925387

Greatest Eclipse = 10:21:06.8 UT J.D. = 2454679.931329

Eclipse Magnitude = 1.0394 Gamma = 0.8307

Saros Series = 126 Member = 47 of 72

Sun at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 08h47m54.1s

Dec. = +17°51'56.4"

S.D. = 00°15'45.5"

H.P. = 00°00'08.7"

Moon at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 08h49m08.8s

Dec. = +18°38'01.5"

S.D. = 00°16'14.1"

H.P. = 00°59'34.8"

External/Internal

Contacts of Penumbra

P1 = 08:04:06.0 UT

P4 = 12:38:26.1 UT

External/Internal

Contacts of Umbra

U1 = 09:21:07.2 UT

U2 = 09:24:10.2 UT

U3 = 11:18:27.6 UT

U4 = 11:21:25.7 UT

Local Circumstances at Greatest Eclipse

Lat. = 65°39.2'N Sun Alt. = 33.5°

Long. = 072°18.0'E Sun Azm. = 235.2°

Path Width = 236.9 km Duration = 02m27.1s

Ephemeris & Constants

Eph. = DE200/LE200

∆T = 65.3 s

k1 = 0.2725076

k2 = 0.2722810

∆b = 0.0" ∆l = 0.0"

Geocentric Libration

(Optical + Physical)

l = 4.23°

b = -1.03°

c = 14.02°

Brown Lun. No. = 1059 Kilometers

0 1000 2000 3000 4000 5000

09:00

UT

09:30 UT

10:00 UT

10:30 UT

11:00 UT

11:30 UT

12:00 UT

Greatest

Eclipse

Sub Solar

P1

P4

0.20

0.40

0.60

0.80

Path of Total Eclipse

0.80

FIGURE 1: ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH
F. Espenak and J. Anderson

47 

Stereographic Projection

Central Lat,Lng = 60.0 70.0

Semi W,H = 0.55 0.65 Offset X,Y = 0.00-0.00

Scale = 6.00 mm/° = 1:18553000

P Factor = 0.20

2006 Aug 23 11:34:50

WorldMap v2.00, F. Espenak High Res World Data [WPD1]

Kilometers

0 1000 2000 3000

0.10

0.20

0.30

0.40

0.50

0.60

0.70

0.80

0.90

0.90

0.80

12:00 UT

11:30 UT

11:00 UT

10:30 UT

10:00 UT

09:30 UT

09:00 UT

Maximum Eclipse at Sunrise

Maximum Eclipse at Sunset

Southern Limit of Partial Eclipse

Path of Total Eclipse

Eclipse Ends at Sunrise

Eclipse Begins at Sunrise

Eclipse Begins at Sunset

Eclipse Ends at Sunset

FIGURE 2: STEREOGRAPHIC PROJECTION MAP OF THE ECLIPSE

Total Solar Eclipse of 2008 August 01
Total Solar Eclipse of 2008 August 01

48

Equidistant Conic Projection Central Lat,Lng = 78.0 -82.0

Semi W,H = 16.0 12.0 Lat 1,2 = 70.0 85.0

Scale = 28.00 mm/° = 1: 3976000

P Factor = 0.21 2006 Aug 22 15:50:22 High Res World Data [WPD1]

Alert

Arctic

Bay

Bathurst

Inlet

Cambridge

Bay

Clyde

Coppermine Elizabeth

Harbour

Gjoa

Haven

Holman

Island

Igloolik

Pangnirtung

Pond

Inlet

Port

Radium

Rae

Repulse Bay 

Resolute

Sachs

Harbour

Spence

Bay

Yellowknife

09:30 UT

 01m55s

16°

09:40 UT

02m09s

23°

09:25 UT

01m44s

9°

09:35 UT

02m03s

20°

Kilometers

 0 200 400 600 800

NASA 2008 Eclipse Bulletin(F. Espenak & J. Anderson)

FIGURE 3: PATH OF THE ECLIPSE THROUGH CANADA AND GREENLAND

Total Solar Eclipse of 2008 August 0

1

GREENLAND

NUNAVUT

CANADA

Maximum Eclipse at Sunrise

Eclipse Ends at Sunrise

Eclipse Begins at Sunrise

 0.90 

 0.80 

 0.70 

 0.90 

 09:30 UT
F. Espenak and J. Anderson

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Total Solar Eclipse of 2008 August 01

50
F. Espenak and J. Anderson

51 
Total Solar Eclipse of 2008 August 01

52

Equidistant Conic Projection

Central Lat,Lng = 54.0 100.0

Semi W,H = 22.0 29.0 Lat 1,2 = 40.0 70.0

Scale = 16.00 mm/° = 1: 6958000

P Factor = 0.20

 2006 Aug 23 15:39:13 WorldMap v2.00, F. Espenak High Res World Data [WPD1]

Beijing

Chengdu

Chongqing

Harbin

Nanjing

Shanghai

Shenyang

Shuicheng

Tianjin

Wuhan

Xi'an

Zibo

Delhi

Kanpur

Alma-Ata

P'yongyang

Soul

Frunze

Ulaanbaatar

Chelyabinsk

Novosibirsk

Omsk

Perm

T'aipei

Altay

Hami

Urumqui

Bijsk

Jiuquan

Zhangye

Niznevartovsk

FIGURE 7: PATH OF THE ECLIPSE THROUGH ASIA

Total Solar Eclipse of 2008 August 01

10:00 UT

02m23s

31°

10:10 UT

02m26s

33°

10:20 UT

02m27s

33°

10:30 UT

02m26s

33°

10:40 UT

02m23s

32°

10:50 UT

02m17s

29°

11:00 UT

02m09s

25°

11:10 UT

01m57s

18°

11:20 UT

01m28s

0°

Greatest

Eclipse

 0.90 

 0.80 

 0.70 

 0.60 

 0.90 

 0.80 

 10:30 UT 

 10:00 UT 

 11:00 UT 

 11:30 UT 

 Maximum Eclipse at Sunset 

 Eclipse Ends at Sunset 

RUSSIA

MONGOLIA

CHINA

KAZAKHSTAN

Kilometers

 0 200 400 600 800 1000 1200

NASA 2008 Eclipse Bulletin (F. Espenak & J. Anderson)
F. Espenak and J. Anderson

53 
Total Solar Eclipse of 2008 August 01

54
F. Espenak and J. Anderson

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Total Solar Eclipse of 2008 August 01

56
F. Espenak and J. Anderson

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Total Solar Eclipse of 2008 August 01

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F. Espenak and J. Anderson

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Total Solar Eclipse of 2008 August 01

60
F. Espenak and J. Anderson

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N

S

E W

Total Solar Eclipse of 2008 Aug 01

000°

180°

090° 270°

Arc-Seconds

 0 1 2 3 4 5

Seconds

 0 1 2 3 4 5

NASA 2008 Eclipse Bulletin (F. Espenak & J. 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

 -10

Sun at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 08h48m00.0s

 Dec. = +17°51'26.0"

 S.D. = 00°15'45.5"

 H.P. = 00°00'08.7"

Moon at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 08h47m59.5s

 Dec. = +17°51'17.8"

 S.D. = 00°16'20.2"

 H.P. = 00°59'59.9"

Geographic Position

Name = Central Line 11:00:00 UT

Lat. = 48°04'01.3"N

Long. = 089°28'15.2"E

Elev. = 0.0 m

Eclipse Contacts

C1 = 09:58:11.4 UT

C2 = 10:58:55.5 UT

C3 = 11:01:04.3 UT

C4 = 11:57:33.2 UT Local Circumstances at Maximum Eclipse

 Sun Alt. = 24.6° Path Width = 251.6 km

Sun Azm. = 269.8° Duration = 02m08.8s

PA(N.Limit) = 28.1° A.Vel. (M:S) = 0.539"/s

Ephemeris & Constants

Eph. = DE200/LE200

ΔT = 65.3 s

 k1 = 0.2725076

 k2 = 0.2722810

Δb ́ = -0.27" Δl ́ = 0.40"

Topocentric Libration

(Optical + Physical)

l = 3.80°

b = -0.21°

c = 13.93°

C2' = 10:58:53.7 UT ( -1.8s)

C3' = 11:01:01.8 UT ( -2.5s)

Limb Corrected Contacts

Calculated Center of Figure

Moon/Sun Diameter Ratio = 1.0367

Moon North

Northern Limit

Southern Limit

Second

Contact

Third

Contact

Mean Limb

(Center of Mass)

(Center of Figure)

Mean Limb

True Limb

Contact Time 

Correction

Scale

Contact Time 

Correction

Scale

Second Contact

Time Correction Curve 

Third Contact

Time Correction Curve

Zenith

FIGURE 16 - LUNAR LIMB PROFILE FOR AUG 01 AT 11:00 UT
Total Solar Eclipse of 2008 August 01

62
F. Espenak and J. Anderson

63 

 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

FIGURE 18: SPECTRAL RESPONSE OF SOME COMMONLY AVAILABLE SOLAR FILTERS

 3

 4

 5

 6

 7

 8

THOUSAND OAKS BLACK POLYMER
Total Solar Eclipse of 2008 August 01

64

0

5

10

15

20

25

30

35

mm

 Film: 200 mm Digital: 135 mm

FIGURE 19 - 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 SLRs which use a CCD 2/3 the size of 35 mm film. Thus, the same lens produces an 

image 1.5x 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
F. Espenak and J. Anderson

65 

N

S

E W

 2008 Aug 01

GMT = 11:00

Local = 19:00

 LST = 13:39

Central Line 11:00 UT

 Lat = 48°04'N

Long = 089°28'E

Zone = 8.0 hours

Arcturus

Vega

Capella

Procyon Altair

Antares

Spica

Pollux

Deneb

Regulus

Castor

 Mercury

 Venus

 Mars

 Saturn

Sun

The sky during totality as seen from the central line in northern China at 11:00 UT. The most conspicuous planets visible 

during the total eclipse will be Mercury (mv=–1.7) and Venus (mv=–3.8) located 3° and 15° east of the Sun, respectively. 

Saturn (mv=+1.1), and Mars (mv=+1.7) will be more difficult to spot at 28° and 39° east of the Sun. Bright stars, which 

might also be visible, include Procyon (mv=+0.38), Castor (mv=+1.94), Pollux (mv=+1.14), and Regulus (mv=+1.36).

The geocentric ephemeris below [using Bretagnon and Simon, 1986] gives the apparent positions of the naked eye planets 

during the eclipse. Delta is the distance of the planet from Earth (A.U.'s), App. Mag. is the apparent visual magnitude of 

the planet, and Solar Elong gives the elongation or angle between the Sun and planet.

Ephemeris: 2008 Aug 01 11:00 UT Equinox = Mean Date

 App. Apparent Solar

Planet RA Declination Delta Mag. Diameter Phase Elong

arc-sec °

Sun 08h48m00s +17°51'32" 1.01494 -26.7 1891.0 - -

Moon 08h50m41s +18°29'43" 0.00246 - 1947.6 - -

Mercury 09h01m57s +18°44'36" 1.34751 -1.7 5.0 0.99 3.4E

Venus 09h48m03s +14°50'50" 1.65314 -3.8 10.1 0.97 14.7E

Mars 11h19m47s +05°12'30" 2.29062 1.7 4.1 0.96 39.2E

Jupiter 19h03m51s -22°52'32" 4.23078 -2.6 46.6 1.00 155.1E

Saturn 10h40m21s +10°11'34" 10.20586 1.6 16.3 1.00 28.3E

Mag Limit = 2.50 NASA 2008 Eclipse Bulletin (F. Espenak & J. Anderson)

FIGURE 20 - SKY DURING TOTALITY AS SEEN FROM CENTRAL LINE AT 11:00 UT

Total Solar Eclipse of 2008 Aug 01 
Total Solar Eclipse of 2008 August 01

66

ACRONYMS

AIDS Acquired Immune Deficiency Syndrome

CD Compact Disk

DCW Digital Chart of the World

DMA Defense Mapping Agency (U.S.)

D-SLR Digital-Single Lens Reflex

GPS Global Positioning System

IAU International Astronomical Union

IOTA International Occultation Timing Association

ISO International Organization for Standardization

JNC Jet Navigation Charts

NMEA National Marine Electronics Association

ONC Operational Navigation Charts

SASE Self Addressed Stamped Envelope

SDAC Solar Data Analysis Center

SEML Solar Eclipse Mailing List

SLR Single Lens Reflex

TDT Terrestrial Dynamical Time

TP Technical Publication

USAF United States Air Force

USGS United States Geological Survey

UT Universal Time

UV Ultraviolet

UVA Ultraviolet-A

WDBII World Data Bank II

UNITS

arcsec arc second

ft foot

h hour

km kilometer

m meter

min minute

mm millimeter

nm nanometer

s second

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Total Solar Eclipse of 2008 August 01

68

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R E Q U E S T F O R M F O R N A S A E C L I P S E B U L L E T I N S

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 18 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 for $3.95. 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-2007-214149 — Total Solar Eclipse of 2008 August 01

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Return Requests Fred Espenak or Jay Anderson

and Comments to: NASA/GSFC Royal Astronomical Society of Canada

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

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Standard Form 298 (Rev. 8-98) Prescribed by ANSI Std. Z39-18 

30-03-2007 Technical Publication

Total Solar Eclipse of 2008 August 01

F. Espenak and J. Anderson

Goddard Space Flight Center

Greenbelt, MD 20771 2006-01919-1

National Aeronautics and Space Administration

Washington, DC 20546-0001

TP-2007-214149

Unclassified-Unlimited, Subject Catagory: 89

Report available from NASA Centerfor Aerospace Information, 7115 Standard Drive, Hanover, MD 21076. (301) 621-0390

J. Anderson: Royal Astronomical Society of Canada, Winnipeg, Manitoba, Canada

On 2008 August 01, a total eclipse of the Sun is visible from within a narrow corridor that traverses half the Earth. The path of the

Moon’s umbral shadow begins in northern Canada and extends across Greenland, the Arctic, central Russia, Mongolia, and China.

A partial eclipse is seen within the much broader path of the Moon’s penumbral shadow, which includes northeastern North

America, most of Europe and Asia.

Detailed predictions for this event are presented and include besselian elements, geographic coordinates of the path of totality,

physical ephemeris of the umbra, topocentric limb profile corrections, local circumstances for 308 cities, maps of the eclipse path,

weather prospects, the lunar limb profile and the sky during totality. Information on safe eclipse viewing and eclipse photography

is included.

Solar Eclipse, celestial mechanics, ephemeris, Sun, Moon

Unclassified Unclassified Unclassified Unclassified 69

Fred Espenak

(301) 286-5333