NASA/TPm2002-211618

Annular and Total Solar Eclipses of 2003

E Espenak and J. Anderson

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/

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National Aeronautics and

Space Administration

Goddard Space Flight Center

Greenbelt, Maryland 20771

October 2002

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PREFACE

This work is the ninth 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 12 to 24 months before each event.

Single copies of the bulletins are available at no cost by sending a 9 x 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.

Unlike previous publications in this series each of which focused on a single event, the current bulletin

covers predictions for two disparate solar eclipses. The annular eclipse of 2003 May 31 has a short broad path

which stretches from northern Scotland to Iceland and central Greenland. Six months later, the total eclipse of

2003 November 23 sweeps across Antarctica. To include both of these very different eclipses into one publication, we've organized the bulletin into three sections:

Section 1.0 - Annular Solar Eclipse of 2003 May 31

Section 2.0 - Total Solar Eclipse of 2003 November 23

Section 3.0 - Eclipse Resources

The figures, tables and sub-sections in each of these divisions are labeled with decimal numerals to quickly

identify which section they refer to (e.g., Figure 2.3 is part of Section 2.0). This organization will make it easier

to navigate around the publication.

The 2003 bulletin uses the World Data Bank II (WDBII) mapping data base for the path figures. WDBII

outline files were digitized from navigational charts to a scale of approximately 1:3,000,000. The data base is

available through the Global Relief Data CD-ROM from the National Geophysical Data Center.

The geographic coordinates data base includes over 90,000 cities and locations. This permits the identification of many more cities within the umbral paths and their subsequent inclusion in the local circumstances

tables. These same coordinates are plotted in the path figures and are labeled 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 a digital form which we've 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 data bases have significantly improved the coverage and level of detail

demanded by eclipse planning. Some of these changes are the direct result of suggestions from our readers. We

strongly encourage you to share your comments, suggestions and criticisms 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. Dr. Chou is

Professor of Optometry at the University of Waterloo and he has over twenty-five 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/.

In 1996, Espenak launched the NASA Eclipse Home Page, a web site which provides general information on every solar and lunar eclipse occurring during the period 1951 through 2050. An online catalog also lists

that date and characteristics of every solar and lunar eclipse from 2000 BC through AD 3000. The URL for the

site is: http://sunearth.gsfc.nasa.gov/eclipse/eclipse.html.

iii
In additiontothegeneralinformationwebsiteabove,twospecialwebsiteshavebeensetup:

2003annularsolareclipse- hnp://sunearth.gsfc.nasa.gov/eclipse/ASE2OO3/ASE2OO3htmI

2003 total solar eclipse - http://sunearth.gsfc.nasa.gov/eclipse/TSE2OO3/TSE2OO3html

These sites include supplemental predictions, figures, tables and maps.

Since the eclipse bulletins are of a limited and finite size, they cannot include everything needed by

every scientific investigation. Some investigators may require exact contact times which include lunar limb

effects or for a specific observing site not listed in the bulletin. Other investigations may need customized predictions for an aerial rendezvous or from 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 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 have performed this service for so many years. The many publications

and algorithms of Dr. Jean Meeus have served to inspire a life-long interest in eclipse prediction. Prof. Jay M.

Pasachoff reviewed the manuscript and offered many helpful suggestions. Internet availability of the eclipse

bulletins is due to the efforts of Dr. Joseph B. Gurman. The support of Environment Canada is acknowledged in

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 Annular and Total Solar Eclipses of 2002, Espenak and Anderson, 2002"). 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 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 data base for future eclipses. All calculations, diagrams and opinions are

those of the authors and they assume full responsibility for their accuracy.

email:

FAX:

Fred Espenak

NASA/Goddard Space Flight Center

Planetary Systems Branch, Code 693

Greenbelt, MD 20771

USA

espenak @gsfc.nasa.gov email:

(301) 286-0212

Jay Anderson

Environment Canada

123 Main Street, Suite 150

Winnipeg, MB,

CANADA R3C 4W2

jander @cc.umanitoba.ca

FAX: (204) 983-0109

Current and Future NASA Solar Eclipse Bulletins

NASA Eclipse Bulletin RP # Publication Date

Annular Solar Eclipse of 1994 May 10

Total Solar Eclipse of 1994 November 3

Total Solar Eclipse of 1995 October 24

Total Solar Eclipse of 1997 March 9

Total Solar Eclipse of 1998 Februa_. 26

Total Solar Eclipse of 1999 August 11

1301 April1993

1318 October l993

1344 Ju_ 1994

1369 Ju_ 1995

1383 April1996

1398 March 1997

iv
NASA Eclipse Bulletin TP # Publication Date

Total Solar Eclipse of 2001 June 21

Total Solar Eclipse of 2002 December 04

Annular and Total Solar Eclipses of 2003

1999-209484

2001-209990

2002-211618

November 1999

October 2001

October 2002

........... future ...........

Annular and Total Solar Eclipses of 2005

Total Solar Eclipse of 2006 March 29

B 2003

2004

V
CONTENTS

1.00 - ANNULARSOLARECLIPSEOF 2003 MAY 31 ............................................................................................. 1

1.01 - INTRODUCTION ............................................................................................................................. 1

1.02 - PATH OF ANNULARITY .................................................................................................................. l

1.03 - ORTHOGRAPHIC MAP OF THE MAY 31 ECLIPSE PATH ...................................................................... 2

1.04 - STEREOGRAPHIC MAP OF THE MAY 31 ECLIPSE PATH ..................................................................... 2

1.05 - DETAILED MAPS OF THE PATH OF ANNULARITY .............................................................................. 3

1.06 - ELEMENTS, SHADOW CONTACTS AND MAY 31 ECLIPSE TABLES ....................................................... 3

1.07 - LOCAL CIRCUMSTANCES TABLES FOR MAY 31 ................................................................................ 5

1.08 - LUNAR LIMB PROFILE FOR MAY 31 ............................................................................................... 6

1.09 - INTRODUCTIONTOWEATHERPROSPECTSFORMAY 31 ..................................................................... 7

1.10 - WEATHERPROSPECTSFORGREENLAND.......................................................................................... 7

1.11 - WEATHER PROSPECTS FOR ICELAND ............................................................................................... 8

1.12 - WEATHER PROSPECTS FOR SCOTLAND ............................................................................................ 8

1.13 - WEATHERSTRATEGIES.................................................................................................................. 9

1.14 - WEATHER WEB SITES FOR THE MAY 31 ANNULAR ECLIPSE ............................................................. 9

FIGURES

1.1 - ORTHOGRAPHIC MAP OF 2003 MAY 31 ANNULAR ECLIPSE ............................................................. 11

1.2 - STEREOGRAPHICMAP OF 2003 MAY 31 ANNULARECLIPSE............................................................ 12

1.3 - ECLIPSE PATH THROUGH EUROPE ................................................................................................... 13

- PATH OF ANNULARITY .................................................................................................................. 14

- ANNULAR PATH THROUGH SCOTLAND AND FAEROE ISLANDS ........................................................... 15

- ANNULAR ECLIPSE PATH THROUGH ICELAND .................................................................................. 16

- LUNAR LIMB PROFILE FOR 2003 MAY 31 AT 04:05 UT ................................................................. 17

1.4

1.5

1.6

1.7

TABLES

1.1

1.2

1.3

- ELEMENTS OF ANNULAR ECLIPSE OF 2003 MAY 31 ........................................................................ 18

- SHADOW CONTACTS AND CIRCUMSTANCES OF ANNULAR ECLIPSE ..................................................... 19

- PATH OF ANTUMBRAL SHADOW OF ANNULAR ECLIPSE ..................................................................... 20

1.4 - PHYSICAL EPHEMERIS OF ANTUMBRAL SHADOW OF ANNULAR ECLIPSE............................................. 21

1.5 - LOCAL CIRCUMSTANCES ON CENTRAL LINE OF ANNULAR ECLIPSE ................................................... 21

1.6 - LOCAL CIRCUMSTANCES FOR SCOTLAND AND OUTLYING ISLANDS ..................................................... 22

1.7 - LOCAL CIRCUMSTANCES FOR ICELAND............................................................................................ 23

1.8 - LOCAL CIRCUMSTANCES FOR FAEROE ISLANDS AND GREENLAND ...................................................... 24

1.9 - LOCAL CIRCUMSTANCES FOR ENGLAND, IRELAND AND WALES ......................................................... 24

1.10 - LOCAL CIRCUMSTANCES FOR EUROPE: ALBANIA - FRANCE ............................................................ 25

1.11 - LOCAL CIRCUMSTANCESFOR EUROPE: GERMANY - NORWAY.......................................................... 26

1.12 - LOCALCIRCUMSTANCESFOREUROPE:POLAND- YUGOSLAVIA....................................................... 27

1.13 - LOCAL CIRCUMSTANCES FOR ASIA MINOR .................................................................................... 28

1.14 - LOCALCIRCUMSTANCESFORASIA ............................................................................................... 29

1.15 - LOCALCIRCUMSTANCESFORALASKA& CANADA......................................................................... 29

1.16 - WEATHER STATISTICS FOR ANNULAR ECLIPSE ............................................................................... 30

KEY TO TABLE 1.16 ............................................................................................................................. 31

2.00 - TOTALSOLARECLIPSE OF 2003 NOVEMBER23 ..................................................................................... 33

2.01 - INTRODUCTION........................................................................................................................... 33

2.02 - PATH OF TOTALITY ..................................................................................................................... 33

2.03 - ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH ............................................................... 34

2.04 - STEREOGRAPHIC MAP OF THE NOVEMBER 23 ECLIPSE PATH .......................................................... 34

2.05 - DETAILED MAP OF THE PATH OF TOTALITY ................................................................................... 35

2.06 - ELEMENTS, SHADOW CONTACTS AND ECLIPSE PATH TABLES .......................................................... 35

2.07 - LOCAL CIRCUMSTANCESTABLES FOR NOVEMBER 23 ..................................................................... 37

2.08 - LUNAR LlMB PROFILE FOR NOVEMBER 23 .................................................................................... 38

vii
2.09 - SKY DURING TOTALITY ............................................................................................................... 39

2.10 - INTRODUCTIONTOWEATHERPROSPECTSFORNOVEMBER23 ......................................................... 40

2.11 - WEATHERPATTERNS................................................................................................................... 40

2.12 - COASTOF QUEENMARYLAND- MIRNY ..................................................................................... 41

2.13 - INTERIOROFANTARCTICA........................................................................................................... 42

2.14 - COAST OF QUEEN MAUD LAND - MAITRI, NEUMAYER, AND NOVOLAZAREVSKAJA ........................... 42

2.15 - SELECTINGA SITE....................................................................................................................... 43

2.16 - WEATHERWEB SITESFORNOVEMBER23 TOTALECLIPSE............................................................. 43

FIGURES

2.1 - ORTHOGRAPHICMAP OF 2003 NOVEMBER23 TOTALECLIPSE......................................................... 45

2.2 - STEREOGRAPHICMAP OF 2003 NOVEMBER23 TOTALECLIPSE........................................................ 46

2.3 - ECLIPSE PATH THROUGH ANTARCTICA ............................................................................................ 47

2.4 - LUNARLIMBPROFILEFOR2003 NOVEMBER23 AT22:40 UT ........................................................ 48

2.5 - SKY DURINGTOTALITYFOR2003 NOVEMBER23 AT22:40 UT ...................................................... 49

2.6 - CLOUD STATISTICS FOR THREE STATIONS FOR NOVEMBER ECLIPSE ................................................... 50

TABLES

2.1 - ELEMENTS OF TOTAL ECLIPSE OF 2003 NOVEMBER23 ................................................................... 51

2.2 - SHADOW CONTACTS AND CIRCUMSTANCES OF TOTAL ECLIPSE .......................................................... 52

2.3 - PATH OF UMBRAE SHADOW OF TOTAL ECLIPSE ............................................................................... 53

2.4 - PHYSICAL EPHEMERIS OF UMBRAE SHADOW OF TOTAL ECLIPSE ....................................................... 54

2.5 - LOCAL CIRCUMSTANCES ON CENTRAL LINE OF TOTAL ECLIPSE ........................................................ 55

2.6 - LOCAL CIRCUMSTANCES FOR ANTARCTICA ...................................................................................... 56

2.7 - LOCAL CIRCUMSTANCES FOR ARGENTINA, CHILE AND FALKLAND ISLANDS ....................................... 56

2.8 - LOCAL CIRCUMSTANCES FOR AUSTRALIA ................................................................................... 57-58

2.9 - LOCAL CIRCUMSTANCES FOR NEW ZEALAND .................................................................................. 58

2.10 - LOCAL CIRCUMSTANCES FOR INDONESIA ....................................................................................... 58

2.11 - ANTARCTICSTATIONCLIMATOLOGYFORTOTALECLIPSE................................................................ 59

3.00 - ECLIPSERESOURCES.............................................................................................................................. 61

3.01 - EYE SAFETY AND SOLAR ECLIPSES ............................................................................................. 61

3.02 - SOURCESFORSOLARFILTERS...................................................................................................... 63

3.03 - IAU SOLARECLIPSEEDUCATIONCOMMITTEE.............................................................................. 64

3.04 - ECLIPSEPHOTOGRAPHY............................................................................................................... 64

3.05 - ECLIPSES AT COLD TEMPERATURES .............................................................................................. 66

3.06 - IAU WORKINGGROUPONECLIPSES............................................................................................ 67

3.07 - INTERNATIONAL SOLAR ECLIPSE CONFERENCE .............................................................................. 68

3.08 - NASA ECLIPSE BULLETINS ON INTERNET .................................................................................... 68

3.09 - FUTURE ECLIPSE PATHS ON INTERNET .......................................................................................... 68

3.10- SPECIALWEB SITES FOR2003 SOLARECLIPSES........................................................................... 69

3.11 - PREDICTIONSFORECLIPSEEXPERIMENTS...................................................................................... 69

3.12 - MEAN LUNARRADIUS................................................................................................................ 69

3.13 - ALGORITHMS,EPHEMER1DESANDPARAMETERS............................................................................. 70

FIGURES

3.1 - SPECTRALRESPONSEOF SOLARFmTERS ........................................................................................ 71

TABLES

3.1 - 35MM FIELDOFVIEW................................................................................................................... 72

3.2 - SOLARECUPSE EXPOSUREGUIDE ................................................................................................. 72

BIBLIOGRAPHY ................................................................................................................................................. 73

REFERENCES......................................................................................................................................... 73

METEOROLOGY..................................................................................................................................... 73

EYE SAFETY......................................................................................................................................... 73

FURTHERREADING............................................................................................................................... 74

REQUESTFORM................................................................................................................................................ 75

viii
1.00 ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

1.01 INTRODUCTION

On Saturday, 2003 May 31, an annular eclipse of the Sun will be visible from a broad corridor that

traverses the North Atlantic. The path of the Moon's antumbral shadow begins in northern Scotland, crosses

Iceland and central Greenland, and ends at sunrise in Baffin Bay (Canada). A partial eclipse will be seen within

the much broader path of the Moon's penumbral shadow, which includes most of Europe, the Middle East,

central and northern Asia, and northwestern North America (Figures 1.1 and 1.2).

The trajectory of the Moon's shadow is quite unusual during this event. The shadow axis passes to the

far north where it barely grazes Earth's surface. In fact, the northern edge of the antumbra actually misses Earth

so that one path limit is defined by the day/night terminator rather than by the shadow's upper edge. As a result,

the track of annularity has a peculiar "D" shape that is nearly 1200 kilometers wide. Since the eclipse occurs just

three weeks prior to the northern summer solstice, Earth's northern axis is pointed sunwards by 22.8 ° . As seen

from the Sun, the antumbral shadow actually passes between the North Pole and the terminator. As a consequence of this extraordinary geometry, the path of annularity runs from east to west rather than the more typical

west to east.

The event transpires near the Moon's ascending node in Taurus five degrees north of Aldebaran. Since

apogee occurs three days earlier (May 28 at 13 UT), the Moon's apparent diameter (29.6 arc-minutes) is still too

small to completely cover the Sun (31.6 arc-minutes) resulting in an annular eclipse.

1.02 PATH OF ANNULARITY

The annular eclipse begins in northern Scotland about 100 kilometers north of Glasgow when the Moon's

antumbral shadow first touches down on Earth at 03:45 UT (Figures 1.3 and 1.4). The antumbra quickly extends

northward as it travels on a northwestern trajectory. In Scotland, the Northwest Highlands, Loch Ness, the Isle of

Lewis (Outer Hebrides), Orkney Islands and Shetland Islands all lie in the annular track where maximum eclipse

occurs at or shortly after sunrise (Figure 1.5). Several minutes later, the shadow's edge reaches the Faeroe

Islands (03:51 UT) where annularity lasts 03 minutes 08 seconds with the Sun 4 ° above the northeastern horizon.

By 03:59 UT, the leading edge of the antumbra arrives along the southeastern coast of Iceland (Figure

1.6). Traveling with a ground velocity of 2 kilometers per second, the shadow sweeps across the entire North

Atlantic nation in ten minutes. The shadow is so broad that the duration of the three and a half minute annular

phase varies by less than 5 seconds across all of Iceland. The capital city of Reykjavik lies in the southwest

corner of the country. Here, the Sun will stand 2 ° high during the 3 minute 36 second annular phase. Unfortunately, the low altitude spectacle may be hidden from city dwellers by mountains lying to the northeast.

The instant of greatest eclipse I occurs at 04:08:18 UT when the axis of the Moon's shadow passes

closest to the center of Earth (gamma 2 = +0.996). The length of annularity reaches its maximum duration of 3

minutes 37 seconds, the Sun's altitude is 3°, and the antumbra's velocity is 1.06 km/s. At that time, the shadow's

axis is just 60 kilometers northwest of Iceland.

After traversing the Denmark Strait, the highly elliptical antumbra bisects Greenland where over a third

of the enormous island lies within the track (Figure 1.4). Crossing the ill-named land mass, the path width

rapidly shrinks as the grazing antumbra begins its return to space. From Umanak, the Sun stands 3° above the

Arctic horizon during the 2 minute 24 second annular phase. Seven hundred kilometers to the south, Godth_b

(Nuuk) lies completely outside the path and will not even witness a partial eclipse.

1The instant of greatest eclipse occurs when the distance between the Moon's shadow axis and Earth's geocenter

reaches a minimum.

2 Minimum distance of the Moon's shadow axis from Earth's center in units of equatorial Earth radii.

Annular and Total Solar Eclipses of 2003 1
As it departsGreenlandandcrossesBaffinBay,theshadowleavesEarth'ssurfaceat04:31UT.From

starttofinish,theantumbrasweepsoveritsentirepathin alittleunder47minutes.

1.03 ORTHOGRAPHIC MAP OF THE MAY 31 ECLIPSE PATH

Figure 1.1 is an orthographic projection map of Earth [adapted from Espenak, 1987] showing the path of

penumbral (partial) and antumbral (annular) eclipse. The daylight terminator is plotted for the instant of greatest

eclipse with north at the top. The point of greatest eclipse is indicated with an asterisk-like symbol. The sub-solar

point (Sun in zenith) at greatest eclipse 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/ends at sunrise and sunset,

respectively. Bisecting the 'eclipse begins/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 antumbral shadow travels east to west and is shaded dark gray.

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 Universal Time (UT), and generally run in a north-south direction. The outline

of the antumbral shadow is plotted every ten minutes in UT. Curves of constant eclipse magnitude 3 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%, while adjacent curves are for

magnitudes of 20%, 40%, 60% and 80%.

At the top of Figure 1.1, the Universal Time of geocentric conjunction between the Moon and Sun is

given followed by the instant of greatest eclipse. The eclipse magnitude is given for greatest eclipse. For central

eclipses (both total and annular), 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 is given along with the eclipse's relative sequence in the series.

1.04 STEREOGRAPHIC MAP OF THE MAY 31 ECLIPSE PATH

The stereographic projection of Earth in Figure 1.2 depicts the path of penumbral and antumbral eclipse

in greater detail. The map is oriented with the north up. International political borders are shown and circles of

latitude and longitude are plotted at 20 ° 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 20%, 40%, 60% and 80%, as are the limits of

the path of annular eclipse. Also included are curves of greatest eclipse at every half hour Universal Time.

Figures 1.1 and 1.2 may be used to quickly determine the approximate time and magnitude of maximum

eclipse at any location within the eclipse path.

3Eclipse 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 may be expressed as either a percentage or a decimal fraction (e.g.:

50% or 0.50).

2 Annular and Total Solar Eclipses of 2003
1.05 DETAILED MAPS OF THE PATH OF ANNULARITY

The path of annularity is plotted on a series detailed maps appearing in Figures 1.3 through 1.6. The

maps were chosen to isolate small regions along path using coastline data from the World Data Bank II (WDBII).

The WDBII outline files are digitized from navigational charts to a working scale of approximately 1:3 million.

The positions of larger cities and metropolitan areas are depicted as black dots. The size of each city is

logarithmically proportional to its population using 1990 census data (Rand McNally, 1991). City data sellected

from a geographic data base of over 90,000 cities are plotted to give as many locations as possible in the path of

annularity. Local circumstances have been calculated for many of these positions and can be found in Tables 1.6

through 1.15.

Although no corrections have been made for center of figure or lunar limb profile, they have little or no

effect at this scale. Altmospheric refraction 4 has not been included because it depends on the atmospheric temperature-pressure profile, which cannot be predicted in advance. These maps are also available on the web at

http://sunearth, gsfc. nasa. gov/eclipse/ASE2OO3/ASE2003, html.

1.06 ELEMENTS, SHADOW CONTACTS AND MAY 31 ECLIPSE TABLES

The geocentric ephemeris for the Sun and Moon, various parameters, constants, and the Besselian elements (polynomial form) are given in Table 1.1. 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 AstronomicalAlmanac for 1984 and thereafter. 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 IAU convention through the use of a smaller constant for the mean lunar radius k for all antumbral contacts (see: LUNAR

LIMB PROFILE). Times are expressed in either Terrestrial Dynamical Time (TDT) or in Universal Time (UT),

where the best value of AT5 available at the time of preparation is used.

From the polynomial form of the Besselian elements, any element can be evaluated for any time tI (in

decimal hours) via the equation:

a = a0 + al*t + a2*t z + a3*t3 (or a = _ Jan*t"], n = 0 to 3)

where: a = x, y, d, 1_,12, or g

t = t_ - to (decimal hours) and to = 4.00 TDT

The polynomial Besselian elements were derived from a least-squares fit to elements rigorously calculated at

five separate times over a six hour period centered at t0.Thus, the equation and elements are valid over the period

1.00 < t 1< 7.00 TDT.

4 The nominal value for atmospheric refraction at the horizon is 34 arc-minutes, but this value can vary by a

factor or 2 depending on atmospheric conditions. For an eclipse in the horizon, the umbral path is shifted in

the direction opposite from the Sun.

5 AT is the difference between Terrestrial Dynamical Time and Universal Time (AT = TDT - UT).

Annular and Total Solar Eclipses of 2003 3
Table2.1listsall contactsof penumbralandantumbralshadowswithEarth.TheyincludeTDTtimes

andgeodeticoordinateswithandwithoutcorrectionsfor AT. 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 antumbral shadow cone with Earth's limb.

(annular eclipse begins)

U4 -- Instant of last external tangency of antumbral shadow cone with Earth's limb.

(annular eclipse ends)

Similarly, the southern extremes of the penumbral and antumbral paths, and extreme limits of the antumbral

central line are given. The IAU (International Astronomical Union) 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 antumbral shadow is delineated at one minute intervals in Universal Time in Table 1.3.

Coordinates of the terminator limit, the antumbral limit and the central line are listed to the nearest tenth of an

arc-minute (- 185 m at the Equator). The Sun's altitude, path width and antumbral duration are calculated for the

central line position. Table 1.4 presents a physical ephemeris for the antumbral shadow at one minute intervals in

UT. The central line coordinates are followed by the topocentric ratio of the apparent diameters of the Moon and

Sun, the eclipse obscuration 6, and the Sun's altitude and azimuth at that instant. The antumbral shadow's instantaneous velocity with respect to Earth's surface are included. Finally, the central line duration of the antumbral

phase is given.

Local circumstances for each central line position listed in Tables 1.4 are presented in Table 1.5. The

first three columns give the Universal Time of maximum eclipse, the central line duration of annularity 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

Second Contact

Third Contact

Fourth Contact

-- Instant of first external tangency between the Moon and Sun.

(partial eclipse begins)

-- Instant of first internal tangency between the Moon and Sun.

(central or antumbral eclipse begins; annular eclipse begins)

-- Instant of last internal tangency between the Moon and Sun.

(central or antumbral eclipse ends; annular eclipse ends)

-- Instant of last external tangency between the Moon and Sun.

(partial eclipse ends)

The position angles P and V identify the point along the Sun's disk where each contact occurs 7. Second

and third contact altitudes are omitted since they are always within 1° of the altitude at maximum eclipse.

6 Eclipse obscuration is defined as the fraction of the Sun's surface area occulted by the Moon.

7 p is defined as the contact angle measured counter-clockwise from the north point of the Sun's disk. V is

defined as the contact angle measured counter-clockwise from the zenith point of the Sun's disk.

4 Annular and Total Solar Eclipses of 2003
1.07 LOCAL CIRCUMSTANCES TABLES FOR MAY 31

Local circumstances for -330 cities and locations in the UK, Iceland, Europe and Asia are presented in

Tables 1.6 through 1.15. These tables give the local circumstances at each contact and at maximum eclipse 8 for

every location. The coordinates are listed along with the location's elevation (meters) above sea-level, if known.

Otherwise, the local circumstances are calculated for sea-level. The Universal Time of each contact is given to a

tenth of a second, along with position angles P and V and the altitude of the Sun. The position angles identify the

point along the Sun's disk where each contact occurs and are measured counter-clockwise (i.e., eastward) from

the north and zenith points, respectively. Locations outside the antumbral path miss the annular eclipse and only

witness first and fourth contacts. The Universal Time of maximum eclipse (either partial or annular) is listed.

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 annular eclipses, 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 annularity. The antumbra!

depth is a relative measure of a location's position with respect to the central line and path limits. It is a unitless

parameter that is defined as:

u = 1 - abs(x/R) [1.1]

where: u = antumbral depth

x = perpendicular distance from the shadow axis (kilometers)

R = radius of the antumbral shadow as it intersects Earth's surface (kilometers)

The antumbral 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 antumbral depth, the central line duration

is calculated as:

D = d / (1 - (1 - u)2) m seconds [1.2]

where: D = duration of annularity on the central line (seconds)

d = duration of annularity at location (seconds)

U = antumbral depth

The final column gives the duration of annularity. 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). The city names

and spellings presented here are for location purposes only and are not meant to be authoritative. They do not

imply recognition of status of any location by the United States Government.

8For 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.

Annular and Total Solar Eclipses of 2003 5
1.08 LUNARLIMB PROFILEFORMAY 31

Eclipsecontactimes,magnitudeanddurationof annularityall dependontheangulardiametersand

relativevelocitiesof theMoonandSun.Thesecalculationsarelimitedin accuracyby thedepartureof the

Moon'slimbfromaperfectlycircularfigure.TheMoon'ssurfaceexhibitsaratherdramatictopography,which

manifestsitselfasanirregularlimbwhenseeninprofile.Mosteclipsecalculationsassumesomemeanradius

thataverageshighmountainpeaksandlow valleysalongtheMoon'sruggedlimb.Suchanapproximationis

acceptablefor manyapplications,butif higheraccuracyis needed,theMoon'sactuallimb profilemustbe

considered. Fortunately, anextensivebodyof knowledgexistsonthissubjectintheformofWatts'limbcharts

[Watts,1963].Thesedataaretheproductof aphotographicsurveyof themarginalzoneof theMoonandgive

limbprofileheightswithrespecttoanadoptedsmoothreferencesurface(ordatum).Analysesof lunaroccultationsof starsbyVanFlandern[1970]andMorrison[1979]haveshownthattheaveragecross-sectionofWatts'

datumisslightlyellipticalratherthancircular.Furthermore, theimplicitcenterofthedatum(i.e.,thecenterof

figure)isdisplacedfromtheMoon'scenterof mass.AdditionalworkbyMorrisonandAppleby[1981] shows

thattheradiusof thedatumvarieswith librationproducingsystematicerrorsin Watts'originallimbprofile

heightsthatattain0.4arc-secondsatsomepositionangles.Thus,correctionstoWatts'limbdataarenecessaryto

ensurethatthereferencedatumisaspherewithitscenteratthecenterof mass.

TheWattschartshavebeendigitizedandmaybeusedtogeneratelimbprofilesforanylibration.EllipticityandlibrationcorrectionscanbeappliedtorefertheprofiletotheMoon'scenterof mass.Suchaprofilecan

thenbeusedtocorrecteclipsepredictionswhichhavebeengeneratedusingameanlunarlimb.

ThelunarlimbprofileinFigure1.7includescorrectionsfor centerofmassandellipticity[Morrisonand

Appleby,1981].It isgeneratedforthecentralineat04:05UT,correspondingto centralIceland.TheMoon's

topocentriclibration(physical+ optical)is 1=-2.46° b=+1.28°, andthetopocentricsemi-diametersof theSun

andMoonare945.5and888.2arc-seconds, respectively. TheMoon'sangularvelocitywithrespecttotheSunis

0.539arc-secondspersecond.

Theradialscaleof thelimbprofile(bottomof Figure1.7)isgreatlyexaggeratedsothatthetruelimb's

departurefromthemeanlunarlimbisreadilyapparent.Themeanlimbwithrespectto thecenterof figureof

Watts'originaldatais shown(dashed)alongwiththemeanlimbwithrespecttothecenterof mass(solid).Note

thatallthepredictionspresentedinthispublicationarecalculatedwithrespecttothelatterlimbunlessotherwise

noted.Positionanglesof variouslunarfeaturescanbereadusingtheprotractormarksalongtheMoon'smean

limb (centerof mass).Thepositionanglesof secondandthirdcontactareclearlymarkedalongwiththenorth

poleof theMoon'saxisofrotationandtheobserver'szenithatmid-annularity.Thedashedlineidentifiesthe

contactpointonthenorthlimbcorrespondingto thepathlimit.Totheupperleft of theprofilearetheSun's

topocentriccoordinatesat maximumeclipse.TheyincludetherightascensionR.A., declination Dec., semidiameter 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 04:05 UT while the

times of the eclipse contacts at that location appear to the lower right. Directly below the profile are the local

circumstances at maximum eclipse. They include the Sun's altitude, azimuth, and central duration of annularity.

The position angle of the path's southern limit axis is PA(N.Limit) and the angular velocity of the Moon with

respect to the Sun is A. VeI.(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 1.7, the Sun's limb can be represented as an

epicyclic curve that is tangent to the mean lunar limb at the point of contact. Using the digitized Watts' datum, an

analytical solution is straightforward and robust. Curves of corrections to the times of second and third contact

for most position angles have been computer generated and plotted. 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

6 Annular and Total Solar Eclipses of 2003
thisscalegraphicallyillustratesthetimecorrectiontothemeanpredictionsfor anypositionangleasaresultof

theMoon'struelimbprofile.Timecorrectionsexternaltothecircularscaleareaddedtothemeancontactime;

timecorrectionsinternaltotheprotractoraresubtractedfromthemeancontacttime.Themagnitudeof thetime

correctionatagivenpositionangleismeasuredusinganyofthefourradialscalesplottedateachcardinalpoint.

Forexample,Table1.7givesthefollowingdatafor Reykjavik,Iceland:

SecondContact= 04:02:27.6UT P2=254°

ThirdContact = 04:06:03.5UT P3=077°

MeasuringthecontacttimecorrectionsinFigure1.7,theresultingcontacttimesare:

C2=+3.2seconds; SecondContact = 04:02:27.6+3.2s = 04:02:30.8UT

C3=-5.2seconds; ThirdContact --04:06:03.5-5.2s = 04:05:58.3UT

Theabovecorrectedvaluesarewithin 0.1 secondsof a rigorouscalculationusingthetruelimb

profile.

1.09 INTRODUCTION TO WEATHER PROSPECTS FOR MAY 31

The two polar eclipses of 2003 occur in the springtimes of their opposing seasons. One cannot help but

be struck by their meteorological parallels -- both occur in a marine environment, both have a polar ice cap to

consider as an observing venue, both occur in regions of the globe that are plagued by many active low pressure

systems, and both are famously cloudy over much of the track. Of the two, the annular eclipse across Greenland,

Iceland and northern Scotland offers the poorer weather prospects, though it is easier to reach than November's

eclipse over Antarctica. The best possible escape from the gray skies and wet climate is to select a site on the

Greenland ice cap where high altitude and a drier air may bring favor on eclipse day. The same is true in

Antarctica.

Low pressure systems that develop and cross North America frequently turn to the northeast when they

leave the continent, eventually ending their existence over the waters between Greenland and Iceland. This

location is the home of the infamous Icelandic low, a semi-permanent depression that dictates not only the

weather of its home island but also the meteorology of Britain and northern Europe. The low lies at the boundary

of the cold Arctic airmass that lurks to the north and the warmer maritime climate that accompanies the Gulf

Stream as it flows past Iceland in its clockwise circuit of the Atlantic.

The clash of warm and cold, both in the water and the atmosphere, generates a never-ending succession

of mid-latitude frontal depressions that travel toward the British Isles. In Iceland, overcast skies with rain or

snow are the norm, though precipitation amounts are not especially high. With its more southerly latitude, Scotland is able to tap occasionally into the drier air around the large high-pressure system that lingers near the

Azores, and so the gloominess of north Atlantic weather is relieved occasionally by southerly breezes.

1.10 WEATHER PROSPECTS FOR GREENLAND

Greenland's population lives on the coastal margins of the island, especially on the western side where

the ice cap lies farther back from the coast. The coasts are surmounted by the Greenland ice cap which rises to

over 3000 m in mid-island. In May an east-west oriented high-pressure system lies across the north of the island

while an extension of the Iceland low reaches to Cape Farewell at the southern tip. The northeasterly winds

between these two semi-permanent systems bring a steady flow of cool and humid Arctic air against the sharply

rising east coast. Nearly forty percent of weather observations at eclipse time at Angmagssalik (Table 1.16) have

precipitation falling as a result of this onshore flow and the frequency of overcast skies is more than fifty percent.

On the west coast winds tend to be lighter and more variable, but Davis Strait is a favorite destination for

lows traveling across North America, and so the coast is visited by a steady series of disturbances. Cloud cover

from these systems plus a persistent fog and low cloud that arises from the cool waters of Davis Strait combine

to make this side of the island as nearly as cloudy as the east. Cloud cover statistics derived from satellite images

are subject to a number of complications at Greenland's latitude, but the data do show a tendency to slightly less

cloud along the west coast.

Annular and Total Solar Eclipses of 2003 7
Air ontheicecapismuchcolderanddenserthanthatinthelowlandsandthereisasteadydownhillflow

of coldairtowardthecoastfromtheinteriorknownasakatabaticwind.Thoughgenerallylight,thekatabatic

flowcanexceed100km/hwhenchanneledbyterrain.It ismostcommononthesteepeasterncoastwherethey

areknownasPiteraq.Downslopewindssuchasthesearewarmedslightlyanddriedbycompressionandreach

thecoastasacoldbutdryflowthatcanclearoutsomeof thepersistentcloudsandbringgoodeclipseviewing

conditions.Thoughtheytendtobemostcommonintheearlymorning,predictionisdifficult,astheyarehighly

variablefromplacetoplace.

Onthewestcoast,asoutheastFoehnwindoftendevelopsbringingwarmdryweatherasit descends

fromthemountainpeaks.It istheGreenlandcounterpartof theChinookof NorthAmerica.Foehnwindsmay

lastfor aslongasthreedaysandarefrequentlyfollowedbyprecipitation.Theyaremoreefficienthankatabatic

windsin clearingoutthepersistentcloudinessalongthecoast.A capcloudonthenearbymountainsoften

heraldsthesewinds.

Forthehardiest(andwealthiest)eclipsetravelers,theinterioricecap likely offers the best chances for

clear eclipse viewing. Observations from the cap are few in number and tend to be more concerned with temperature and wind rather than cloud cover. Automatic satellite measurements of cloudiness are unreliable because of the bright ice background and the cold temperatures of the plateau. A Russian study using ten years of

imagery from 1971 to 1980 measured very good sky conditions on the ice cap -- 60 to 68% of the observations

had clear skies or scattered clouds and only 12 to 18% were overcast. The clouds over the ice cap are also likely

to be thinner than that on the coast as the cold air inland is not capable of holding as much moisture as that at

lower altitude.

1.11 WEATHER PROSPECTS FOR ICELAND

Iceland lies alongside one of the most active weather areas in the Northern Hemisphere. The Icelandic

low, about 1000 km to the southwest, is the source of a frequent and endless supply of weather systems that move

past the island, each one bringing its own retinue of cloud and precipitation. The Gulf Stream waters that bathe

Iceland also warm the air and fill it with moisture. As this warm and humid air encounters the colder water from

the Arctic basin west and north, fog and low clouds form and keep gray weather even when an active low is not

present.

Southern regions are marginally more promising than those in the north, in large part because of the

lower frequency of low cloud and fog. Prevailing winds tend to be from the easterly side, so that there is a modest

downslope to the flow at Reykjavik and a consequent drying of the atmosphere. Clear skies are almost unknown,

being less than 5% of observations at all stations save one. Because the eclipse occurs very early with the Sun

only a few degrees above the northeast horizon, clear or scattered cloudiness is almost mandatory.

Satellite observations show a complex pattern of cloudiness around the island. The largest amounts are

in the interior where the higher terrain promotes condensation in the atmosphere. The least cloud is found

straddling the south shore, and reaches slightly inland near Keflavik and Eyrarbakki. On the basis of the available data, a location near Reykjavik would be the most promising, though a good eclipse expedition will follow

the forecast rather than the climatology.

1.12 WEATHER PROSPECTS FOR SCOTLAND

In spite of its more southerly location, Scotland offers no better prospects for viewing the eclipse than

Iceland or Greenland. In spite of this gloomy statement, there is approximately a one-third chance of a sunny

morning for the event according to the cloud and sunshine statistics. Aberdeen sees 36% of possible sunshine in

May and 34% in June, figures very close to the probability calculated in Table 1.16 (which are for the hour of the

eclipse).

Once again the main culprit is the series of frequent frontal lows that pass across or north of the British

Isles in their eastward migration. Virtually all of these lows will bring precipitation to northern Scotland but

spring is the driest season with changeable weather and a chance of a dry spell. Inland areas tend to be cloudier

8 Annular and Total Solar Eclipses of 2003
thanthecoast,inlargepartbecauseof thehigherterrainthatpromotesthelifting of themoistair massesand

theirconversionintocloudyweather.

FogisalsocommonontheScottishcoast,buthighlyvariablefromplacetoplace.FromthedatainTable

1.16,it appearsthatlocationsalongMorayFirth(Inverness, Lossiemouth)havearelativelylowincidenceof fog

whilethoseexposedto theNorthSea(Aberdeen)aremuchmorelikelytoencounterit. Thisdoesnotseemto

havemuchof animpactontheprobabilityof seeingtheeclipse,forthestationswithinandnearthetrackareall

remarkablyalike.OntheScottishmainlandthemostpromisingsiteisatLossiemouthwithascoreof0.34while

theleastpromisingsiteshaveascoreof 0.30.Thesedifferencesaretoosmalltorecommendoneoveranother.

1.13 WEATHER STRATEGIES

While the footprint of the lunar shadow on Earth is very large, the opportunities to view annularity are

very limited. In Iceland, the distance from the capital Reykjavik to the opposite end of the island is only about

450 km (though much longer by road). Scotland's annular zone is barely more than 300 km across from the most

southerly point to the mainland tip. Both of these distances are short enough to allow ready movement to a clear

location on the basis of forecasts on the day before the eclipse. In Scotland, Inverness would seem to be a

convenient staging point, and it has a small weather advantage to boot. In Iceland the same benefits can be

extended to Reykjavik.

Rapid travel from site to site in Greenland is all but impossible unless by aircraft, and so the site selection must be on the basis of the climatology. The available evidence points to the interior ice cap as the best site

by far on the entire track, but cost and opportunity will limit access there. Elsewhere in Greenland, the west coast

holds more promise than the east, which dictates a site at Christianshab or Godhavn, the two largest communities

within the annular zone. These sites are close to the observation sites of Egdesminde and Jacobshavn in Table 1.

The Sun does not set on May 31 and so the lucky eclipse observer could be treated to a midnight sun in annular

eclipse. A sequence of solar images with an eclipse just 2° above the north horizon would surely be one of the

great eclipse photographs - except, perhaps, for those that can be obtained in Antarctica just six months later.

1.14 WEATHER WEB SITES FOR THE MAY 31 ANNULAR ECLIPSE

World m

1. http://www.tvweather.com -- Links to current and past weather and climate around the world

2. http://www.worldclimate.com/climate/index.htm -- World data base of temperature and rainfall

3. http://www.accuweather.com -- Forecasts for many cities worldwide

4. http://www.worldweather.org/A site operated by the World Meteorological Organization with links to climate

and meteorological data worldwide. This site is still being developed and in many instances only climate information is available.

5. http://www.fnoc.navy.mil/PUBLIC/WXMAP/index.html -- U.S. Navy weather center (Fleet Numerical Meteorology and Oceanographic Center - FNMOC). This site provides several (3) model outputs for many areas of

the globe. While complex to use (meteorological expertise is a real bonus), it contains a wealth of model data.

Look for relative humidity forecasts for 700 hPa (hectopascals) - this is a mid-level of the atmosphere and the

relative humidity forecasts provide an indication of the forecast cloud cover from larger weather systems. Use

the 70% contour as the outline of cloud areas. Areas with 90% or greater will likely have precipitation. Model

forecasts for six days in advance for many parts of the world are available.

Scotland, Iceland and Greenland

1. http://weather.uwyo.edu/- An impressive site at the University of Wyoming that allows you to build your own

numerical model output. Choose "Forecasts from Numerical Models" and then "Aviation Model" to be given a

choice of a model output over Scotland, Iceland, or Greenland (chose Europe). Choose 700 mb relative humidity. Values above 70% at 700 mb frequently indicate deep cloudiness.

Annular and Total Solar Eclipses of 2003 9
2.http://www.nottingham.ac.uk/meteosat - NottinghamUniversitysiteforobtainingsatelliteimageryoverScotland,IcelandandpartsofGreenland.Thetwoislandsarequitedistortedintheimagesastheyliewellaroundthe

curveof theEarthfromthesatelliteperspective.

3. http://www.sat.dundee.ac.uk/pdus/- DundeeUniversitysiteof satelliteimageryfor Scotland,Icelandand

Greenland.SelecttheAVsubdirectoryfor visualimagesandtheAI subdirectoryforinfraredpictures.Theseare

largewhole-EarthimageswhereasNottingham'simagesaresectoredandonlyasmallpartof theglobeneedsto

beselectedtoseeeitherIcelandorsouthernGreenland.

4.http://www.weatheroffice.ec.gc.ca/charts/index_e.html -TheMeteorological ServiceofCanadasitehassatelliteimageryof theCanadianArcticandfrequentlymostof Greenland.Select"SatelliteImagery"andlookfor

theCanadianArcticCompositeimageunderHRPT(NOAApolarorbiting).Becausethesatellitesusedarepolar

orbitersinsteadof geostationarysatellites,theimagesoverGreenlandareverydetailed.

5.http://www.met.no/satellitt/- TheNorwegianMeteorological Institutesatellitewebpage.Rectifiedimagesof

Icelandareavailable.Choose"Europa,animasjon:"forananimatedimageofEuropeandthenorthAtlantic.The

satellitesiteisnotinEnglish.

10 AnnularandTotalSolarEclipsesof2003
Annular Solar Eclipse of 2003 May 31

FIGURE 1.1 - ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH

Geocentric Conjunction = 04:38:15.7 UT

Greatest Eclipse = 04:08:17.7 UT

Sun at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 04h30m33.5s

Dec. = +21°50'57.1 ''

S.D. = 00o15'46.5 ''

H.P. = 00o00'08.7 ''

Eclipse Magnitude = 0.93842

Saros Series = 147 Member = 22 of 80

N

I

J.D.= 2452790.693236

J.D.= 2452790.672426

Gamma = 0.99598

Moon at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 04h29m35.5s

Dec.= +22°43'13.2 ''

S.D. = 00°14'48.1 ''

H.P. = 00°54'19.3 ''

W -E

External/Internal

Contacts of Penumbra

P1 = 01:46:16.2 UT

P4 = 06:30:03.6 UT

Ephemeris & Constants

Eph. =DE200/LE200

AT = 64.7 s

kl = 0.2725076

k2 = 0.2722810

Ab = 0.0" AI= 0.0"

I

$

Local Circumstances at Greatest Eclipse

Lat. = 66°33.2'N Sun Alt. = 2.9 °

Long. = 024°30.0'W Sun Azm. = 35.1 °

Duration = 03m36.8s

Ii ii Ipl ill ii Ir p Ill q r I

0 1000 2000 3000 4000 5000

Kilometers

NASA 2003 Eclipse Bulletin (F. Espenak & J. Anderson)

sunearth.gsfc, nasa.gov/eclipse/eclipse, html

External/Internal

Contacts of Umbra

U1 = 03:44:45.8 UT

U4 = 04:31:28.7 UT

Geocentric Libration

(Optical + Physical)

1= -2.60 °

b= -1.15 °

c = -7.26 °

Brown Lun. No. = 995

Annular and Total Solar Eclipses of 2003 11
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Annular Solar Eclipse of 2003 May 31

FIGURE 1.5 - THE PATH THROUGH SCOTLAND AND FAEROE ISLANDS

62 ° N

60 ° N

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NASA 2003 Eclipse Bulletin (F, Espenak & J. Anderson)

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Annular and Total Solar Eclipses of 2003 15
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67 ° N

66 ° N

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63 ° N

Annular Solar Eclipse of 2003 May 31

FIGURE 1.6 - THE PATH THROUGH ICELAND

NASA ( F. Espenak & J. Anderson)

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Annular Solar Eclipse of 2003 May 31

FIGURE 1.7 - LUNAR LIMB PROFILE FOR MAY 31 AT 04:05 UT

Sun at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 04h30m33.1s

Dec. = +21050'47.6 ''

S.D. = 00o15'46.5 ''

H.P. = 00000'08.7 ''

Moon/Sun Ratio = 0.9383

N

000°

True Limb

Mean Limb

(Center of Figure)

Mean Limb

(Center of Mass)

2 0 -2

Seconds

/

Third Contact

Time Correction Cu_e

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Second Contact

Time Correction Curve

180°

Moon at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 04h30m32.Ts

Dec. = +21°50'46.1"

S.D. = 00°14'48.1 ''

H.P. = 00°54'21.7"

\

\

\

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Geographic Position

Name = Center Line at 04:05 UT

Lat. = 65015'55.6"N

Long. = 021°07'33.1"W

Elev. = 0.0 m

Ephemeris & Constants

Eph. = DE200/LE200

AT = 64.7 s

kl = 0.2725076

k2 = 0.2722810

Ab = 0.00" AI = 0.00"

Local Circumstances at Maximum Eclipse

Sun Alt. = 2.8 °

Sun Azm. = 37.3 °

PA(N.Limit) = 165.2 °

Duration = 03m36.6s

A.Vel. (M:S) = 0.539"/s

lllll ill [pl

0 1 2 3 4 5

Arc-Seconds [_ , I , r , I , I ,llot 2 4 6 8Seconds

cor.C2 = 04:03:14.5 UT (2.8s)

Eclipse Contacts

CI= --

C2 = 04:03:11.7 UT

C3 = 04:06:48.3 UT

C4 = 05:02:28.8 UT

AC2 = 2.8s AC3 =-4.7s

Topocentric Libration

(Optical + Physical)

1= -2.46 °

b = -0.26 °

c = -7.18 °

cor.C3 = 04:06:43.6 UT (-4.7s)

NASA 2003 Eclipse Bulletin (F. Espenak & J. Anderson)

Annular and Total Solar Eclipses of 2003 17
TABLE 1.1

ELEMENTS OF THE ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Geocentric Conjunction

of Sun & Moon in R.A.:

Instant of

Greatest Eclipse:

04:39:20.37 TDT

(=04:38:15.67 UT)

04:09:22.42 TDT

(=04:08:17.72 UT)

J.D. = 2452790.693986

J.D. = 2452790.673176

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

Sun: R.A. = 04h30m33.482s

Dec. =+21°50'57.15 ''

Semi-Diameter = 15'46.51"

Eq. Hor. Par. = 08.67"

A R.A. = 10.215s/h

A Dec. = 21.78"/h

Moon: R.A. = 04h29m35.526s

Dec. =+22°43'13.15 "

Semi-Diameter = 14'48.14"

Eq. Hor. Par. = 0°54'19.28 ''

A R.A. = 126.148s/h

A Dec. = 436.27"/h

Lunar Radius

Constants:

kl = 0.2725076 (Penumbra)

k2 = 0.2722810 (Umbra)

Shift in Ab = 0.00"

Lunar Position: A1 = 0.00"

Geocentric Libration:

(Optical + Physical)

1 = -2.6 °

b = -1.2 °

c = -7.2 °

Brown Lun. No. = 995

Saros Series = 147 (22/80)

Ephemeris = (DE200/LE200)

Eclipse Maqnitude = 0.93842 Gamma = 0.99598 AT = 64.7 s

Polynomial Besselian Elements for: 2003 May 31 04:00:00.0 TDT (=t O )

n x y d 11 12

0 -0.3238544 0.9452118 21.8459854 0.5644051 0.0181570 240.614990

1 0.4939022 0.1263288 0.0057463 -0.0000530 -0.0000527 14.999788

2 0.0000545 -0.0001691 -0.0000051 -0.0000098 -0.0000098 -0.000001

3 -0.0000056 -0.0000016 0.0000000 0.0000000 0.0000000 0.000000

Tan /i = 0.0046126 Tan /2 = 0.0045896

At time 't I' (decimal hours), each Besselian element is evaluated by:

a = a 0 + al*t + a2*t 2 + aB*t 3 (or a = E [an*tn] ; n = 0 to 3)

where: a = x, y, d, ii, 12, or

t = t I - t O (decimal hours) and t O = 4.000 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

t O . Thus the elements are valid over the period 1.00 _ t I S 7.00 TDT.

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

Saros Series 147: Member 22 of 80 eclipses in series.

18 Annular and Total Solar Eclipses of 2003
TABLE 1.2

SHADOW CONTACTS AND CIRCUMSTANCES

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

AT = 64.7 s

=000°16'13.2 "

External/Internal

Contacts of Penumbra:

Extreme

North/South Limits

of Penumbral Path:

External/Internal

Contacts of Umbra:

Extreme

North/South Limits

of Umbral Path:

Extreme Limits

of Central Line:

Instant of

Greatest Eclipse:

Circumstances at

Greatest Eclipse:

Terrestrial

Dynamical Ephemeris True

Time Latitude Longitudet Longitude*

h m s

P1 01:47:20.9 23°22.1'N

P4 06:31:08.3 48°42.6'N

052°34.7'E

161°12.9 W

L1 02:12:58.5 I0°51.5'N 051°44.0'E

L2 06:05:33.5 37°05.6'N 164°20.8'W

052°50.9 E

160°56.7 W

052°00.2 E

164°04.6'W

U1 03:45:50.5 56°51.6'N 004°57.3'W 004°41.I'W

U4 04:32:33.4 67°56.3'N 060°22.9'W 060°06.7'W

N1 03:45:59.3 56°47.1'N 004°52.0'W 004°35.7'W

N2 04:32:24.5 67°57.1'N 060°36.3'W 060°20.0'W

CI 04:03:10.5 62°24.9'N 021°31.5'W 021°15.2'W

C2 04:15:14.7 65°29.0'N 035°57.4'W 035°41.2'W

GO 04:09:22.4 66°33.2'N 024°46.3'W 024°30.0'W

Sun's Altitude = 2.9 °

Sun's Azimuth = 35.1 ° Central Duration = 03m36.8s

Ephemeris Longitude is the terrestrial dynamical longitude assuming a

uniformly rotating Earth.

* True Longitude is calculated by correcting the Ephemeris Longitude for

the non-uniform rotation of Earth.

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

Note: Longitude is measured positive to the East.

Since AT is not known in advance, the value used in the predictions is an

extrapolation based on pre-2003 measurements. Nevertheless, the actual

value is expected to fall within ±0.3 seconds of the estimated AT used here.

Annular and Total Solar Eclipses of 2003 19
TABLE 1.3

PATH OF THE ANTUMBRAL SHADOW

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Universal Terminator Limit Antumbral Limit Central Line

Time Latitude Lc_gitude Latitude Lmngitude Latitude Lmngitude

Limits

03:45

03:46

03:47

03:48

03:49

03 :50

03 :51

03 :52

03 :53

03 :54

03 :55

03 :56

03 :57

03:58

03 :59

04 :00

04 :01

04 :02

04 :03

04 :04

04 :05

04 :06

04 :07

04 :08

04 :09

04 :i0

04 :ii

04 :12

04 :13

04 :14

04 :15

04 :16

04 :17

04 :18

04 :19

04:20

04 :21

04 :22

04 :23

04 :24

04:25

04 :26

04 :27

04 :28

04:29

04 :30

04:31

Limits

56°47.1,N 004°35.7,W 56°47.1,N

56°49.0,N 004°40.3,W 57°19.1,N

57°I0.5,N 005°32.3'W 59°16.8,N

57°31.8'N 006°24.9'W 60°26.5'N

57°52.9,N 007°18.3,W 61°24.0,N

58°13.8'N 008°12.3'W 62°14.9'N

58°34.5,N 009°07.1,W 63°01.4,N

58°54.9,N 010°02.7'W 63°44.8,N

59°15.2,N 010°59.1,W 64°25.7,N

59°35.1,N 011°56.2,W 65°04.7,N

59°54.9,N 012°54.1,W 65°42.0,N

60°14.4,N 013°52.9,W 66°17.9'N

60°33.6,N 014°52.5,W 66°52.5,N

60°52.5,N 015°53.0,W 67°25.9,N

61°II.2,N 016°54.4'W 67°58.3,N

61°29.7,N 017°56.6,W 68°29.7,N

61°47.8'N 018°59.8'W 69°00.2'N

62°05.7'N 020°03.9'W 69°29.7'N

62°23.2,N 021°09.0'W 69°58.3,N

62°40.4'N 022°15.0'W 70°26.0'N

62°57.3,N 023°22.0'W 70°52.9,N

63°13.9,N 024°30.0'W 71°18.7,N

63°30.2'N 025°39.0'W 71°43.7'N

63°46.1,N 026°49.0'W 72°07.6,N

64°01.6'N 028°00.0'W 72°30.5'N

64°16.8,N 029°12.1'W 72°52.2,N

64°31.6'N 030°25.2'W 73°12.8'N

64°46.0,N 031°39.4'W 73°32.1,N

65°00.0'N 032°54.6'W 73°50.I'N

65°13.6'N 034°I0.9'W 74°06.6'N

65°26.8'N 035°28.2'W 74°21.5'N

65°39.6'N 036°46.6'W 74°34.7'N

65°51.9,N 038°06.0'W 74°46.0,N

66°03.7'N 039°26.5'W 74°55.3'N

66°15.1,N 040°48.0,W 75°02.3'N

66°26.0'N 042°I0.4'W 75°06.9'N

66°36.5'N 043°33.9'W 75°08.9,N

66°46.4'N 044°58.4'W 75°08.0'N

66°55.8'N 046°23.8'W 75°03.9,N

67°04.7'N 047°50.I'W 74°56.2,N

67°13.0'N 049°17.3'W 74°44.7,N

67°20.8'N 050°45.4'W 74°28.8'N

67°28.1'N 052°14.3'W 74°07.7'N

67°34.8,N 053°44.0'W 73°40.6,N

67°40.9'N 055°14.4'W 73°05.8'N

67°46.5'N 056°45.4'W 72°20.6,N

67°51.4'N 058°17.1'W 71°18.4,N

67°55.8,N 059°49.4,W 69°34.4,N

67°57.1'N 060°20.0'W 67°57.1'N

004°35.7'W

003°40.2'W

000 ° 59.9 'W

000 ° 05.6 'E

000°46.0'E

001 ° 12.2 'E

001°28.4 'E

001°36.9'E

001°39.1'E

001°35.7'E

001°27.3 'E

001 ° 14.2 'E

000°56.5'E

000°34.5'E

000 ° 08.2 'E

000°22.4 'W

000 ° 57.3'W

001 ° 36.6 'W

002°20.4,W

003°08 8'W

004°02 0'W

005°00 I'W

006°03 3'W

007°11 8'W

008°25 8'W

009°45.4'W

011 ° i0.9 'W

012°42.4'W

014 ° 20.0 'W

016 ° 03.9 'W

017 ° 54.1 'W

019 ° 50.5 'W

021 ° 53.2 'W

024 ° 01.9 'W

026 ° 16.3 'W

028 ° 36.0 'W

031 ° 00.6 'W

033°29.4'W

036 ° 01.6 'W

038 ° 36.4 'W

041 ° 12.9 'W

043 ° 50. I' W

046°27.0'W

049 ° 02.8 'W

051 ° 36.7 'W

054 ° 08.1 'W

056 ° 37.7 'W

059 ° ii. 3 'W

060 ° 20.0 'W

Sun Path Central

Aft Width Durat.

o km

62°24.9'N 021° 15.2'W 0

63° 54.6'N 020° II.7'W

64°40.6'N 020°29.7'W

65° 15.9'N 021° 07.6'W

65°44.8'N 021° 58.0'W

66° 08.7'N 022° 58.5'W

66°28.3'N 024° 07.9'W

66°43.4'N 025°25.7'W

66° 54.0'N 026° 51.8'W

66° 59.2'N 028°26.6'W

66° 57.6'N 030° II.5'W

66°45.2'N 032° 10.1'W

66° 03.5'N 034°43.3'W

65°29.0'N 035°41.2 'W 0

2 - 03m36. Is

2 - 03m36.4s

3 - 03m36.6s

3 - 03m36.7s

3 - 03m36.8s

3 - 03m36.8s

3 - 03m36.7s

3 - 03m36.7s

3 - 03m36.6s

2 - 03m36.4s

2 - 03m36. is

1 - 03m35.5s

20 Annular and Total Solar Eclipses of 2003
TABLE 1.4

PHYSICAL EPHEMERIS OF THE ANTUMBRAL SHADOW

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Universal

Time

Central Line Diameter Eclipse Sun Sun Path Major Minor Umbra Central

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

o o km km km km/s

04:03

04:04

04:05

04:06

04:07

04:08

04:09

63°54.6'N 020°II.7'W 0 9380 0.8799

64°40.6'N 020°29.7'W 0

65°15.9'N 021°07.6'W 0

65°44.8'N 021°58.0'W 0

66°08.7'N 022°58.5'W 0

66°28.3'N 024°07.9'W 0

66°43.4'N 025°25.7'W 0

1.5 37.7 -

9382 0.8802 2 1 37.6 -

9383 0.8804 2 5 37.3 -

9384 0.8805 2 7 36.8 -

9384 0.8806 2 9 36.1

9384 0.8806 2 9 35.3

9384 0.8806 2 9 34.4 -

1.851 03m36.1s

1.338 03m36.4s

1.166 03m36.6s

1.090 03m36.7s

1.059 03m36.8s

1.057 03m36.8s

1.077 03m36.7s

04:10 66°54.0'N 026°51.8'W 0.9384 0.8806 2.8 33.3 -

04:11 66°59.2'N 028°26.6'W 0.9383 0.8805 2.6 32.1 -

04:12 66°57.6'N 030°ii.5'W 0.9383 0.8803 2.2 30.8 -

04:13 66°45.2'N 032°i0.I'W 0.9381 0.8801 1.7 29.2 -

04:14 66°03.5'N 034°43.3'W 0.9379 0.8796 0.7 27.1 -

1.123 03m36.7s

1.206 03m36.6s

1.364 03m36.4s

1.740 03m36.1s

4.724 03m35.5s

TABLE 1.5

LOCAL CIRCUMSTANCES ON THE CENTRAL LINE

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Central Line

Maxi_amEclipse First Contact

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

O O O O

Second Contact Third Ccntact Fourth Contact

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

O O O O O o O

04:03 03m36.1s 2 - - - 04:01:12 255 272 04:04:48 75 92 05:00:09 75 96 6

04:04 03m36.4s 2 - - - 04:02:12 255 271 04:05:48 75 92 05:01:21 75 95 7

04:05 03m36.6s 3 - - - 04:03:12 255 271 04:06:48 75 91 05:02:29 75 95 7

04:06 03m36.7s 3 03:09:47 256 266 0 04:04:12 255 271 04:07:48 75 91 05:03:33 75 94 7

04:07 03m36.8s 3 03:10:43 256 266 1 04:05:12 255 270 04:08:48 75 90 05:04:35 75 94 7

04:08 03m36.8s 3 03:11:40 256 265 1 04:06:12 255 270 04:09:48 75 90 05:05:35 75 94 7

04:09 03rn36.7s 3 03:12:40 256 265 1 04:07:12 255 269 04:10:48 75 90 05:06:32 75 93 7

04:10 03m36.7s 3 03:13:41 256 265 1 04:08:12 256 269 04:11:48 76 89 05:07:28 75 93 7

04:11 03rn36.6s 3 03:14:44 256 264 1 04:09:12 256 269 04:12:48 76 89 05:08:22 75 93 6

04:12 03m36.4s 3 03:15:50 256 264 1 04:10:12 256 268 04:13:48 76 88 05:09:13 75 92 6

04:13 03m36.1s 2 - - - 04:11:12 256 268 04:14:48 76 88 05:09:59 75 92 5

04:14 03m35.5s 1 - - - 04:12:12 256 267 04:15:48 76 88 05:10:33 76 92 4

Annular and Total Solar Eclipses of 2003 21
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Annular and Total Solar Eclipses of 2003 27
bo

Oo TABLE 1.13

LOCAL CIRCUMSTANCES FOR ASIA MINOR

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

>

tO

Location Name Latitude Longitude Elev.

ARMENIA

Jerevan 40°ll'N 044°30,E

AZERBAIJAN

Baku 40°23 'N 049°51'E

BAHRAIN

Ai-Manamah 26°13 'N 050°35 'E

GEORGIA

Tbilisi 41°43'N 044°49'E

IRAN

E s f a han

@as_ad

Qom

Shiraz

Tehran

IRAQ

Baghdad

ISRAEL

Tel Aviv-Ya fo

JORDAN

' _nman

KUWAIT

Ai-Kuwayt

LEBANON

Beirut

Tripoli

OMAN

Masqat

SAUDI ARABIA

Riyadh

SYRIA

Damascus

TURKEY

Adana

Ankara

Bursa

Gaziantep

Istanbul

Izmir

Konya

UNITED ARAB EMIRATES

Abu Dhabi 24°28 'N 054°22 'E

YEMEN

Sana 15°23 _N 044°12 ,E

First Contact

U.T. P V Alt

m h m s

-- 01:59:56.6 273 320 4

-- 01:58:38.6 275 324 7

-- 01:46:57.7 290 351 0

-- 02:01:40.1 272 318 5

32°40'N 051°38'E 1597 01:50:28.6 282 339 4

36°18'N 059°36'E -- 01:53:31.5 283 339 12

34°39'N 050°54'E -- 01:52:20.0 280 334 4

29°37'N 052°33'E -- 01:48:16.1 286 346 3

35°40'N 051°26'E 1200 01:53:10.2 279 333 5

33°21'N 044°25'E 34

32°04'N 034°46'E i0

31°57'N 035°56'E 776

29°20'N 047°59'E 5

33°53,N 035°30,E _ _

34°26,N 035°51,E

23°37'N 058°35'E -- 01:47:12.9 299 6 5

24°38'N 046°43'E 591

33°30'N 036°18'E 720

37°01'N 035°18'E 25

39°56'N 032°52'E 861

40°ll,N 029°04,E

37°05,N 037°22,E

41°01'N 028°58'E 18

38°25'N 027°09'E 28

37°52,N 032°31,E

-- 01:46:22.4 294 359 2

Second Contact Third Contact

U.T. P V U.T.

h m s h m s

Fourth CoDtact Maximum EGliD_@

P V U.T. P V Alt U.T. P V Aft Azm Mag. Obs.

o h m s o o o h m s o o o o

03:54:55.0 43 98 24 02:55:03.4 338 30 13 72 0.582 0.474

03:54:35.2 40 95 28 02:54:06.8 337 30 17 75 0.541 0.428

03:18:36.9 24 92 19 02:31:06.1 337 42 9 70 0.321 0.204

03:58:22.3 44 98 25 02:57:36.2 338 29 14 73 0.598 0.492

03:34:54.7 31 94 25 02:40:31.5 337 37 14 73 0.418 0.298

03:42:23.9 28 89 33 02:45:32.4 336 34 22 78 0.395 0.275

03:40:12.0 34 95 25 02:43:59.3 337 35 14 73 0.454 0.335

03:26:32.2 26 93 23 02:35:26.9 336 39 12 72 0.361 0.241

03:42:36.5 34 94 27 02:45:33.0 337 34 15 74 0.464 0.345

03:39:17.8 37 98 20 02:44:04.4 338 35 9 70 0.489 0.372

03:40:48.6 42 102 12 02:46:59.1 339 35 2 65 0.540 0.427

03:39:59.1 41 i01 13 02:46:09.3 339 35 2 65 0.531 0.417

03:28:07.9 30 95 19 02:36:38.2 337 39 9 70 0.397 0.277

03:44:09.3 43 102 14 02:49:04.3 339 34 3 66 0.562 0.452

03:45:07.6 43 102 14 02:49:39.7 339 33 4 66 0.568 0.458

03:04:34.1 12 84 22 02:24:38.5 335 45 13 72 0.196 0.100

03:17:08.0 25 94 15 02:30:39.1 337 43 5 68 0.327 0.209

03:43:00.3 42 102 14 02:48:05.8 339 34 3 66 0.552 0.440

03:50:37.7 46 102 16 02:53:41.3 339 31 5 66 0.607 0.503

03:57:21.5 50 103 16 02:59:14.5 339 29 6 66 0.660 0.563

03:59:11.5 52 104 14 03:01:34.8 340 28 4 64 0.685 0.593

03:50:01.5 45 i01 17 02:52:47.7 339 31 6 67 0.594 0.488

04:00:49.4 53 104 14 03:02:51.4 340 27 4 64 0.696 0.605

03:56:38.4 51 105 ii 03:00:09.1 340 29 1 62 0.674 0.580

03:53:23.1 48 103 14 02:56:21.6 339 30 4 65 0.636 0.536

03:10:57.7 18 88 20 02:27:11.8 336 44 i0 71 0.254 0.146

02:54:11.1 ii 86 4 02:33 Rise 0 67 0.142 0.062

Eclip. Eclip. Umbral Umbral

Depth Durat.
>

=_

CO

tO

C_

L_

TABLE 1.14

LOCAL CIRCUMSTANCES FOR ASIA

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Location Name Latitude Longitude Elev. First Contact

U.T. P V Alt U.T.

m h m s o _ h m s

Second Contact Third Contac_ Fourth Contact Maximum Eclinse Eclip. Eclip. Umbral Umbral

P V U.T. P V U.T. P V A/t U.T. P V Alt Azm Mag. Obs. Depth Durat.

o o h m s o h m s _ o a h m s o o o o

AFGHANISTAN

Kabul 34°31'N 069°12'E 1815 01:55:36.8 292 351 19 --

CHINA

Shihezi 44°18'N 086°02'E -- 02:23:06.5 295 346 38 --

Wulumuqi 43°48'N 087°35'E 906 02:25:35.1 298 349 40 --

INDIA

Ahmadabad 23°02'N 072°37'E 55 02:07:06.5 321 34 22 --

Delhi 28°40'N 077°13'E -- 02:06:47.3 312 20 27 --

Jaipur 26°55'N 075°49'E -- 02:06:02.4 314 24 25 --

New Delhi 28°36'N 077°12'E 212 02:06:50.1 312 20 27 --

KAZAKHSTAN

Alma-Ata 43°15'N 076°57'E 775 02:10:08.0 288 340 29 --

Karaganda 49°50'N 073°I0'E _ 02:16:11.6 280 324 28 --

KYRGYZSTAN

Bishkek (Frunze) 42°54'N 074°36'E -- 02:07:38.2 287 339 27 --

PAKISTAN

Faisalabad 31°25'N 073°05'E -- 01:58:00.2 300 4 22 --

Islamabad 33°42'N 073°I0'E _ 01:58:40.2 297 358 23 --

Karachi 24°52'N 867°03'E 4 01:52:34.8 305 14 14 --

Lahore 31°35'N 074°18'E -- 01:59:35.7 301 5 23 --

Rawalpindi 33°36'N 073°04'E 511 01:58:30.5 297 358 23 --

TAJIKISTAN

Dusanbe 38°35'N 068°48'E -- 01:58:52.3 287 342 20 --

TURKMENISTAN

Aschabad 37°57'N 058°23'E -- 01:55:06.9 281 334 12 --

UZBEKISTAN

Taskent 41°20'N 069°18'E -- 02:02:10.4 284 337 22 --

03:33:59.0 17 79 39 02:42:42.7 334 36 29 82 0.264 0.154

04:07:53.3 13 55 56 03:13:24.8 334 22 47 106 0.215 0.114

04:05:36.1 i0 52 57 03:13:41.5 334 22 48 107 0.188 0.094

02:37:07.3 345 60 28 02:22:02.0 333 47 25 76 0.022 0.004

03:00:38.1 353 63 38 02:33:08.0 333 42 33 81 0.065 0.020

02:53:36.1 351 63 35 02:29:24.0 333 44 30 79 0.052 0.014

03:00:17.3 353 63 38 02:32:59.7 333 42 32 81 0.064 0.019

04:03:25.5 21 69 50 03:04:14.1 334 26 39 96 0.306 0.190

04:23:44.9 32 71 48 03:17:08.2 336 19 38 i01 0.437 0.318

04:02:01.i 22 72 48 03:02:13.2 335 27 37 94 0.327 0.210

03:19:46.4 7 73 39 02:37:25.3 333 39 30 81 0.168 0.078

03:28:52.2 Ii 74 41 02:41:59.6 334 37 32 83 0.203 0.105

02:59:33.2 3 76 29 02:25:07.0 334 45 21 75 0.125 0.051

03:19:18.1 5 72 40 02:38:03.4 333 39 31 82 0.154 0.070

03:28:33.0 10 75 41 02:41:45.4 334 37 31 83 0.203 0.105

03:47:46.6 22 80 41 02:50:51.2 335 32 30 85 0.330 0.213

03:47:14.3 31 89 33 02:48:39.6 336 33 22 79 0.431 0.311

03:56:36.5 25 79 43 02:56:44.7 335 29 32 88 0.364 0.245

bO

_O

TABLE 1.15

LOCAL CIRCUMSTANCES FOR ALASKA & CANADA

ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Location Name Latitude Longitude Elev.

ALASKA

Anchorage

Barrow

Cordova

Fairbanks

Juneau

Kenai

Kodiak

Nome

Petersburg

Seward

Sitka

First Contact Second Contact

U.T. P V Aft U.T. P V

m h m s o o h m s o

61°13'N 149°54'W 26 04:31:17.2 288 259 15

71°18'N 156°47'W -- 04:09:59.1 280 260 22

60°33'N 145°45'W -- 04:31:21.7 287 258 13

64°51'N 147°43'W 133 04:23:02.2 284 258 16

58°18 'N 134°25'W 4 04:30:38.1 285 256 7

60°33'N 151°16'W -- 04:33:07.2 289 259 15

57°47'N 152°24'W -- 04:39:35.1 293 260 14

64°30 'N 165°25'W -- 04:25:51.4 290 262 23

56°48'N 132°58'W -- 04:32:23.8 286 256 5

60°07 'N 149°27'w -- 04:33:30.3 289 259 14

57 °03'N 135°20'W -- 04:33:17.7 287 256 6

-- 03:32:47.6 262 261 14

-- 03:49:21.5 265 256 i0

04:26:43.6 283 256 9

04:13:21.8 275 254 3

CANADA

Alert, NU 82°30 'N 062°18 ,W

Resolute Bay, NU 74°43'N 094°59,W

Whitehorse, YT 60°43 'N 135°03 'W 702

Yellowknife, NT 62°27'N i14°21 ,W 205

Third Contac_ Fourth Contact Maximum Eclipse Eclip. Eclip. Umbral Umbral

U.T. P v U.T. P V Alt U.T. P V Alt Azm Mag. Obs. Depth Durat.

h m s o h _ s o _ h m s Q o o o

06:21:21.1 54 31 4 05:27:42.9 351 324 9 300 0.530 0.417

06:11:30.5 59 41 13 05:12:00.0 349 330 17 288 0.623 0.521

06:20:33.7 55 33 2 05:27:18.2 351 325 7 303 0.546 0.434

06:17:14.6 58 38 6 05:21:28.3 351 327 Ii 300 0.588 0.481

-- 05:25:05.4 352 327 2 313 0.586 0.478

06:22:19.5 53 29 4 05:29:08.2 351 324 9 299 0.514 0.398

06:24:49.8 51 24 2 05:33:37.3 352 322 8 299 0.468 0.349

06:20:46.0 51 27 ii 05:24:51.2 351 324 17 285 0.493 0.376

-- 05:26:00.0 352 327 0 314 0.577 0.468

06:22:09.4 54 30 3 05:29:13.4 352 324 8 301 0.518 0.404

-- 05:27:03.0 352 326 1 312 0.565 0.455

05:36:38.1 70 73 15 04:34:42.5 346 347 14 7 0.873 0.817

05:47:14.7 71 69 7 04:48:42.3 348 342 8 339 0.853 0.792

06:15:53.4 0 0 0 05:22:29.4 351 328 3 311 0.610 0.506

-- 05:09:01.2 350 334 0 327 0.735 0.652
O

>

=_.

O.-

c

m

o

I-O

L..o

Perc,

Location Latitude Longitude Clear Scattered

Greenland

Angmagssalik 65.60 -37.63 10.0 18.7

Danmarkshaun 76.77 -18.67 19.6 26.3

Egedesminde * 68.70 -52.75 4.8 24 4

Fredenskshab 62.00 -43.72 6.4 16.4

Godthab 64.17 -51.75 6.2 19,1

Holsteinsborq 66 92 -53.67 13.5 21.1

Jakobshavn * 69.25 -51.07 11.4 20.0

Julianehab 60 72 -46.05 12.8 20.5

Narssarssuaq 60.18 -45.42 6.7 25.9

Prir_s Christian 60.03 -43.12 14.8 20.1

Sonder Stromfjord 67.00 -50.80 7.8 29.6

Upernavik 72,78 -56.17 12.2 25 8

Iceland

Akureyri* 65.68 -18.08 3.0 18,4

Raufarhofn * 66.45 -15.95 6.8 15.1

Blonduos * 65.67 -20.30 1.1 1 7

Stykkisholmur * 65.08 -22.73 4.1 15.6

Hlardarnes ° 65.25 -15.18 0.5 23.2

Reykjavik ° 64.13 -21 54 0.9 26 9

Keflavik * 63.97 -22.60 2.4 20.7

Eyrarbakkl * 63.87 -21.15 1.1 26.3

Vestmannaeyjar * 63.40 -20.28 2.8 25.2

62.02 -6.77

Table 1.16 - Weather Statistics for

Annular Solar Eclipse of 2003 May 31

Faeroes

Thorshaun *

% hours with Monthly

Overcast & cloud< 0.3 & pcpr_

Broken Obscured obabihty vls >2 (mm)

17.3 53.9 0.27 17 58.4

17.7 36.4 0.42 30 5.1

32.5 38.2 0.30 1 1 15.2

13.9 63.2 0.21 1 1

21.8 52.9 0.25 1 2 43.2

20.7 44.8 0.33 2 1

42.9 25.8 0.37 1 1

19 1 47 6 0,32 1 9

28.1 39.2 0.32 1 9

16.7 46.4 0.33 22 177.8

42.2 20.4 0.40 20 12.7

22.9 39.1 0,36 21

29.3 49.3 0.24 20 17.8

22.3 55.9 0.23 1 1

11.6 70.2 0,16 8

31.1 49.1 0.24 9 35.6

24.7 51.6 0.23 8 86.4

35.2 36.9 0.29 1 3 43.2

32.3 44 7 0.26 1 0 76.2

28.3 44 3 0.27 1 5

23.2 48.8 0.26 I 5 83.8

4.6 12.4 28.3 54.6 0 21 7 78.7

Jan Mayen * 70.93 -8.67 1.1 12.9

United Kingdom

Lerw_ck, Shetland Is. * 60 13 -1.18 0.6 21.2

Kirkwall, Orkney Is * 58.95 -2.90 1.9 25.0

Wick * 58.45 -3.08 2.4 22.4

Stornoway • 58.22 -6.32 2.3 32 0

Aberdeen 57.20 -2.22 1.8 25.9

Benbecula Island 57.47 -7.37 3.7 32.8

Fort William 56.83 -5.10 2 7 26.6

Invergordon Harbour * 57.68 -4.17 6.7 21.2

Inverness * 57.53 -4.05 1.7 17.8

Klnloss RAF " 57.65 -3.57 1.6 24.1

Lossiemouth RAF * 57.72 -3.32 2.5 25.3

Peterhead Harbour 57 50 -1.77 5.9 23 2

Edinburgh 55.95 -3.21 2.6 27 2

Manchester 53.21 -2.27 7 7 27.9

Leeds 53.48 -1.55 12.7 31.7

Birmingham 52.45 -1.73 7.8 30

London 51.48 -0.45 15.2 27.1

Glasgow 55.87 -4.43 3.3 27.8

* indicates station is within annular zone

% obsewat_ons % observatioe_

with precipitation with fog

38.0 15 5

22.1 18.9

20.7 5.2

30.9 14.0

37.4 11.1

24.3 5.4

2 34 8.4

28.8 8.8

3 3.7 2.2

31.1 5.6

21.5 0.2

18.4 4.4

12.8 3.3

17.3 19.1

22.6 10.3

13.8 4.9

25.4 17.5

34.3 7.4

23 1 8.2

24,4 9.1

28.3 8.3

32.3 9.9

37.2 48 7 0.21 5 30.5 25.9

39.1 39.1 0.26 9 55.9

41.2 31.8 0.31 10

47.6 27.6 0.31 9

36 5 29.2 0.34 1 7 55.9

40.5 31.8 0.31 1 1 53.3

39.3 24.0 0.37 1 7

42.3 28.4 0.33 1 0 99.1

32.0 40.1 0.30 12

56.1 24.4 0.30 10 45,7

52.4 21.8 0.33 1 4 48.3

51.0 21.1 0.34 13 53.3

30.8 40.2 0,30 8

46 0 24.3 0.34 1 4 50.8

42.6 21.8 0.39 1 7 63.5

39.7 15.9 0.45 29

36.1 26.1 0.38 19 55.9

32.9 24 9 0.43 24 45.7

44 24 9 0.35 1 4

Key to tab/e t. 16 appears on next page.

Mean Prevailing

Wind direction

11.1 vrbl 3 -2

10.0 W -4 -9

5.8 W 0 -4

6.1 _ 3 -1

10.3 S 2 -2

5.0 _ 2 -3

4,6 S 0 -4

5.6 calm 6 1

6.7 ENE 8 2

12.1 N 3 0

6.9 ENE 6 -2

5.5 calm -2 -6

7,5 SIS 9 3

9.1 _ 6 1

6.2 calm 7 3

9.9 E 7 4

10.5 E 8 4

9.3 E 8 4

10.0 _ 4 4

10.1 I',E 9 5

18.3 _ 7 4

8.0 calm 8 6

17.4 10.4 N 1 -2

27.4 19 1

24.0 20.1

19.9 17.5

27.1 6 7

24.2 21.5

25.1 5.2

11.9 0.5

17.8 6.4

18.8 7.1

24.0 11.0

21.8 9.7

18 76

23.6 18.0

20.5 8 0

14.3 6.3

21.8 26

18 3 9.7

22.2 11.7

10.8 N 9 6

10.4 S 11 6

8.2 SE 11 6

8.6 vrbl 12 6

5,9 vrbl 1 3 6

10.5 vrbl 12 7

4.9 calm 14 8

5.8 calm 13 8

6.0 SW 13 7

6.5 SW 13 6

6.9 SW 13 6

7.9 S 11 7

5.7 WSW 14 6

6.2 S 15 7

3 6 WNW 16 8

5,7 vrbl 16 6

5,2 N 17 6

6 E)XIE 15 6
WEATHER STATISTICS FOR ANNULAR SOLAR ECLIPSE OF 2003 MAY 31

Key to Table 1.16

Percent Frequency of Clear, Scattered (2-4 tenths), Broken (5-9 tenths)

and Overcast or Obscured Skies

These data are compiled from surface observations at the site. The time of the observation is usually

0300 UTC except for a few stations where observations at that time are missing. This is about one

hour before the eclipse.

Probability

A rough calculation of the probability of seeing the eclipse based on the frequency of clear,

scattered, broken or overcast cloud. It is essentially the sums of the frequency of the cloud category

times a representative clear sky amount for the category.

% hours with cloud <0.3 and vis > 2

This the frequency of hours with less than 3 tenths cloud and visibilities of 3 miles or more. The

time of observation is 0300 UTC except for a few cases as noted above.

Monthly pcpn

Average May precipitation in mm. Snow is melted and the water content measured.

% of observations with precipitation

The percent of observations at 0300 UTC in May in which precipitation is reported.

% of observations with fog

The percent of 0300 UTC observations with visibility less than 3 miles.

Mean wind

The average wind speed in May at 0300 UTC

Prevailing Direction

The most frequent wind direction. Where winds do not show a dominant direction, "vrbl"

(variable) is shown. If calm winds are the most common condition and more than 20% of

observations, "calm" is indicated.

Tmax

Mean daily high temperature (°C) for December.

Tmin

Mean daily minimum temperature (°C) for December.

Annular and Total Solar Eclipses of 2003 31
2.00 TOTALSOLAR ECLIPSEOF 2003 NOVEMBER23

2.01 INTRODUCTION

On Sunday, 2003 November 23, a total eclipse of the Sun will be visible from a broad corridor that

traverses portions of the Southern Hemisphere. The path of the Moon's umbral shadow begins in the Indian

Ocean, crosses Antarctica, and ends at sunrise near the edge of the southern continent. A partial eclipse will be

seen within the much broader path of the Moon's penumbral shadow, which includes Australia, New Zealand,

Antarctica and southern South America (Figures 2.1 and 2.2).

The trajectory of the Moon's shadow takes it between the sunrise terminator and the South Pole. As

viewed from the Sun's direction, the Moon's shadow passes around the "back" side of the pole between Earth's

axis of rotation and the terminator. Consequently, the track of totality travels east to west rather the usual west to

east direction. Furthermore, the 500 kilometer wide path both begins and ends at sunrise, just like the May 3 l

annular eclipse. The unusual characteristics of these two events is directly attributed to their grazing geometries

in Earth's polar regions coupled with the close temporal proximity of the eclipses with summer solstice in each

hemisphere.

2.02 PATH or TOTALITY

The path of the Moon's umbral shadow begins at 22:19 UT in the southern Indian Ocean about 1100

kilometers southeast of Kerguelen Island (Figure 2.2). Curving south, the five hundred kilometer wide umbral

path reaches the coast of Antarctica at 22:35 UT. The Shackleton Ice Shelf and Russia's Mirny research station

lie in the path where the central duration is 1 minute 55 seconds and the Sun stands 13° above the frozen

landscape. Quickly moving inland, the elongated shadow sweeps over the desolate interior of the continent at

velocities exceeeding 1 kilometer per second (Figure 2.3). No other permanently staffed research stations are

encountered for the next half hour.

The instant of greatest eclipsC occurs in Wilkes Land at 22:49:17 UT when the axis of the Moon's

shadow passes closest to the center of Earth (gamma 2= -0.964). At this point, the duration of totality reaches its

maximum of 1 minute 55 seconds with a Sun altitude of 15°. The duration and altitude slowly drop as the

umbra's path curves from southwest to northwest. The umbra reaches the Antarctic coast in Queen Maud Land,

which harbors several more research stations (Novolazarevskaya, Maitri). From Maitri, the 1 minute 19 second

total phase occurs with the Sun just 2 ° above the horizon at 23:17 UT.

Two minutes later, the path ends and the shadow leaves Earth's surface (23:19 UT) one hour after it

began. Over the course of its sixty minute trajectory, the Moon's umbra sweeps over a track approximately 5,000

kilometers long and covering 0.51% of Earth's surface area.

The rest of Antarctica will see a partial eclipse as well as most of New Zealand, Australia, southern

Argentina and Chile (Figure 2.2). Outside of Antarctica, southwestern Australia will witness the largest eclipse.

For instance, citizens of Perth will be treated to an early morning partial eclipse of magnitude 0.612. In contrast,

the Cape York Peninsula in northeastern Australia lies beyond the penumbra's path and will miss the eclipse

entirely.

' The instant of greatest eclipse occurs when the distance between the Moon's shadow axis and Earth's geocenter

reaches a minimum. Although greatest eclipse differs slightly from the instants of greatest magnitude and

greatest duration (for total eclipses), the differences are usually quite small.

2 Minimum distance of the Moon's shadow axis from Earth's center in units of equatorial Earth radii.

Annular and Total Solar Eclipses of 2003 33
2.03 ORTHOGRAPHICPROJECTIONMAP OFTHEECLIPSE PATH

Figure 2.1 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-like symbol. The sub-solar point (Sun in zenith) at that instant is also shown.

The limits of the Moon's penumbral shadow define the region of visibility of the partial eclipse. This

saddle shaped region often covers more than half of Earth's daylight hemisphere and consists of several distinct

zones or limits. At the northern 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/ends at sunrise and sunset,

respectively. Bisecting the 'eclipse begins/ends at sunrise and sunset' loops is the curve of maximum eclipse at

sunrise (western loop) and sunset (eastern loop). The exterior tangency points P1 and P4 mark the coordinates

where the penumbral shadow first contacts (partial eclipse begins) and last contacts (partial eclipse ends) Earth's

surface. The path of the umbral shadow bisects the penumbral path from west to east and is shaded dark gray.

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 Universal Time (UT), and generally run in a north-south direction. The outline

of the umbral shadow is plotted every ten minutes in UT. Curves of constant eclipse magnitude 3 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 northern penumbral limit and the umbral path of total eclipse. The southern limit of the penumbra may be thought of as a

curve of constant magnitude of 0%, while adjacent curves are for magnitudes of 20%, 40%, 60% and 80%. The

northern and southern limits of the path of total eclipse are curves of constant magnitude of 100%.

At the top of Figure 2.1, the Universal Time of geocentric conjunction between the Moon and Sun is

given followed by the instant of greatest eclipse. The eclipse magnitude is given for greatest eclipse. For central

eclipses (both total and annular), 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. The shadow axis passes south of Earth's geocenter for negative values of Gamma. Finally, the Saros series

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

2.04 STEREOGRAPHIC MAP OF THE NOVEMBER 23 ECLIPSE PATH

The stereographic projection of Earth in Figure 2.2 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 20 ° increments. The region of penumbral or partial eclipse is identified by its northern 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 20%, 40%, 60% and 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 2.1 and 2.2 may be used to quickly determine the approximate time and magnitude of maximum

eclipse at any location within the eclipse path.

3 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 may be expressed as either a percentage or a decimal fraction (e.g.:

50% or 0.50).

34 Annular and Total Solar Eclipses of 2003
2.05 DETAILED MAP OF THE PATH OF TOTALITY

The path of totality is plotted on a detailed map appearing in Figures 2.3. The map uses coastline data

from the World Data Bank II (WDBII). The WDBII outline files are digitized from navigational charts to a

working scale of approximately 1:3 million. Major scientific research stations are plotted to show their relative

positions with respect to the path of totality. Only three of the several dozen stations actually lie within the track

of total eclipse: Mirny, Novolazarevskaya, and Maitri. Local circumstances have been calculated for the research

stations and can be found in Table 2.6.

Although no corrections have been made for center of figure or lunar limb profile, they have little or no

effect at this scale. Altmospheric refraction 4 has not been included because it depends on the atmospheric temperature-pressure profile, which cannot be predicted in advance. These maps are also available on the web at

http ://sunearth.gsfc.nasa.gov/eclipse/TSE2OO3/TSE2003. html.

2.06 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 2.1. 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 for 1984 and thereafter. 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 IAU convention through the use of a smaller constant for the mean lunar radius k for all umbral contacts (see: LUNARLIMB

PROFILE).Times are expressed in either Terrestrial Dynamical Time (TDT) or in Universal Time (UT), where the

best value of AT5 available at the time of preparation is used.

From the polynomial form of the Besselian elements, any element can be evaluated for any time tj (in

decimal hours) via the equation:

a = a0 + a_*t + a2*t 2 + a3*t3 (or a = Y_[an*t°]; n = 0 to 3)

where: a = x, y, d, 1_,12, or

t = t_ - to (decimal hours) and t o = 23.00 TDT

The polynomial Besselian elements were derived from a least-squares fit to elements rigorously calculated at

five separate times over a six hour period centered at t0.Thus, the equation and elements are valid over the period

20.00 < t_ < 02.00 TDT (Nov 23 to Nov 24).

4 The nominal value for atmospheric refraction at the horizon is 34 arc-minutes, but this value can vary by a

factor or 2 depending on atmospheric conditions. For an eclipse in the horizon, the umbral path is shifted in the

direction opposite from the Sun.

5 AT is the difference between Terrestrial Dynamical Time and Universal Time.

Annular and Total Solar Eclipses of 2003 35
Table2.2listsall externalandinternalcontactsof penumbralandumbralshadowswithEarth.They

includeTDTtimesandgeodeticoordinateswithandwithoutcorrectionsfor AT. 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.

(umbral 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.

(umbral eclipse ends)

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

umbra's central line are given. The IAU (International Astronomical Union) 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 two minute intervals in Universal Time in Table 2.3.

Coordinates of the northern limit, the southern limit and the central line are listed to the nearest tenth of an

arc-minute (~ 185 m at the Equator). The Sun's altitude, path width and umbral duration are calculated for the

central line position. Table 2.4 presents a physical ephemeris for the umbral shadow at two minute intervals in

UT. The central line coordinates are followed by the topocentric ratio of the apparent diameters of the Moon

and Sun, the eclipse obscuration 6, 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 2.3 and 2.4 are presented in Table

2.5. 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

Second Contact

Third Contact

Fourth Contact

-- Instant of first external tangency between the Moon and Sun.

(partial eclipse begins)

-- Instant of first internal tangency between the Moon and Sun.

(central or umbral eclipse begins; total or annular eclipse begins)

-- Instant of last internal tangency between the Moon and Sun.

(central or umbral eclipse ends; total or annular eclipse ends)

-- Instant of last external tangency between the Moon and Sun.

(partial eclipse ends)

The position angles P and V identify the point along the Sun's disk where each contact Occurs 7. Second and

third contact altitudes are omitted since they are always within 1° of the altitude at maximum eclipse.

6 Eclipse obscuration is defined as the fraction of the Sun's surface area occulted by the Moon.

7 p is defined as the contact angle measured counter-clockwise from the north point of the Sun's disk.

V is defined as the contact angle measured counter-clockwise from the zenith point of the Sun's disk.

36 Annular and Total Solar Eclipses of 2003
2.07 LOCAL CIRCUMSTANCES TABLES FOR NOVEMBER 23

Local circumstances for -140 cities and locations in Antarctica, Australia, New Zealand and South

America are presented in Tables 2.6 through 2.10. These tables give the local circumstances at each contact and

at maximum eclipse 8 for every location. The coordinates are listed along with the location's elevation (meters)

above sea-level, if known. 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 counter-clockwise (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 total

eclipses, 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 - abs(x/R) [2.1 ]

where: u = umbral depth

x = perpendicular distance from the shadow axis (kilometers)

R = radius of the umbral shadow as it intersects Earth's surface (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) la seconds [2.2]

where: D = duration of totality on the central line (seconds)

d = duration of totality at location (seconds)

u = 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.

The geographic coordinates of cities are from The New International Atlas (Rand McNally, 1991).

Coordinates in Antarctica are from www.scar.org/Antarctic%20Info/wintering_stations_2000.htm. The city names

and spellings presented here are for location purposes only and are not meant to be authoritative. They do not

imply recognition of status of any location by the United States Government.

8For 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.

Annular and Total Solar Eclipses of 2003 37
2.08 LUNAR LIMB PROFILE FOR NOVEMaEa 23

Eclipse contact times, magnitude and duration of totality all depend on the angular diameters and relative velocities of the Moon and Sun. 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 rather 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 if 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' 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' 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. Additional work by Morrison and Appleby [1981] shows that the

radius of the datum varies with libration producing systematic errors in Watts' original limb profile heights that

attain 0.4 arc-seconds at some position angles. Thus, corrections to Watts' limb data are necessary to ensure that

the reference datum is a sphere with its center at the center of mass.

The Watts charts have been digitized and may be used to generate limb profiles for any libration. Ellipticity and libration corrections can 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.

The lunar limb profile in Figure 2.5 includes corrections for center of mass and ellipticity [Morrison and

Appleby, 1981 ]. It is generated for the central line at 22:40 UT which is close to Russia's Mirny research base.

The Moon's topocentric libration (physical + optical) is 1=+0.21 ° b=+0.29 °, and the topocentric semi-diameters

of the Sun and Moon are 971.8 and 1008.4 arc-seconds, respectively. The Moon's angular velocity with respect

to the Sun is 0.632 arc-seconds per second.

The radial scale of the limb profile (bottom of Figure 2.5) 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' original data is shown (dashed) along with the mean limb with respect to the center of mass (solid). 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 along with 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 center line at 22:40 UT while the times of the four eclipse contacts at that location appear to the lower right.

Directly below the 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/southern limit axis is

PA(N.Limit) and the angular velocity of the Moon with respect to the Sun is A. VeI.(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 2.4, the Sun's limb can be represented as an

epicyclic curve that is tangent to the mean lunar limb at the point of contact. Using the digitized Watts' datum, an

analytical solution is straightforward and robust. Curves of corrections to the times of second and third contact

for most position angles have been computer generated and plotted. 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

38 Annular and Total Solar Eclipses of 2003
thisscalegraphicallyillustratesthetimecorrectiontothemeanpredictionsfor anypositionangleasaresultof

theMoon'struelimbprofile.Timecorrectionsexternalto thecircularscaleareaddedtothemeancontacttime;

timecorrectionsinternaltotheprotractoraresubtractedfromthemeancontacttime.Themagnitudeofthetime

correctionatagivenpositionangleismeasuredusinganyofthefourradialscalesplottedateachcardinalpoint.

Forexample,Table2.6givesthefollowingdatafortheAntarcticbaseMirny:

SecondContact = 22:37:37.0UT P2=117°

ThirdContact = 22:39:30.7UT P3=283°

UsingFigure18,themeasuredtimecorrectionsandtheresultingcontacttimesare:

C2=+0.5seconds; SecondContact = 22:37:37.0+0.5s = 22:37:37.5UT

C3=-4.3seconds; ThirdContact = 22:39:30.7-4.3s = 22:39:26.4UT

Theabovecorrectedvaluesarewithin0.1secondsof arigorouscalculationusingthetruelimbprofile.

2.09 SKY DURINGTOTALITY

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 2003, the Sun is in northern Scorpius near the border with Libra. From

Antarctica, three naked eye planets and a number of bright stars will be above the horizon within the umbral

path. Figure 2.5 depicts the appearance of the sky during totality as seen from the central line at 22:40 UT. This

is close to Russia's Mirny research base, where the early morning eclipse occurs low in the southeastern sky.

The most conspicuous planet visible during totality will be Venus (mv=-3.8) located 25 ° east of the Sun

in Ophiuchus. Mercury (mv=-0.4) lies between the Sun and Venus at a solar elongation of 16° east. Jupiter (m=-

1.8) is over a magnitude brighter than Mercury but it will be located in Leo in the northeastern sky 75 ° away

from the Sun. From the central line at 22:40 UT, Venus, Mercury and Jupiter will have altitudes above the

horizon of 9.4 °, 12.6 ° and 12.7 °, respectively. For comparison, the Sun's altitude will be 14°. Saturn and Mars

are both be below the horizon.

A number of the bright stars may also be visible it the twilight sky during the total eclipse. Antares

(mv=+1.06) is 10° southeast of the Sun. The great southern stars Alpha (my=+0.14) and Beta (my=+0.58) Centauri

are high in the sky about 44 ° from the Sun. Canopus is near the zenith about 100 ° away and Achernar (m =+0.45)

stands high in the southwest. Sirius (mv=- 1.44) and the bright stars of Orion lie in the northwest quadrant of the

sky. It should be noted that star visibility requires a very dark and cloud free sky during totality.

The following ephemeris [using Bretagnon and Simon, 1986] gives the 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 oi' angle between the Sun and planet.

Annular and Total Solar Eclipses of 2003 39
Ephemeris:2003Nov 23 23:00:00UT Equinox--MeanDate

App. Apparent

Planet RA Declination Delta Mag. Diameter Phase

t*

Sun 15h56m25s -20024'28 '' 0.98745 -26.7 1943.7

Moon 15h55m35s -21°22'40" 0.00239 2009.3 0.00

Mercury 17h04m34s -25003'35 '. 1.28941 -0.4 5.2 0.89

Venus 17h43m08s -24032'35 '. 1.49229 -3.8 11.2 0.91

Mars 23h16m20s -05057'46 '' 0.79238 -0.6 11.8 0.87

Jupiter 1 lhl lm23s +06020'50 '' 5.56825 -1.8 35.4 0.99

Saturn 6h53m56s +22008'25 '' 8.26635 +0.1 20.1 1.00

Solar

Elong

o

1.0W

16.4E

25.0E

106.4E

74.9W

138.8W

2.10 INTRODUCTION TO WEATHER PaOSPECTS FOR NOVEMBER 23

This will probably be the first eclipse to be systematically observed from Antarctica - the coldest, windiest, highest and driest place on the Earth. The meteorology is simple because it is dominated by one factor: cold.

Cold air forms in the center of the Antarctic Plateau, close to the south pole, and flows outward to the margins of

the continent. The flow is primarily katabatic, driven by gravity as the heavy frigid air moves downhill toward

the sea. Where the terrain funnels and confines this steady flow, wind speeds reach exceptional values, among

the strongest ever recorded.

Weather stations are isolated and mostly confined to the shores. Inland, automatic stations measure a

small selection of tbe possible variables: wind, temperature, pressure but not cloud cover, humidity, visibility or

precipitation. It doesn't matter much - in the cold air absolute humidities are always low and precipitation is

sparse. Data are often missing and frequently suspect. The length of the climatological record is short so that the

statistics represent more "what is possible or typical" rather than give a serious account of the average conditions.

On the coast and at a very few inland locations, humans supplement the machine measurements, and the

full suite of observations is available. For the eclipse observer, cloud cover is usually paramount, but in the

extremes of the White Continent, temperature, wind and wind chill demand the attention of eclipse planners far

more than in any other location in the world. While Mongolia and Siberia offered the possibility of extreme cold

in the 1997 eclipse, Antarctica in 2003 virtually guarantees it.

The eclipse track is not forgiving, and there are only four venues from which it can be realistically

observed. Two of these are at coastal locations, one near the Russian base at Mirny and the other near the western

limit of the eclipse where a collection of German, Indian, Japanese and Russian bases congregate. The third site

is "inland", at whatever point adventure and finances can take an eclipse expedition. The fourth possibility is

aboard an icebreaker at sea or near the coast along the sunrise portion of the path.

2.11 WEATHER PATTERNS

Antarctic winds flow outward from a cold high pressure system overlying the continent, turning gradually toward the west as they approach the coast. Descending from the 3000 meter mid-continent plateau, the air

is dried even farther, bringing bright sunny skies to the continental margins. In some regions the winds are

exceptionally strong - over 100 km/h - as the local topography squeezes and redirects them. Blizzards and

blowing snow are common in such circumstances.

As the cold outflow moves over the relatively warm waters surrounding the continent, the air is rapidly

saturated with moisture. Clouds form quickly bringing snow showers to the coastal regions and oftshore ice

fields. The wind shear along the edges of the cold air outbreaks and the strong temperature contrast between air

and water helps to create a continuous supply of small scale lows along the coast.

40 Annular and Total Solar Eclipses of 2003
Fartheroffshore,thesoutheastwindsflowingoff of thecontinentgraduallyabateandthewesterly

globalflowassertsitself.Thischangeinwinddirectioncreatesazoneof intenselow-pressuredevelopment. The

lowsthatformtendtotraveleastandsouthward, graduallymovingtowardtheAntarcticcoastwheretheyweaken

anddie.Somestrongerlowscanpenetrateintothecontinent,butthesearerare,thoughthelackof observation

andmeasurement makestheexactfrequencyof suchsystemsuncertain.Eventhoughthelow itselfmaybe

confinedtocoastalwaters,thehighercloudsfromsuchsystemscanpenetratewellinland.

Lowsmovingalongthecoasttendto bringonshorewindsastheyapproachandoffshore

southerliesastheydepart.Thefirst pushesmoistair againstthelandandbringsextensivestratiform

cloudinessandcontinuousprecipitation- eitherrain or snow- whilethelatterreinforcesthenormal

cold outflow with its sunnyskiesfrom thecontinentmargins.

Theinteriorof thecontinentoffersaconsiderablymorerelaxedclimatology,notwithstandingthelow

temperatures. Watervaporisinshortsupplyandweathersystemsfromthenorthhavedifficultyscalingthesteep

slopesof thecoast.Unfortunatelyobservationsof cloudcoverarealmostnon-existent incentralAntarctica,and

satelliteobservationsarelimitedbythelackofcontrastbetweentheicysurfaceandthecloudsandthelongpolar

nights.TheRussianbaseatVostokistheonlyoneinthevicinityoftheeclipsetrackthatcanprovideclouddata

buttheirstatisticsareprobablyrepresentativeof theconditionsovermuchof themid-continentportionof the

track.

Temperaturesalongthecoastarerelativelywarmandhavethepotentialto riseabovezero,butthose

inlandaremuchlower.Thecoldestemperaturesarearesultof thelongAntarcticnights,low humidity,high

albedo,lowcloudcoverandhighaltitudeoftheinteriorthatallowsthesurfacetoradiateenergyintospacewith

little interruption.Thewarmesttemperaturesthatarefoundin theinterior-18° C atVostok)area resultof

advectionfromcoastalregions.OntheeclipsetrackthecoldestemperaturestendtobefoundneartheAustralian automaticweatherstationsLGB20andLGB35.Fortunatelysuchtemperaturescomewith muchbetter

prospectsfor clearskies.Sincewarmtemperaturesonthecoastareassociatedwith cloudyweather,falling

temperatureswill bepreferredoneclipsedayasthesebringinthedrierairfromtheinterior.

Thoughwindsinlandareabouthalfthestrengthof thoseonthecoast,thelowertemperaturesinthe

interiordominatethecalculationof windchill tobringvalueswhichcanreachintotheminussixties.Frostbite

canoccurinlessthanfourminutesin suchweather.Whiletheactualtemperaturesareconsiderablywarmer,

observerswill probablywanttolimit theiroutdoorexposurewhilewaitingforthelunarshadow,oratleastmake

suretheyhavesomeshelterfromthewind.

2.12 COAST OF QUEEN MARY LAND m MIRNY

Mirny is the main Russian base in the Antarctic, situated on the coast of Queen Mary Land on a small

peninsula that juts northward into the Davis Sea. Established in 1956, the station has the distinction of being best

placed within the eclipse track, for the central line lies only a few tens of kilometers to the east. The station

buildings, a collection of two-story rectangular blocks topped by various instrument domes, lies on four rocky

outcrops about 20 meters above sea level. South of the station, the land rises to a height of 1500 meters within

100 km. A few small rocky islands lie offshore, but land-fast ice is observable much of the year. The 24-hour

polar day begins on December 10 at Mirny, and so eclipse day will be one with long daylight and a short twilight.

Mirny's weather is governed by strong downslope winds and a high frequency of offshore low pressure

systems. While the blizzard season is receding in November, winds at eclipse time average a brisk 41 km/h

(Table 2.11) with the highest reported value in the past 15 years reaching over 110 km/h. Temperatures are

modest by Antarctic standards, with an average of-7°C and a range from minus 20 to the freezing point at eclipse

time. The high winds bring a significant wind chill to the station however, and eclipse observers will have to

dress accordingly. By Canadian and north European winter standards, the average eclipse-day conditions at

Mirny appear to be relatively tolerable though the wind speeds are higher than is typical of the Earth's northern

hemisphere.

Cloud cover at Mimy averages 6.4 tenths, a large value when compared with opportunities at past eclipses

but comparable to the other coastal stations on and near the track. The distribution of cloudiness is a typical Ushape (Figure 2.5), with a high frequencies of low and high cloudiness and smaller frequencies of intervening

Annular and Total Solar Eclipses of 2003 41
values.If wemaketheassumptionthattheprobabilityof seeingtheeclipseisproportionaltothefrequencyof

thevariouslevelsof cloudcover,thenMimy offersa36%chanceof asuccessful expedition.Thisisslightly

optimisticasnoaccounthasbeentakenof thelow 13° altitudeof theSun.

Low-pressuredisturbancesmovingtowardthestationcanbringheavycloudsandprecipitationfor severaldaysinarowbutNovemberisapproachingthedriestmonthsof theyearandthesearerelativelyuncommon.

Eclipseobserverswill belookingfor southerlykatabaticwindsblowingfromthehighplateau,for suchwinds

bringdrycoldairandclearskies.Suchwindsaremorefrequentintheeveningandovernight,whichfavorsthe

sunsetportionof theeclipsetrackratherthanthemorningportionatMirny.Thewindspeediscriticalhowever,

for evenunderclearskies,blizzardconditionscandevelopif windsaretoostrong- anythingabove35krn/h

bringspoorvisibility andblowingsnow.Heavysnowis rareduringthesummermonthsfrom Novemberto

February.Fogandicecrystalhazearerareatanytime.

2.13 INTERIOROFANTARCTICA

Whilehumanobservationsareinlimitedsupply,severalautomaticweatherstationsliewithinthetrack

of theeclipseandcanprovidetemperatureandwindinformation.Thesestations,LGB20,LGB35andLGB59

(Table2.11)showaconsiderablycolderclimatethanthecoastalregions.Thoughwindsarefrequentlylighteron

theinteriorplateau,windchillvaluesarecolderbecauseof thelowerinitialtemperature. Observingfromdistant

inlandsitesalongtheeclipsetrackwill requirespecialcareforequipmentandpeople.

Theinteriorstationshaveashortperiodofrecord- from4 to 10years- andtheclimatologyof the

interiorisonlypoorlyrevealed.ForthethreeAustralianautomaticstations,averagetemperaturesateclipsetime

rangedfrom-28°Cto-33°C.Extremetemperaturesdroppedaslowas-41.5°CatLGB20.Windchillvaluesare

15to 20degreescolderonaverage,reachingbelow-60°CatLGB20.At LGB20andLGB35,windspeedsare

relativelylow,abouthalfof thoseatLGB59.Theexplanationlikelyliesintheconfigurationof thesurrounding

terrain.TheprevailingwinddirectionatLGB59isalsoat oddswithmostof theotherinteriorstations,being

northerlyratherthanthemoretypicalsoutherlyoutflow.

ForcloudcoverstatisticsweareforcedtorelyonthedatacollectedatVostok,whichliesconsiderably

fartherinlandandatahigheraltitude.Hereweseeacompletereversalof thecloudpatternsof thecoast,with

clearskiesbeingthemostfrequentreport.Themeancloudinessof3.4tenthsisnearlyhalfthatof Mirny,andthe

probabilityof seeingtheeclipserisesto66%.Whileinlandsitesonthetrackareprobablynotquitethisfavorable,theimplicationscannotbeignored- forthiseclipse,inlandareasaremostlikelyto seetheeventby a

considerablemargin.

Theimpactof frontalcloudinessandweathersystemsismutedbydistancefromtheoceansandthehigh

altitudeof theinterior.Mostof thecloudsareat midandhighlevelswhere,beingcomposedentirelyof ice

crystals,theyarefrequentlysemi-transparent. Thisimpliesthattheprobabilityof seeingtheeclipseisgreater

thantheformalcalculation(66%)wouldsuggest.

Theatmospherictransparencyof inlandAntarcticais legendary.Theairisunpollutedexceptfor occasionalwatervaporandicecrystals.Snowstormsarerareandtendtobeataminimuminthespring.Duringcalm

andclearweather,icecrystalsarefrequent,bringingahazyskyandoccasional icefog.Bothofthesephenomena

aremorelikelyin winterthansummerbuttheirmaineffectontheeclipsewill beto produceahaloaroundthe

sun.Driftingsnowiscommon,occurringonnearlyonethirdof thedaysatVostok.

2.14 COAST OF QUEEN MAUD LAND -- MAITRI, NEUMAYER, AND NOVOLAZAREVSKAJA

The eclipse track comes to an end just beyond Antarctica's coast and the solar altitude is very low for

observation sites in this area. The Russian base Novolazarevskaja and the near-by Indian base at Maitri are the

two stations within the path, and yon Neumayer (Germany) lies just to the west. Maitri and Novolazarevskaja,

four kilometers apart, are situated on the rocky ground of the Schirmacher oasis, a group of low-lying hills

interspersed with many glacial lakes. Neumayer lies on a flat ice shelf in Atka Bay, buried beneath the snow and

ice. Those with an urge to see the station first hand can go to http://www.awi-bremerhaven.de/NM_WebCam/

42 Annular and Total Solar Eclipses of 2003
for hourlyphotographsfromtheirwebcam.Thesestationsare80to 100kilometersfromopenwaterbecauseof

thepresenceof theiceshelfatthefootof thecontinent.

Temperature, windchillandwindstatisticsforthesunsetstationsaresimilartothoseatMirnybutcloud

statisticsaremorevariable.Neumayerisoneof thegrayestlocationsonthetrackwithanaveragecloudinessof

7.6tenths.Novolazarevskajaaverages5.7tenthsandMaitri only3.9tenths,aratherdiscordantamountgiven

theirproximitytotheothers.ThereasonforthemuchlowercloudcoveratMaitrimaybeduetolocalconditions

thatfavordownslopewindsortotheshortperiodofrecordthatjusthappenstolie inarelativelysunnytime.A

comparisonof hourlyreportsfromMaitriwiththoseatNovolazarevskajashowsafewlargedifferencesbuta

near-zerobias,sothesecondexplanationwouldseemtobethemostreasonable. Thecloudclimatologyof the

Russianbasewithitslongerperiodofrecordseemstobemorereliablefor planningpurposes.

Withthisinmind,cloudinesspatternsalongtheeclipsesunsetcoastaresimilartothoseatMirny(Figure

2.5).Mostofthecloudisatmidandhighlevels,afactorthatdoesnotaugurwellforsuchalowaltitudeeclipse.

Theformalprobabilityof seeingtheeclipseis calculatedto bebetween27and52percent,with the44%at

Novolazarevskajabeingthemostrepresentativefigure.Thesemustberegardedastoolargeinviewof thevery

lowangletowardtheeclipse.

2.15 SELECTING A SITE

Antarctic eclipse adventurers are likely to have little choice in their selection of an observing site, as

most travel will be to existing bases. Most sites offer some alternative locations relatively nearby: at

Novolazarevskaja the airport is 15 km inland from the base, and most other sites have inland and upland scientific bases. Where movement is possible, it is best to look for a spot where the southeast katabatic winds are most

favored, in the northwest lee of a plateau for instance.

In interior regions, site selection will be more versatile, as almost all access will be by plane. Flat vistas

where the winds are lightest should be easy to locate - a high spot might even be best, as winds will tend to flow

downhill and away. Satellite imagery (most big bases have it) can be used to predict cloud motion and help select

a site with a high prospect of clear skies.

The interior offers the best chances and the biggest challenges. Prospects for clear skies are twice those

of the coast, depending on the distance and altitude at the site. Coastal regions offer more comfort and easier

access, but at the expense of a high cloud frequency. Mirny seems to be the best lowland site, in large part

because of the higher Sun. Observers there should attempt to move as far inland as possible to take advantage of

the better weather away from the coast.

2.16 - WEATHER WEB SITES FOR NOVEMBER 23 TOTAL ECLIPSE

World --

1. http://www.tvweather.com - Links to current and past weather and climate around the world

2. http://www.worldclimate.com/climate/index.htm - World data base of temperature and rainfall

3. http://www.accuweather.com - Forecasts for many cities worldwide

4. http://www.worldweather.org/A site operated by the World Meteorological Organization with links to the

climate and meteorological data worldwide. This site is still being developed and in many instances only climate

information is available.

5. http://www.fnoc.navy.mil/PUBLIC/WXMAP/index.html - U.S. Navy weather center (Fleet Numerical Meteorology and Oceanographic Center - FNMOC). This site provides several (3) model outputs for many areas of

the globe. While complex to use (meteorological expertise is a real bonus), it contains a wealth of model data.

Look for relative humidity forecasts for 700 hPa (hectoPascals) - this is a mid-level of the atmosphere and the

relative humidity forecasts provide an indication of the forecast cloud cover from larger weather systems. Use

the 70% contour as the outline of cloud areas. Areas with 90% or greater will likely have precipitation. Model

forecasts for six days in advance for many parts of the world are available.

Annular and Total Solar Eclipses of 2003 43
Antarctica m

1. http://weather.uwyo.edu/- An impressive site at the University of Wyoming that allows you to build your own

numerical model output. Choose "Forecasts from Numerical Models" and then "Aviation Model" to be given a

choice of a model output over Antarctica. For coastal Antarctica, choose 700 mb relative humidity. For the

interior of Antarctica choose 500 mb relative humidity. Values above 70% at 700 mb frequently indicate deep

cloudiness but values over 80% are likely required for cloud over the cold dome of Antarctica.

2. http://www.people.fas.harvard.edu/-dbaron/sat/comp/ - Latest composite (assembled from several satellite

passes over several hours) over Antarctica. Choose "Antarctica Composite Images" and select from available

links. Because of the low latitude of the continent, there are frequently holes in the coverage, but eclipse areas

are usually well shown. A Japanese mirror site provides animated views but the speed of animation is very quick

and requires careful orientation and study.

3. http://uwamrc.ssec.wisc.edu/amrchome.html - The Antarctic Meteorology Research Centre. This

site provides links to polar orbiting satellite imagery and current weather observations.

44 Annular and Total Solar Eclipses of 2003
Total Solar Eclipse of 2003 Nov 23

FIGURE 2.1 - ORTHOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH

Geocentric Conjunction = 23:20:14.6 UT

Greatest Eclipse = 22:49:16.7 UT

Sun at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 15h56m23.2s

Dec. = -20024'22.9 ''

S.D. = 00°16'11.8"

H.P. = 00000'08.9 ''

Eclipse Magnitude = 1.03788

Saros Series = 152 Member = 12 of 70

N

I

J.D. = 2452967.472391

J.D. = 2452967.450887

Gamma =-0.96381

Moon at Greatest Eclipse

(Geocentric Coordinates)

R.A. = 15h55m07.5s

Dec.=-21020'45.7 ''

S.D.= 00°16'44.8 ''

H.P. = 01001'27.3 ''

W -E

External/Internal

Contacts of Penumbra

P1 = 20:46:04.9 UT

P4 = 00:52:15.3 UT

Ephemeris & Constants

Eph. = DE200/LE200

AT = 65.0 s

kl = 0.2725076

k2 = 0.2722810

Ab= 0.0" AI= 0.0"

I

S

Local Circumstances at Greatest Eclipse

Lat. = 72°40.0'S Sun Alt. = 14.9 °

Long. = 088°23.5'E Sun Azm. = 111.2 °

Path Width = 495.5 km Duration = 01m57.3s

I [ i i i [ _ _ i [ i i [ [ J i i [ I I I [

0 1000 2000 3000 4000 5000

Kilometers

NASA 2003 Eclipse Bulletin (F. Espenak & J. Anderson)

sunearth.gsfc.nasa.gov/eclipse/eclipse.html

External/Internal

Contacts of Umbra

U1 = 22:19:20.6 UT

U2 = 22:26:26.2 UT

U3 = 23:11:46.8 UT

U4 = 23:18:52.7 UT

Geocentric Libration

(Optical + Physical)

l = 0.01 °

b= 1.28 °

c = 10.41 °

Brown Lun. No. = 1001

Annular and Total Solar Eclipses of 2003 45
O_

>

_z

©

©

_O

O

L_

100 _ E

• /

• / •

14_ E

+

Total Solar Eclipse of 2003 November 23

FIGURE 2.2 - STEREOGRAPHIC PROJECTION MAP OF THE ECLIPSE PATH

!

I L_L__l I I I IIJ__

- 0 1000 2000 3000 4000

Kilometers

IGO ° W

[ • •

l

\ \

NASA 2003 Eclipse Bulletin (F. E.spenak & J. Anderson)

"\

\\

/

i

i

i

!

i

/

/ /

i /

,i

\

\

\\

/

/

!

/

,/

/

/
>

E

o

m

o

bo

O

O

L.O

4_

-,-J

Total Solar Eclipse of 2003 November 23

FIGURE 2.3 - THE ECLIPSE PATH THROUGH ANTARCTICA

, . 180_ . _ . ._

:_ '_ _,,_ L I I I I I

0 500

Dumont d'Urville

III III I III I i I I

1000 1500 2000

Kilometers

22:25 UT

01 m43s

6°

22:30 UT

01 m49s

10 °

Davis

Molodezhnaya

23:00 UT

01 m55s

14°

23:10 UT

01 m48s

9°

23:15 UT

01 m38s

3 °

Maitri ISANAEIV

• Maximum Ectipse at Sul , _.,

San Martin
Total Solar Eclipse of 2003 November 23

FIGURE 2.4 - LUNAR LIMB PROFILE FOR NOV 23 AT 22:40 UT

Sun at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 15h56m21.8s

Dec. = -20024 ' 10.1"

S.D. = 00°16'11.8"

H.P. = 00000'08.9 ''

090

\

Second Contact

Correction Curve

\

\

Contact Time

Correction

Scale

10-1-2

Seconds

Moon/Sun Ratio = 1.0376

N

Third Contact

Time Correction Curve

\

\

\

\

Contact Time

Correction

Scale

\

\

\

-3

\

Moon at Maximum Eclipse

(Topocentric Coordinates)

R.A. = 15h56m21.6s

Dec. = -20024'06.7 ''

S.D. = 00016'48.4 ''

H.P. = 01001'43.3 ''

\

\

\

\

\

\

True Limb

Mean Limb

(Centerof Figure)

Mean Limb

(Centerof Mass)

Geographic Position

Name = Center Line at 22:40 UT

Lat. = 67°30'45.6"S

Long. = 093°28'29.5"E

Elev. = 0.0 m

Ephemeris & Constants

Eph. = DE200/LE200

AT = 64.8 s

kl = 0.2725076

k2 = 0.2722810

Ab= 0.00" AI= 0.00"

Local Circumstances at Maximum Eclipse

Sun Alt. = 14.0 ° Path Width = 516.5 km

Sun Azm. = 109.9 ° Duration = 01m55.6s

PA(N.Limit) = 19.8 ° A.Vel. (M:S) = 0.632"/s

Ii III Ill I i I

0 1 2 3 4 5

Arc-Seconds

I _ I i I i J i I J J

0 1 2 3 4 5

Seconds

cor.C2 = 22:39:01.9 UT (-0.3s) cor.C3 = 22:40:54.2 UT

NASA 2003 Eclipse Bulletin (F. Espenak & J. Anderson)

Eclipse Contacts

C1 = 21:48:32.5 UT

C2 = 22:39:02.2 UT

C3 = 22:40:57.9 UT

C4 = 23:33:06.7 UT

AC2 = -0.3s AC3 = -3.7s

Topocentric Libration

(Optical + Physical)

1= 0.21 °

b = 0.29 °

c = 10.31 °

(-3.7s)

48 Annular and Total Solar Eclipses of 2003
Total Solar Eclipse of 2003 November 23

FIGURE 2.5 - SKY DURING TOTALITY AS SEEN FROM CENTRAL LINE AT 22:40 UT

E

2003 Nov 23

GMT = 22:40

LST = 09:03

N

I

/

/

!

/

/o Spica

/

/

/

i / ,

I

un i

\

\ • Antares

\ •

Crux

BetaCen

AlphaCen

• /

"" /

• /

Central Line at 22;40 UT I

Lat = 67°31'S

Long = 093°28'E

Zone = 0.0 hours

\

\

\

--W

• Fomalhaut *

f

Magnitude Limit: mv= 2.5 S NASA 2003 Eclipse Bulletin (F. Espenak & J. Anderson

The sky during totality as seen from the central line in Antarctica at 22:40 UT. The most

conspicuous planets visible during the total eclipse will be Venus (m v=-3.8), Mercury

(mv=-0.4) and Jupiter (mv=-l.8) located 25 ° east, 16 ° east and 75 ° west of the Sun,

respectively. Bright stars which might be visible include Antares (m v=+l.06), Alpha

(mv=+0.14) and Beta (my=+0.58) Centauri, Canopus (mv=-0.62), Achernar (mv=+0.45) and

Sirius (mv=-l.44).

http://sunearth.gsfc.nasa.govleclipse/TSE2OO3/TSE2OO3html

Annular and Total Solar Eclipses of 2003 49
Figure 2.6 - Cloud Statistics for Three Stations

for the Total Solar Eclipse of 2003 Nov 23

>.

0J

(:I"

oJ

u_

(D

Mirny

clear 1 2 3 4 5 6 7 overcast

Cloud Amount in Octas (eighths)

t0)

uI19

t.)

0A

Q..

45

40

35

30

25

20

15

10

5

0

c_ear

Vostok

1 2 3 4 5 6 7 overcast

Cloud Amount in Octas (eighths)

e-

(2)

o0A

t_

45

35

30

25

Novolazarevskaja

clear 1 2 3 4 5 6 7 overcast

Cloud Amount in Octas (eighths)

These graphs show the frequency of various cloud amounts at selected stations within or near the eclipse path.

At Mirny and Novolazarevskaja the distribution has a "U" shape, with higher values at low and high cloudiness.

This is typical of most cloud distributions around the globe. At Vostok the distribution is more one-sided, with clear

skies having the highest frequency. The sites chosen reflect the coastal and inland cloud climatologies along the track.

Data are taken from the archives of the British Antarctic Society.

50 Annular and Total Solar Eclipses of 2003
TABLE 2.1

ELEMENTS OF THE TOTAL SOLAR ECLIPSE OF 2003 NOVEMBER 23

Geocentric Conjunction

of Sun & Moon in R.A.:

Instant of

Greatest Eclipse:

23:21:19.59 TDT

(=23:20:14.79 UT)

22:50:21.65 TDT

(=22:49:16.85 UT)

J.D. = 2452967.473143

J.D. = 2452967.451639

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

Sun: R.A. = 15h56m23.195s

Dec. =-20o24'22.85 ''

Semi-Diameter = 16'11.82"

Eq. Hor. Par. = 08.91"

A R.A. = i0.562s/h

A Dec. = -30.99"/h

Moon: R.A. = 15h55m07.521s

Dec. =-21°20'45.70 "

Semi-Diameter = 16'44.76"

Eq. Hor. Par. = 1°01'27.25 ''

A R.A. = 157.138s/h

A Dec. = -673.37"/h

Lunar Radius

Constants:

kl = 0.2725076 (Penumbra)

k2 = 0.2722810 (Umbra)

Shift in Ab = 0.00"

Lunar Position: A1 = 0.00"

Geocentric Libration:

(Optical + Physical)

1 = 0.0 °

b = 1.3 °

c = 10.3 °

Brown Lun. No. = i001

Saros Series = 152 (12/70)

Ephemeris = (DE200/LE200)

Eclipse Maqnitude = 1.03788 Gamma =-0.96381 AT = 64.8 s

Polynomial Besselian Elements for: 2003 Nov 23 23:00:00.0 TDT (=t O )

n x y d 11 12

0 -0.1979529 -0.9479029-20.4053841 0.5373482 -0.0087654 168.398682

1 0.5568983 -0.1739249 -0.0081768 -0.0000032 -0.0000032 14.998531

2 0.0000570 0.0001989 0.0000050 -0.0000131 -0.0000130 -0.000003

3 -0.0000094 0.0000031 0.0000000 0.0000000 0.0000000 0.000000

Tan /i = 0.0047348 Tan /2 = 0.0047112

At time 't I' (decimal hours), each Besselian element is evaluated by:

a = a 0 + al*t + a2*t 2 + a3*t 3 (or a = _ [an*tn] ; n = 0 to 3)

where: a = x, y, d, 1 I, 12 , or

t = t I - t O (decimal hours) and t O = 23.000 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

t O . Thus the elements are valid over the period 20.00 _ t I _ 02.00 TDT (Nov

23 to Nov 24).

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

Saros Series 152: Member 12 of 70 eclipses in series.

Annular and Total Solar Eclipses of 2003 51
TABLE 2.2

SHADOW CONTACTS AND CIRCUMSTANCES

TOTAL SOLAR ECLIPSE OF 2003 NOVEMBER 23

AT = 64.8 S

=000°16 '14.7 "

External/Internal

Contacts of Penumbra:

Extreme

North/South Limits

of Penumbral Path:

Terrestrial

Dynamical

Time

h m s

Ephemeris True

Latitude Longitudet Longitude*

P1 20:47:09.9 20°08.9'S 126°58.2'E 127°14.4'E

P4 00:53:20.3 51°16.4'S 079°04.0'W 078°47.8'W

N1 21:10:09.3 07°41.8'S 126°I0.8'E

S1 00:30:23.4 39°47.4'S 082°55.9'W

126°27.1 E

082°39.7 W

External/Internal

Contacts of Umbra:

Extreme

North/South Limits

of Umbral Path:

U1 22:20:25.6 50°59.5'S 084°09.8'E

U2 22:27:31.2 54°07.1'S 078°46.9'E

U3 23 :12 :51 .8 69007 .0 'S 021o11 .7 'E

U4 23:19:57.7 69°34.8'S 008°40.1'E

N1 22:20:31.6 50°55.9'S 084°12.2'E

S1 22:27:26.8 54°09.8'S 078°44.5'E

N2 23:19:51.7 69°34.9'S 008°29.3'E

$2 23:12:56.3 69°06.3'S 021°19.6'E

084°26.0 E

079°03.1'E

021o27 .9 E

008°56.4 E

084°28.4 E

079°00.8 E

008o45 .5 E

021°35.8'E

Extreme Limits

of Central Line: C1 22:23:45.0 52°27.4'S 081°43.3'E

C2 23:16:38.1 69°26.9'S 014°32.8'E

081o59 .5 E

014°49.1 E

Instant of

Greatest Eclipse: GO 22 :50 :21 .7 72o40 .0 'S 088o07 .2 'E 088°23.4 E

Circumstances at

Greatest Eclipse: Sun's Altitude = 14.9 °

Sun's Azimuth = 111.2 °

Path Width = 495.5 km

Central Duration = 01m57.3 s

t 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,AT/240, where AT(in seconds) = TDT UT)

Note: Longitude is measured positive to the East.

Since AT is not known in advance, the value used in the predictions is an

extrapolation based on pre-2003 measurements. Nevertheless, the actual

value is expected to fall within ±0.5 seconds of the estimated AT used here.

52 Annular and Total Solar Eclipses of 2003
TABLE 2.3

PATH OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2003 NOVEMBER 23

Universal Northern Limit Southern Limit Central Line Sun

Time Latitude Ix]ngitude Latitude Lmngitude Latitude Lc_git_de Alt

o

Limits 50°55.9'S 084°28.4'E 54°09.8'S 079°00.8'E 52°27.4'S 081°59.5'E 0

22:24 57°29.2'S 094°55.6'E - - 55°32.6'S 087°36.8'E 5 534

22:26 59°06.0'S 096°23.1'E - - 57°43.2'S 090°14.1'E 7 544

22:28 60°34.4'S 097°26.9'E 57°24.6'S 084°15.8'E 59°27.7'S 091°46.4'E 9 545

Path Central

Width Durat.

km

497 01m33.8s

01m40.7s

01m44.6s

01m47.4s

22:30 61°57.3'S 098°13.7'E 59°27.2'S 086°14.5'E 61°00.4'S 092°46.8'E i0 543 01m49.5s

22:32 63°16.3'S 098°46.9'E 61°07.9'S 087°18.0'E 62°26.1'S 093°25.7'E ii 539 01m51.2s

22:34 64°32.4'S 099°08.2'E 62°37.9'S 087°51.I'E 63°47.0'S 093°47.8'E 12 533 01m52.7s

22:36 65°46.3'S 099°18.4'E 64°01.i'S 088°02.0'E 65°04.2'S 093°55.2'E 13 528 01m53.9s

22:38 66°58.3'S 099°17.8'E 65°19.5'S 087°54.1'E 66°18.7'S 093°48.7'E 13 522 01m54.8s

22:40 68°08.8'S 099°06.2'E 66°34.1'S 087°28.7'E 67°30.8'S 093°28.5'E 14 516 01m55.6s

22:42 69°18.1'S 098°42.8'E 67°45.4'S 086°45.8'E 68°40.8'S 092°54.0'E 14 511 01m56.3s

22:44 70°26.1'S 098°06.5'E 68°53.8'S 085°44.7'E 69°49.0'S 092°04.0'E 15 506 01m56.7s

22:46 71°33.0'S 097°15.6'E 69°59.3'S 084°24.0'E 70°55.4'S 090°57.0'E 15 502 01m57.1s

22:48 72°38.7'S 096°08.0'E 71°01.9'S 082°41.6'E 71°59.8'S 089°30.4'E 15 498 01m57.2s

22:50 73°43.2'S 094°40.6'E 72°01.2'S 080°34.6'E 73°02.2'S 087°41.4'E 15 494 01m57.2s

22:52 74°46.2'S 092°49.6'E 72°56.7'S 077°59.9'E 74°02.0'S 085°26.1'E 15 491 01m57.1s

22:54 75°47.3'S 090°30.I'E 73°47.7'S 074°53.7'E 74°58.8'S 082°39.9'E 15 489 01[[66.8s

22:56 76°46.0'S 087°35.7'E 74°33.0'S 071°12.2'E 75°51.6'S 079°17.4'E 14 487 01m56.4s

22:58 77°41.3'S 083°58.7'E 75°Ii.2'S 066°51.8'E 76°39.4'S 075°12.7'E 14 486 01m55.8s

23:00 78°32.0'S 079°30.0'E 75°40.2'S 061°50.4'E 77°20.4'S 070°20.2'E 14 485 01m55.0s

23:02 79°16.3'S 074°00.5'E 75°57.4'S 056°08.4'E 77°52.6'S 064°36.2'E 13 485 01m54.1s

23:04 79°51.6'S 067°22.9'E 75°59.4'S 049°50.3'E 78°13.2'S 058°00.8'E 12 486 01m52.9s

23:06 80°14.8'S 059°36.4'E 75°41.5'S 043°05.3'E 78°18.6'S 050°41.2'E ii 487 01m51.5s

23:08 80°21.9'S 050°52.3'E 74°56.2'S 036°06.3'E 78°05.0'S 042°53.0'E I0 489 01m49.8s

23:10 80°09.0'S 041°37.0'E 73°26.4'S 029°04.7'E 77°27.2'S 034°58.7'E 9 493

23:12 79°31.7'S 032°28.1'E - 76°17.2'S 027°22.6'E 7 497

23:14 78°25.3'S 024°02.4'E - 74°13.6'S 020°22.7'E 5 502

Limits 69°34.9'S 008°45.5'E 69°06.3'S 021°35.8'E 69°26.9'S 014°49.1'E 0 504

01m47.7s

01m45.0s

01m41.3s

01m33.8s

Annular and Total Solar Eclipses of 2003 53
TABLE 2.4

PHYSICAL EPHEMERIS OF THE UMBRAL SHADOW

TOTAL SOLAR ECLIPSE OF 2003 NOVEMBER 23

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

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

o o km km km km/s

22:22.7 52°27.4'S 081°59.5'E 1.0331 1.0674 0.0 124.9 497.4 - 111.7 - 01m33.8s

22:24 55°32.6'S 087°36.8'E 1.0346 1.0704 4.6 120.0 533.8 - 116.6 3.218 01m40.7s

22:26 57°43.2'S 090° 14.1'E 1.0354 1.0721 7.2 117.3 544.0 969.9 119.2 2.032 01m44.6s

22:28 59°27.7'S 091°46.4'E 1.0360 1.0733 8.9 115.4 545.4 792.0 121.0 1.637 01m47.4s

22:30 61°00.4'S 092°46.8'E 1.0364 1.0742 10.2 113.9 542.9 696.8 122.4 1.435 01m49.5s

22:32 62°26.1'S 093°25.7'E 1.0368 1.0749 11.3 112.7 538.6 636.7 123.5 1.312 01m51.2s

22:34 63°47.0'S 093°47.8'E 1.0370 1.0754 12.1 111.7 533.4 595.4 124.4 1.232 01m52.7s

22:36 65°04.2'S 093°55.2'E 1.0373 1.0759 12.9 110.9 527.7 565.7 125.1 1.178 01m53.9s

22:38 66°18.7'S 093°48.7'E 1.0374 1.0763 13.5 110.3 522.0 543.8 125.7 1.140 01m54.8s

22:40 67°30.8'S 093°28.5'E 1.0376 1.0766 13.9 109.9 516.5 527.5 126.2 1.115 01n155.6s

22:42 68°40.8'S 092°54.0'E 1.0377 1.0768 14.3 109.7 511.2 515.6 126.6 1.098 01m56.3s

22:44 69°49.0'S 092°04.0'E 1.0378 1.0770 14.6 109.7 506.3 507.2 126.8 1.088 01n]56.7s

22:46 70°55.4'S 090°57.0'E 1.0378 1.0771 14.7 ii0.0 501.8 501.8 127.0 1.085 01m57.1s

22:48 71°59.8'S 089°30.4'E 1.0379 1.0772 14.8 110.6 497.8 499.1 127.1 1.087 01m57.2s

22:50 73°02.2,S 087°41.4'E 1.0379 1.0772 14.8 111.5 494.3 499.0 127.1 1.095 01m57.2s

22:52 74°02.0'S 085°26.1'E 1.0379 1.0771 14.8 112.9 491.3 501.4 127.0 1.107 01n_57.1s

22:54 74°58.8'S 082°39.9'E 1.0378 1.0770 14.6 114.8 488.8 506.5 126.9 1.125 01m56.8s

22:56 75°51.6'S 079°17.4'E 1.0377 1.0769 14.3 117.3 486.9 514.6 126.6 1.150 01m56.4s

22:58 76°39.4'S 075°12.7'E 1.0376 1.0766 14.0 120.5 485.6 526.2 126.2 1.181 01m55.8s

23:00 77°20.4'S 070°20.2'E 1.0375 1.0763 13.5 124.5 484.9 542.0 125.8 1.222 01m55.0s

23:02 77°52.6'S 064°36.2'E 1.0373 1.0759 12.9 129.4 484.9 563.2 125.2 1.274 01n154.1s

23:04 78 °13.2'S 058 °00.8'E 1.0371 1.0755 12.2 135.1 485.6 592.0 124.5 1.344 01m52.9s

23:06 78°18.6'S 050°41.2'E 1.0368 1.0749 11.4 141.5 487.1 631.8 123.6 1.438 01nlSI.Ss

23:08 78°05.0'S 042°53.0'E 1.0365 1.0742 10.3 148.5 489.4 689.5 122.5 1.572 01m49.8s

23:10 77°27.2'S 034°58.7'E 1.0360 1.0734 9.0 155.5 492.7 779.7 121.2 1.780 01m47.7s

23:12 76°17.2'S 027°22.6'E 1.0355 1.0723 7.4 162.3 497.1 944.1 119.4 2.160 01m45.0s

23:14 74°13.6'S 020°22.7'E 1.0347 1.0707 5.0 168.5 502.5 - 116.9 3.175 01m41.3s

23:15.6 69°26.9'S 014°49.1'E 1.0331 1.0674 0.0 173.3 504.5 - 111.7 01m33.8s

54 Annular and Total Solar Eclipses of 2003
Central Line

Maximum Eclipse

U.T. Durat. Aft

o

TABLE 2.5

LOCAL CIRCUMSTANCES ON THE CENTRAL LINE

TOTAL SOLAR ECLIPSE OF 2003 NOVEMBER 23

First Contact Second Contact Third Contact

U.T. P V Aft U.T. P V U.T. P V

o o o o o o o

22:24 01[n40.7S 5 - - - 22:23:10 ii0 258 22:24:50 290 78

22:26 01m44.6s 7 21:36:50 289 82 2 22:25:08 ii0 259 22:26:52 290 79

22:28 01m47.4s 9 21:38:18 290 83 4 22:27:06 Ii0 261 22:28:54 290 81

22:30 01m49.5s

22:32 01m51.2s

22:34 01m52.7s

22:36 01[n53.9s

22:38 01m54.8s

22:40 01m55.6s

22:42 01m56.3s

22:44 01m56.7s

22:46 01m57.1s

22:48 01m57.2s

22:50 01m57.2s

22:52 01m57.1s

22:54 01m56.8s

22:56 01m56.4s

22:58 01m55.8s

I0 21:39:52 290 84 5 22:29:05 II0 262 22:30:55 290 82

ii 21:41:31 290 85 6 22:31:04 ii0 263 22:32:56 290 83

12 21:43:13 290 86 7 22:33:04 Ii0 264 22:34:56 290 84

13 21:44:57 289 87 8 22:35:03 ii0 265 22:36:57 290 85

14 21:46:44 289 88 9 22:37:03 ii0 266 22:38:57 290 86

14 21:48:33 289 89 i0 22:39:02 ii0 267 22:40:58 290 87

14 21:50:23 289 90 i0 22:41:02 ii0 268 22:42:58 290 88

15 21:52:15 289 91 ii 22:43:02 109 269 22:44:58 290 89

15 21:54:09 289 92 Ii 22:45:02 109 270 22:46:59 289 90

15 21:56:05 289 93 ii 22:47:01 109 271 22:48:59 289 91

15 21:58:02 289 94 12 22:49:01 109 272 22:50:59 289 92

15 22:00:01 289 95 12 22:51:02 109 273 22:52:59 289 93

15 22:02:01 288 96 12 22:53:02 109 274 22:54:58 289 94

14 22:04:04 288 97 12 22:55:02 108 275 22:56:58 288 95

14 22:06:08 288 98 12 22:57:02 108 276 22:58:58 288 96

14 22:08:14 288 99 ii 22:59:03 108 277 23:00:58 288 97

13 22:10:22 288 I00 Ii 23:01:03 108 278 23:02:57 288 98

12 22:12:33 287 i01 ii 23:03:04 108 279 23:04:56 288 99

ii 22:14:47 287 102 i0 23:05:04 107 280 23:06:56 287 99

I0 22:17:04 287 103 9 23:07:05 107 280 23:08:55 287 i00

9 22:19:25 286 104 8 23:09:06 107 281 23:10:54 287 i01

7 22:21:54 286 105 7 23:11:08 106 282 23:12:53 286 102

5 22:24:36 286 106 5 23:13:09 106 283 23:14:51 286 103

23:00 01m55.0s

23:02 01m54.1s

23:04 01m52.9s

23:06 01m51.5s

23:08 01m49.8s

23:10 01m47.7s

23:12 01m45.0s

23:14 01m41.3s

Fourth Contact

U.T. P V Aft

o o o

23:14:19 ii0 256 ii

23:17:06 iii 257 14

23:19:38 iii 259 15

23:22:02 iii 260 16

23:24:21 IIi 261 17

23:26:37 ii0 263 18

23:28:49 ii0 264 18

23:30:59 ii0 265 19

23:33:07 ii0 266 19

23:35:12 ii0 267 19

23:37:15 ii0 268 19

23:39:17 ii0 269 19

23:41:16 ii0 270 19

23:43:14 109 271 19

23:45:10 109 272 18

23:47:04 109 273 18

23:48:56 109 274 17

23:50:46 109 275 17

23:52:34 108 276 16

23:54:20 108 276 15

23:56:03 108 277 14

23:57:44 108 278 13

23:59:21 107 278 12

00:00:53 107 279 ii

00:02:19 107 279 9

00:03:32 106 280 6

Annular and Total Solar Eclipses of 2003 55
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56 Annular and Total Solar Eclipses of 2003
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Annular and Total Solar Eclipses of 2003 57
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58 Annular and Total Solar Eclipses of 2003
Table 2.11 - Antarctic Station Climatology for the

Total Solar Eclipse of 2003 Nov 23

I I Ave.

Ave. Min. Max. I Wind

POR ' Temp. Temp. Temp. t Chill

Station '(years)' (°C) (°C) --: (°_C)_" . (°C)

von Neumayer , 15_ 1 _-9.8 ,............ -24.3 = 1.0 -17.9

Maitri " : 5 -5.3 -11.9 4.1 -13.2

Min.

Wind

Chill

(oc)

-36.0

-27.0

Most

Ave. Max. Average ' Freqent

Wind Wind Prevail. Cloud Cloud

Speed Speed Wind Cover Cover

(kin/h) ,.-(kin/h) . Direction (tenths_) (te_nths)

29 ' 113._ I E 7.6 _ 10.0

32 : .1_11.... S I 3.9 10.0

Novolazarevskaja* [ 15 I :_7 _:16.3-, 4_.0. [_.-:13.2 . -27._7 ,

Asuka 5 : -14.5 -28.4 I -5.6 _.-26 3.j

Syowa i 4 -7.5 -152 ' -1.4 r -15

ReayStation . 6 ; -41.1 , -50. 6 ! -28_:6 : .-58 3 .

L.G_B_20* _.... [. 9_ _ _-_32.6]__1:5.. "_1_8.._2._ -44._5

LGB10 _ i 6 _ ! "3_2.5 i_ -42.4 ! -17.1 i___2.0 i

GEO3 4 .-22.0 i -31.7 : -11,3 ,-36.6 :

.................... i - -- J

Mawson 15 , -5.9 ' -14.9 _ 5.2 -16 L

LGB35* : 7 _ -27.9 -36.9 i -16.3 ,i -43,2 '

Zho_n_gshan i 4 I -5.3 , -13.1 0 ! -13.4

LGB59" [ .... 4 i_ ........... -28.8 -37.1 ] -18.5 ,

6.4

;

_ , W-SW

-63.3 16 46 S -SW

-59.9 20 50 S - SW

-45.4 . 41 .._ 87 . $_ ,

-29_.6 . _51 -, 139 SE __ 6.1

-58.2 18 ! 56 SE

-26.4 37 130 .i E I 6.1

-57.1 36 61 NE

36 100 E - SE ' 5.7 10.0

-37_.5 i 42 ._. 80 _. SE _

-24.3 ! 27 78 N- NE 8.8

-70.2 , 25 61

- - ; - --; ....... i .........

Davis ' 15 -4.3 -14.3 I 5.6 r -10.4 i -23.8 13 53 E-NE ... 6.6_

Vo§tok .... :_15_ _ -39.5_ _[._-53.7__I -25_.7. - -53.7 : -73._6- , . 17 41 S-SW 3.4

GC46 I 2 ! -40.2 I -53.6 I -31.8 ',-55. 7 ._-73;6 !, 20 i__ 33._! .SE _.

Casey ! _--i-_4.3 [ -13.4 i 5.1 -10.5 -23.6 23 [ 126 E-NE 6.9

10.0

10

8.8

10.0

0.0

8.8

Eclipse

Observin(

Probabilib

(%)

27

52

44

36

39

39

34

37

66

31

indicates stations within the eclipse track

Key to Table 2.11

Data for this table was taken from the archive of the British Antarctic Society. They are based on hourly observations taken

at O0 hour UTC between November 9 and December 9 for a variable number of years.

POR

Period of record, or the length of time in years for which meteorological data are available.

Ave. Tamp,

The mean of the temperatures at 00 UTC between November 9 and December 9 for the period of record, in degrees Celsius.

Many values are missing from Antarctic stations, but most means are based on at least 90 reports.

MIn. Temp.

The lowest temperature (°C) in the data collected during the period of record.

Max. Temp.

The highest temperature (°C) in the data collected during the period of record.

Ave. Wind Chill

Mean wind chill (*C) calculated using the new wind chill formula developed by Environment Canada and U. S. National Weather Service.

The formula can be found at http://windchill.ec.gc.ca.

MIn. Wind Chill

Coldest wind chill - the lowest wind chill value (°C) calculated during the period of record.

Ave. Wind Speed

The mean wind speed (kin/h) for the period of record.

Max. Wind Speed

The greatest wind speed (km/h) for the period of record.

Prevail. Wind Direction

Prevailing wind direction - the most common wind direction or directions in the record.

Average Cloud Cover

Mean cloud amount in tenths in the record. Cloud observations are recorded in octas (eighths); these values are converted from those

records. Obscured conditions are included in the overcast category. These make up only a small percentage of the observations.

Moat Frequent Cloud Cover

The cloud amount that had the highest frequency in the period of record.

Eclipse Observing Probability

The summed product of the cloud amount times its frequency. It assumes that the sun is high (above 45 °) and that all observed cloud

is opaque. It provides a good comparison between observing sites.

Annular and Total Solar Eclipses of 2003 59
3.00 ECLIPSE RESOURCES

3.01 EYE SAFETY AND SOLAR ECLIPSES

B. Ralph Chou, MSc, OD

Associate Professor, School of Optometry, University of Waterloo

Waterloo, Ontario, Canada N2L 3G 1

A solar eclipse offers students a unique opportunity to see a natural phenomenon that illustrates the

basic principles of mathematics and science that are 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 orbital motion 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.

However, observing the Sun can be dangerous if you do not take the proper precautions. The solar

radiation that reaches the surface of the earth includes ultraviolet (UV) radiation at wavelengths longer than 290

nm, to radio waves in the meter range. The tissues in the eye transmit a substantial part of the radiation between

380 and 1400 nm to the light-sensitive retina at the back of the eye. While environmental exposure to UV

radiation is known to contribute to the accelerated aging of the outer layers of the eye and the development of

cataracts, the concern over improper viewing of the Sun during an eclipse is for the development of "eclipse

blindness" or retinal bums.

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 protection for the eyes, this photochemical retinal damage may be accompanied by a thermal injury - the high level of visible light causes heating that literally cooks the exposed tissue.

This thermal injury or photocoagulation destroys the rods and cones, creating a small blind area. The danger to

vision is significant because photic retinal injuries occur without any feeling of pain (the retina has no pain

receptors), and the visual effects do not occur 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 thermal retinal injury because of the high irradiance level due to visible light, as well as near infrared

radiation, 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 Sun. It is never safe to look at an annular eclipse or the partial phases of any

eclipse without theproper equipment and techniques. Even when 99.9% 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, 1996; Marsh,

1982). Failure to use proper observing methods may result in permanent eye damage or severe visual loss. This

can have important adverse effects on career choices and earning potential, since 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).

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 & Covington, 1993; Reynolds

& Sweetsir, 1995). The safest and most inexpensive method is by projection. A pinhole or small opening is used

Annular and Total Solar Eclipses of 2003 61
toformanimageof theSunonascreenplacedaboutameterbehindtheopening.Multipleopeningsinperfboard,

alooselywovenstrawhat,orevenbetweeninterlacedfingerscanbeusedto castapatternof solarimagesona

screen.Asimilareffectisseenonthegroundbelowabroad-leafedtree:themany"pinholes"formedbyoverlappingleavescreateshundredsof crescent-shapedimages.Binocularsorasmalltelescopemountedonatripod

canalsobeusedtoprojectamagnifiedimageoftheSunontoawhitecard.All of thesemethodscanbeusedto

provideasafeviewof thepartialphasesof aneclipsetoagroupof observers,butcaremustbetakento ensure

thatno-onelooksthroughthedevice.Themainadvantageof theprojectionmethodsisthatnobodyislooking

directlyattheSun.Thedisadvantageof thepinholemethodis thatthescreenmustbeplacedatleastameter

behindtheopeningtogetasolarimagethatislargeenoughto seeeasily.

TheSuncanonlybevieweddirectlywhenfiltersspeciallydesignedtoprotectheeyesareused.Mostof

thesefiltershaveathinlayerof chromiumalloyoraluminumdepositedontheirsurfacesthatattenuatesboth

visibleandnear-infraredradiation.A safesolarfiltershouldtransmitlessthan0.003%(density-4.5)_of visible

light(380to 780nm)andnomorethan0.5%(density-2.3)of thenear-infraredradiation(780to 1400nm).

Figure3.1showstransmittancecurvesfor aselectionof safesolarfilters.

Oneof themostwidelyavailablefiltersfor safesolarviewingisshadenumber14welder'sglass,which

canbeobtainedfromweldingsupplyoutlets.Apopularinexpensivealternativeisaluminizedpolyester'-thathas

beenmadespeciallyfor solarobservation.("Spaceblankets"andaluminizedpolyesterusedin gardeningare

NOTsuitableforthispurpose!)Unliketheweldingglass,aluminizedpolyestercanbecutto fit anyviewing

device,anddoesn'tbreakwhendropped.It hasrecentlybeenpointedoutthatsomealuminizedpolyesterfilters

mayhavelarge(uptoapproximately1mminsize)defectsintheiraluminumcoatingsthatmaybehazardous. A

microscopicanalysisof examplesof suchdefectsshowsthatdespitetheirappearance, thedefectsarisefroma

holeinoneofthetwoaluminizedpolyesterfilmsusedinthefilter.Thereisnolargeopeningcompletelydevoid

of theprotectivealuminumcoating.Whilethis is aqualitycontrolproblem,thepresenceof a defectin the

aluminumcoatingdoesnotnecessarilyimplythatthefilterishazardous. Whenindoubt,analuminizedpolyestersolarfilterthathascoatingdefectslargerthan0.2mmin size,or morethana singledefectin any5 mm

circularzoneof thefilter,shouldnotbeused.

An alternativeto aluminizedpolyestersolarfilter materialthathasbecomequitepopularis "black

polymer"in whichcarbonparticlesaresuspendedin a resinmatrix.Thismaterialis somewhatstifferthan

polyesterandrequiresa specialholdingcell if it is to beusedatthefrontof binoculars,telephotolensesor

telescopes. Intendedmainlyasavisualfilter,thepolymergivesayellowimageof theSun(aluminizedpolyester

producesablue-whiteimage).Thistypeof filtermayshowsignificantvariationsindensityofthetint acrossits

extent;someareasmayappearmuchlighterthanothers.Lighterareasofthefiltertransmitmoreinfraredradiationthanmaybedesirable.A recentdevelopment is afilter thatconsistsof aluminum-coatedblackpolymer.

Combiningthebestfeaturesof polyesterandblackpolymer,thisnewmaterialmayeventuallyreplacebothas

thefilter of choicein solareclipseviewers.Thetransmittancecurveof oneof thesehybridfilters(Polymer

PlusTM by Thousand Oaks Optical) is shown in Figure 3.1. Another material, Baader AstroSolar Safety Film, can

be used for both visual and photographic solar observations. It is an ultrathin resin film with excellent optical

quality and less scattered light than most polyester filters.

1In 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 = logl0[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 ....

2Aluminized polyester is popularly known as mylar. DuPont actually owns the trademark "Mylar Tw' and does

not manufacture this material for use as a solar filter.

62 Annular and Total Solar Eclipses of 2003
Manyexperiencedsolarobserversuseoneortwo layersof black-and-whitefilm thathasbeenfully

exposedto lightanddevelopedto maximumdensity.Themetallicsilvercontainedinthefilm emulsionisthe

protectivefilter;howeveranyblack-and-whitenegativewithimagesinit isnotsuitableforthispurpose.More

recently,solarobservershaveusedfloppydisksandcompactdisks(CDsandCD-ROMs)asprotectivefiltersby

coveringthecentralopeningsandlookingthroughthediskmedia.However,theopticalqualityof thesolar

imageformedby afloppydiskor CDisrelativelypoorcomparedto aluminizedpolyesteror welder'sglass.

SomeCDsaremadewithverythinaluminumcoatingsthatarenotsafe- if youcanseethroughtheCDinnormal

roomlighting,don'tuseit!! Nofiltershouldbeusedwithanopticaldevice(e.g.,binoculars,telescope,camera)

unlessit hasbeenspecificallydesignedforthatpurposeandismountedatthefrontend.Somesourcesof solar

filtersarelistedbelow.

Unsafe filters include color film, black-and-white film that contains no silver, 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 3.1). The fact that the Sun appears dim, or that you feel no discomfort when looking at the Sun

through the filter, is no guarantee that your 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. Your local planetarium, science central, or amateur

astronomy club can provide additional information on how to observe the eclipse safely.

There are some concerns that UVA radiation (wavelengths between 315 and 380 nm) in sunlight may

also adversely affect the retina (Del Priore, 1991). 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. However, the solar filter

materials discussed in this article attenuate solar UV radiation to a level well below the minimum permissible

occupational exposure for UVA (ACGIH, 1994), 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 occurs, 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 seeing the

eclipse at all. However, this tactic may backfire, 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 learns later 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, AIDS, or smoking is given? Misinformation may be just as bad, if not worse

than no information (Pasachoff, 2001).

3.02 SOURCES FOR SOLAR FILTERS

A brief list of sources for solar filters appears below. For additional sources, see advertisements in

Astronomy and/or Sky & Telescope magazines. The inclusion of any source on this list does not imply an endorsement of that source by the authors or NASA.

• American Paper Optics, 3080 Bartlett Corporate Drive, Bartlett, TN 38133.

• Celestron International, 2835 Columbia St., Torrance, CA 90503.

• Meade Instruments Corporation, 16542 Millikan Ave., Irvine, CA 92714.

• Orion Telescopes and Binoculars, P.O. Box 1815, Santa Cruz, CA 95061-1815.

• Pocono Mountain Optics, 104 NP 502 Plaza, Moscow, PA 18444.

• Rainbow Symphony, Inc., 6860 Canby Ave., #120, Reseda, CA 91335

• Thousand Oaks Optical, Box 5044-289, Thousand Oaks, CA 91359.

(800)767-8427

(310) 328-9560

(714) 756-2291

(800) 447-1001

(717) 842-1500

(800) 821-5122 *

(805) 491-3642 *

Annular and Total Solar Eclipses of 2003 63
• KhanScopeCentre,3243DufferinStreet,Toronto,Ontario,CanadaM6A2T2

•PerceptorTelescopesTransCanada, BrownsvilleJunctionPlaza,Box38,

Schomberg, Ontario,CanadaLOG1T0

• StarfieldScientific,POBox232,PortKembla,NSW2505,Australia

(416)783-4140

(905)939-2313

0425235804

* sourcesforinexpensivehandheldsolarfiltersandeclipseglasses

3.03 IAU SOLAR ECLWSEEDUCATIONCOMMITTEE

In order to ensure that astronomers and public health authorities have access to information on safe

viewing practices, the Commission on Astronomy Education and Development of the International Astronomical Union, the international organization for professional astronomers, set up a Solar Eclipse Education Committee. Under Prof. Jay M. Pasachoff of Williams College, the Committee has assembled information on safe

methods of observing the Sun and 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, Hopkins Observatory, Williams College,

Williamstown, MA 01267, USA (e-mail: jay.m.pasachoff@williams.edu). Information on safe solar filters can

be obtained by contacting Dr. B. Ralph Chou (e-mail: bchou@sciborg.uwaterloo.ca).

3.04 ECLIPSE PHOTOGRAPHY

From a photographic perspective, annular eclipses are similar to partial eclipses. They both require the

use of safe solar filters as described in the previous section. The partial phases of total eclipses also require

filters. Only the total phase can be viewed and photographed without a filter.

Almost any kind of camera with manual controls can be used to capture these rare events. However, a

lens with a fairly long focal length is recommended to produce as large an image of the Sun as possible. A

standard 50 mm lens yields a minuscule 0.5 mm image, while a 200 mm telephoto or zoom produces a 1.9 mm

image. A better choice would be one of the small, compact catadioptic or mirror lenses that have become widely

available in the past ten years. The focal length of 500 mm is most common among such mirror lenses and yields

a solar image of 4.6 mm. Adding a 2x tele-converter will produce a 1000 mm focal length, which doubles the

Sun's size to 9.2 mm. Focal lengths in excess of 1000 mm usually fall within the realm of amateur telescopes. If

full disk photography of the Sun on 35 mm format is planned, the focal length of the optics must not exceed 2600

mm. However, since most cameras don't show the full extent of the image in their viewfinders, a more practical

limit is about 2000 mm. Longer focal lengths permit photography of only a magnified portion of the Sun's disk.

For November's total eclipse, a focal length no longer than 1500 mm is recommended in order to capture the

solar corona. However, a focal length of 1000 mm requires less critical framing and can capture some of the

longer coronal streamers. For any particular focal length, the diameter of the Sun's image is approximately equal

to the focal length divided by 109 (Table 3.1).

A solar filter must be used on the lens throughout the partial phases (and annularity) for both photography and viewing. Such filters can be obtained through manufacturers and dealers listed in Sky & Telescope and

Astronomy magazines (see: SOURCESFORSOLARFILTERS). These filters typically attenuate the Sun's visible and

infrared energy by a factor of 100,000. However, the actual filter factor and choice of ISO film speed will play

critical roles in determining the correct photographic exposure. Almost any speed film can be used since 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 between 1/1000 and 1/4 second. After the film is developed, note the best exposures

and use them to photograph all the partial phases. The Sun's surface brightness remains constant throughout the

eclipse, so no exposure compensation is needed except for the crescent phases (and annularity) which require

two more stops due to solar limb darkening. Bracketing by several stops is also necessary if haze or clouds

64 Annular and Total Solar Eclipses of 2003
IMAGE SCALE OF A TOTAL SOLAR ECLIPSE AT VARIOUS FOCAL LENGTHS

_--0

7-5

--15

--20

7_ 25

-ao

za5

F. E_laeamk 1995 Ju.e

interfere on eclipse day. This is especially true for the May 31 annular eclipse which occurs low on the horizon.

A camera with a built in spot meter would be of great value in determining the exposure. If the haze is thick

enough, you may need to remove the solar filter in order to see and photograph the annular eclipse, but extreme

caution must be used.

For November's eclipse, the most spectacular and awe inspiring phase is totality. For two brief minutes,

the Sun's pearly white corona, red prominences and chromosphere are visible. The most important point to

remember is that during the total phase, all solar filters must be removed! The corona is a million times fainter

than the photosphere, so photographs of the corona must be made without a filter. It is completely safe to view

the totally eclipsed Sun directly with the naked eye. No filters are needed and they will only hinder your 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. Thus, 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/! 000 down

to 1 second). Rehearsing this sequence is highly recommended since great excitement accompanies totality and

there is little time to think.

Exposure times for various film speeds (ISO), apertures (f/number) and features (chromosphere, prominences, inner, middle and outer corona) are summarized in Table 3.2. The table was developed from eclipse

photographs made by Espenak and photographs published in Sky and Telescope. To use the table, first select the

ISO film speed in the upper left column. Next, move to the right to the desired aperture or f/number for the

chosen ISO. 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, you can calculate the recommended

shutter speed using the 'Q' factors tabulated along with the exposure formula at the bottom of Table 3.2. Keep in

mind that these exposures are based on a clear sky and a corona of average brightness. You should bracket your

exposures one or more stops to take into account the actual sky conditions and the variable nature of these

phenomena.

Finally, an eclipse effect that is easily captured with point-and-shoot or automatic cameras should not be

overlooked. Use a kitchen sieve or colander and allow its shadow to fall on a piece of white card-board placed

several feet away. The holes in the utensil act like pinhole cameras and each one projects its own image of the

Sun. The effect can also be duplicated by forming a small aperture with one's hands and watching the ground

below. The pinhole camera effect becomes more prominent with increasing eclipse magnitude. Virtually any

Annular and Total Solar Eclipses of 2003 65
cameracanbeusedtophotographthephenomenon, butautomaticamerasmusthavetheirflashesturnedoff

sincethiswouldotherwiseobliteratethepinholeimages.

If photographyisdoneaboardashipatsea,thisputscertainlimitsonthefocallengthandshutterspeeds

thatcanbeused.Generalrecommendations aredifficultto make since it depends on the stability of the ship as

well as wave heights encountered on eclipse day. Certainly telescopes with focal lengths of 1000 mm or more

can be ruled out since their small fields of view would require the ship to remain virtually motionless and this is

rather unlikely even given calm seas. A 500 mm lens might be a safe upper limit in focal length. ISO 400 is a

good film speed choice for photography at sea. For the total eclipse, shutter speeds as slow as 1/8 or 1/4 may be

tried if the ocean is calm day. Otherwise, stick with a 1/15 or 1/30 and shoot a sequence through 1/1000 second.

It might be good insurance to bring a wider 200 mm lens just in case the seas are rougher than expected. New

image stabilized lenses from Canon and Nikon may also be helpful aboard ship by allowing the use of slower

shutter speeds.

Cold weather and below freezing temperatures will be the greatest challenge especially for travelers to

the total eclipse in Antarctica (see ECLIPSESATCOLD TEMPERATURES). The best advice is to keep observing and

photography plans very simple and uncomplicated.

For more information on eclipse photography, observations and eye safety, see FURTHERREADINGin the

BIBLIOGRAPHY.

3.05 ECLIPSES AT COLD TEMPERATURES

Along the coast of Antarctica, the average and even the coldest temperatures do not constitute a particularly difficult challenge for astronomy. Commercial telescopes and telescope equipment work reasonably well

and cameras will usually function without fatal complaint. The wind chill values will make instruments cool

quickly and steal the heat from any warming devices, but will not reduce the temperatures below the ambient

values. Battery power is a different story. The power supplied by internal batteries of many cameras and camcorders

begins to fail when temperatures fall below -10°C. Batteries must be kept warmer than this if they are to

function.

Antarctica's interior temperatures are a far more challenging adversary. Commercial telescopes begin to

fail at about -30°C, especially after several hours at those temperatures. Only manual cameras can be trusted,

although shutters begin to lock up or fail at -35°C. Chemical warming packs will not work unless boosted by

being tucked up against a warm human body, especially if the wind chill is significant. In such a cold weather

venue, photographic plans should be modest.

Eyepieces will be quick to frost over when an errant breath of moist air condenses on their cold surfaces,

so a spare should be kept within easy reach inside a pocket. Camera viewfinders are similarly affected. Metal

stings immediately, and so a thin inner glove can permit fine adjustments possible at the last critical moments.

Latex medical gloves can prevent hands from sticking to metal, but these provide no warmth and leave hands

feeling clammy. However, they do prevent the skin from drying and cracking.

Cold and dry air brings static electrical discharges within the camera body that can leave jagged streaks

across film that is advanced too rapidly. Motor driven cameras are most likely to suffer this fate. All film should

be advanced slowly and carefully to avoid the discharges and breaking the brittle film. With average temperatures, cameras and telescopes should be able to tough it out in the interior. Below normal temperatures will be

too much without supplementary heating but even something as simple as covering equipment in a black cloth to

absorb whatever energy the Sun can offer may bring sufficient warming to make eclipse observation and photography more successful.

Cameras are best kept inside a coat against the skin and brought out for photography when needed. The

eclipse is short and warm equipment will not cool so quickly that it fails in the time available. Attaching cameras

to telescopes is more difficult, but even at -30°C, bare hands can be used for a half-minute to make a final

adjustments. Small parts don't have a great heat capacity and won't usually burn in a short minute but large metal

objects can produce a very quick frostbite.

66 Annular and Total Solar Eclipses of 2003
Windscanplayhavocwitheclipseplans,especiallyalongcoastalAntarcticawhereaveragespeedsare

nearlytwicethoseinland.Forthemostpartprevailingwindstendtocomeoutof thesouthandsoutheast, the

samedirectioninwhichtheSunliesduringtheeclipse.Windbreakswill havetobeselectedcarefullyto avoid

blockingtheeclipseif theycanbeusedatall.

Warmthiscriticalif theeclipseistobeenjoyedandinAntarcticconditionsthismeanseverallayersof

clothing.Foraverageconditionsonthecoastwithmodestwindsthefollowingmightsuffice:

• Longunderwearortightsunderloose-fittingpants

•Twopairof socks,onelightandtheotherheavier,madeof woolorsimilarmaterial

•T-shirtandregularshirt

• Lightundercoat-asummerjacketwoulddohere

•Well-insulatedwintercoat.Syntheticfillingsarenomatchfor goosedown.

• Pairof lightbicycleglovescoveredbymoresubstantial mittsorgloves

• Hatthatcancovertheears

•Insulatedboots

Forcolderinteriortemperaturesthefollowingshouldbeaddedorsubstituted:

•Winterbootswithhightops,thickinsolesandwarmliners

•Outerwindpants,preferablyfilledwithdown,andloosefitting(snowmobilepants)

• Heavymittswithlighterglovesinside

• Chemicalhand-warmers, tuckedintoaconvenientpocketorloose-fittingboot.Be

careful!

• Longdown-filledwintercoatwithahood.Don'tkeepthehoodupwhenworking

withequipmentasit will trapmoisturethatcanfreezeonopticalsurfaces.

•Balaclavatocovertheface,exceptforeyesandmouth

3.06 IAU WORKING GROUP ON ECLIPSES

Professional scientists are asked to send descriptions of their eclipse plans to the Working Group on

Eclipses of the International Astronomical Union, so that 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 web: www.williams.edu/astronomy/IAU eclipses

Williams College-Hopkins Observatory email: jay.m.pasachoff@williams.edu

Williamstown, MA 01267, USA FAX: (413) 597-3200

The members of the Working Group on Eclipses of the Solar Division of the International Astronomical

Union are: Jay M. Pasachoff (USA), Chair; E Clette (Belgium), E Espenak (USA); Iraida Kim (Russia); Francis

Podmore (Zimbabwe); V. Rusin (Slovakia); Jagdev Singh (India); Yoshinori Suematsu (Japan); consultant: J.

Anderson (Canada).

The web site of the Program Group on Public Education at the Times of Eclipses of the Education and

Development commission of the IAU is www.eclipses.info.

Annular and Total Solar Eclipses of 2003 67
3.07 INTERNATIONAL SOLAR ECLIPSE CONFERENCE

An international Solar Eclipse Conference 2004 (SEC2004) will be held on 2004 Aug 20-22 at Open

University, Milton Keynes, England. The main objective of the conference is to bring together professionals and

amateurs to discuss all aspects of solar eclipses. Two days of lectures will be given in each of the following

disciplines: predictions, mathematics, solar physics, weather forecasting, eye safety, diameter measuring, edge

and central, and ancient eclipse research. Both past and future solar eclipses will be discussed, as well as the

2004 transit of Venus. For registration and more details, contact Patrick Poitevin (email:

solareclipsewebpages @btopenworld.com) or visit the SEC2004 web page:

http://solareclipsewebpages.users.btopenworld.com/SEC_files/SEC2004.html

3.08 NASA ECLIPSE BULLETINS ON 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 World-Wide Web using a Web browser (e.g.:

Netscape, Microsoft Explorer, etc.) from the GSFC SDAC (Solar Data Analysis Center) Eclipse Information

home page, or from top-level URL's for the currently available eclipse bulletins themselves:

http://umbra.nascom.nasa.gov/eclipse/ (SDAC Eclipse Information)

http://umbra.nascom.nasa.gov/eclipse/94 l 103/rp.html

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

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

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

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

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

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

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

(1994 Nov 3)

(1995 Oct 24)

(1997 Mar 9)

(1998 Feb 26)

(1999 Aug 11)

(2001 Jun 21)

(2002 Dec 04)

(2003 eclipses)

The original Microsoft Word text files, GIF and PICT figures (Macintosh format) are also available via anonymous ftp. They are stored as BinHex-encoded, StuffIt-compressed Mac folders with .hqx suffixes. For PC's, the

text is available in a zip-compressed format in files with the .zip suffix. There are three sub directories for figures

(GIF format), maps (JPEG format), and tables (html tables, easily readable as plain text). Some of the newer

bulletins are also available in pdf format.

Current plans call for making all future NASA eclipse bulletins 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.

3.09 FUTURE ECLIPSE PATHS ON INTERNET

Presently, the NASA eclipse bulletins are published 12 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, Jones

and Clark, 1954]. The value used for the Moon's secular acceleration is n-dot = -26 arc-sec/cy 2, as deduced by

68 Annular and Total Solar Eclipses of 2003
MorrisonandWard[1975].A correctionof-0.6"wasaddedto theMoon'seclipticlatitudeto accountforthe

differencebetweentheMoon'scentralof massandcentralof figure.ThevalueforATisfromdirectmeasurementsduringthe20thcenturyandextrapolationintothe21stcentury.Thevalueusedfor theMoon'smean

radiusisk=0.272281.

The umbral path characteristics have been predicted at 2 minute intervals of time compared to the 6

minute interval used in Fifty Year Canon of Solar Eclipses: 1986-2035 [Espenak, 1987]. This should provide

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 page for the path tables and

maps is:

http://sunearth.gsfc.nasa.gov/eclipse/SEpath/SEpath.html

3.10 SPECIAL WEB SITES FOR 2003 SOLAR ECLIPSES

Two special web sites have been set up to supplement this bulletin with additional predictions, tables

and data for the solar eclipses of 2003. The URL's of these two web sites are:

http://sunearth.gsfc.nasa.gov/eclipse/ASE2003/ASE2003.html

http://sunearth.gsfc.nasa.gov/eclipse/TSE2003/TSE2003.html

3.11 PREDICTIONS FOR ECLIPSE EXPERIMENTS

This publication provides comprehensive information on the 2003 solar eclipses to both the professional

and amateur/lay communities. However, certain investigations and eclipse experiments may require additional

information which lies beyond the scope of this work. We invite the international professional community to

contact us 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 2003 eclipses as well as for previous eclipses in which analysis is still in

progress. To discuss your needs and requirements, please contact Fred Espenak (espenak@gsfc.nasa.gov).

3.12 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 due to the irregularity in the limb profile. From 1968 through 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, 1974]. Unfortunately, the use of two different values of k for umbral eclipses introduces

a discontinuity in the case of hybrid or annular-total eclipses.

In August 1982, the International Astronomical Union (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 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 annular-total 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. A total eclipse can be defined as an eclipse in which the

Sun's disk is completely occulted by the Moon. This cannot occur so long as any photospheric rays are visible

Annular and Total Solar Eclipses of 2003 69
throughdeepvalleysalongtheMoon'slimb[Meeus,GrosjeanandVanderleen, 1966].ButtheuseoftheIAU's

meank guarantees that some annular or annular-total eclipses will be misidentified as total. A case in point is the

eclipse of 3 October 1986. Using the IAU value for k, the Astronomical Almanac identified this event as a total

eclipse of 3 seconds duration when it was, in fact, a beaded annular eclipse. Since a smaller value of k is more

representative of the deeper lunar valleys and hence the minimum solid disk radius, it helps ensure the correct

identification of an eclipse's true nature.

Of primary interest to most observers are the times when 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 must be performed, especially if one plans to

observe near the path limits [Herald, 1983]. For observers near the center line of a total eclipse, the limb corrections can be more closely approxin]ated 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, we depart 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]. Consequently, the smaller k 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 result in longer umbral durations and wider paths for annular eclipses than do predictions using the IAU's k.

3.13 ALGORITHMS, EPHEMERIDES AND PARAMETERS

Algorithms for the eclipse predictions were developed by Espenak primarily from the Explanatory Supplemerit [1974] with additional algorithms from Meeus, Grosjean and Vanderleen [1966] and Meeus [1982]. 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 fiom 2002 to 2003, a value for AT of 64.7 and 64.8 seconds for the May and November eclipses,

respectively, 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, da 3, hour, minute, second).

The primary source for geographic coordinates used in the local circumstances tables is The New International Atlas (Rand McNally, 1991). Coordinates for research stations in Antarctica are from www.scar.org/

Antarctic%20Info/wintering_stations_2000.htm. Elevations for major cities were taken from Climates of the

World (U.S. Dept. of Commerce, 1972).

All eclipse predictions presented in this publication were generated on a Macintosh G4 iMac computer.

Word processing and page layout for the publication were done using Microsoft Word v5.1. Figures were annotated with Claris MacDraw Pro 1.5. Meteorological diagrams and tables were prepared using Microsoft Excel 98.

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 data base for future eclipses. All calculations, diagrams and opinions

presented in this publication are those of the authors and they assume full responsibility for their accuracy.

70 Annular and Total Solar Eclipses of 2003
FIGURE 3.1 - SPECTRAL RESPONSE OF SOME COMMONLY AVAILABLE SOLAR FILTERS

0 500 1000 1500 2000 2500

8L i i i ii i i i it i i i i i i i i i , i F , ]

SN 14 WELDER'S FILTER _

i

aj , , , !, I , , i, , ; , , , , t , , , , l , , , ,_A

i i

t i

' " '' ''''' '' '' '

6 II ___

', SOLAR SKREEN -_

43 I I I P I I I il I 1 I I I I 1 I I I F I I I I I _

i I

i I

II _ i ""-'_'7 BAADER ASTROSOLAR FILM_

t i i i p [ i i Ill i t i i i P p i i i i 4 q i P p J

4

3 i i

p i

i

/ I I I I I I I _ I I /

._ 8 i I I I Ill I ' I Ill I I ' I I THOUSAND

7 : yAKS T2 GLASS .K,"

•

Q 4

*

9 ' THOUSAND OAKS POLYMER PLUS

8 _

6_

5 . :ii "iI :ll i'l" : 1 _ il " il'_ , ii : i_ _ I i :l i ill :1" _ iI : I " Ii _ ii" il_ i ii i I _. "1 "

I

i

8

7

6

5

4

3

2

1

0

0

i

I I I i _ I I iI I I I L I I I I I I I I I /

- ,h ' l ....

_AAJ^,,., .L.; _. , EXPOSED & DEVELOPED FILM

- i \

__-- II : '"\_ COLOR NEGATIVE (UNSAFE FOR SOLAR VIEWING. _)

- i I "',_ | / I

I 500 I 1000 1500 2000 2500 i i

!"_F--VISIBLE_', Wavelength (nm) B. _. Cho, ,,d r. esp_,a_

Annular and Total Solar Eclipses of 2003 71
TABLE 3.1

35 MM FIELD OF VIEW AND SIZE OF SUN'S IMAGE

FOR VARIOUS PHOTOGRAPHIC FOCAL LENGTHS

Focal Length Field of View Size of Sun

28 mm 49 ° x 74 ° 0.2 mm

35 mm 39 ° x 59 ° 0.3 mm

50 mm 27 ° x 40 ° 0.5 mm

105 mm 13° x 19 ° 1.0 mm

200 mm 7° x 10° 1.8 mm

400 mm 3.4 ° x 5.1 ° 3.7 mm

500 mm 2.7 ° x 4.1 ° 4.6 mm

1000 mm 1.4 ° x 2.1 ° 9.2 mm

1500 mm 0.9 ° x 1.4 ° 13.8 mm

2000 mm 0.7 ° x 1.0 ° 18.4 mm

2500 mm 0.6 ° x 0.8 ° 22.9 mm

Image Size of Sun (mm) = Focal Length (mm) / 109

SOLAR

TABLE 3.2

ECLIPSE EXPOSURE

__ ISO

25 1.4

50 2

100 2.8

200 4

400 5.6

800 8

1600 11

__ Subject Q

Solar Eclipse

Partial _ - 4.0 ND 11 --

PartiaP - 5.0 ND 8 1/4000

Baily's Beads 2 11 --

Chromosphere 10 --

Prominences 9 --

Corona - 0.1 Rs 7 1/2000

Corona - 0.2 Rs 3 5 1/500

Corona - 0.5 Rs 3 1/125

Corona - 1.0 Rs 1 1/30

Corona - 2.0 Rs 0 1/15

Corona - 4.0 Rs -1 1/8

Corona - 8.0 Rs -3 1/2

GUIDE

f/Number

2 2.8 4 5.6 8

2.8 4 5.6 8 11

4 5.6 8 11 16

5.6 8 11 16 22

8 11 16 22 32

11 16 22 32 44

16 22 32 44 64

11 16 22

16 22 32

22 32 44

32 44 64

44 64 88

64 88 128

88 128 176

Shutter Speed

-- -- 1/4000 1/2000 1/1000 1/500 1/250 1/125

1/2000 1/1000 1/500 1/250 1/125 1/60 1/30 1/15

-- -- 1/4000 1/2000 1/1000 1/500 1/250 1/125

-- 1/4000 1/2000 1/1000 1/500 1/250 1/125 1/60

1/4000 1/2000 1/1000 1/500 1/250 1/125 1/60 1/30

1/1000 1/500 1/250 1/125 1/60 1/30 1/15 1/8

1/250 1/125 1/60 1/30 1/15 1/8 1/4 1/2

1/60 1/30 1/15 1/8 1/4 1/2 1sec 2 sec

1/15 1/8 i/4 1/2 1 sec 2 sec 4 sec 8 sec

1/8 1/4 1/2 1 sec 2 sec 4 sec 8 sec 15 sec

1/4 1/2 1 sec 2 sec 4 sec 8 sec 15 sec 30 sec

1 sec 2 sec 4 sec 8 sec 15 sec 30 sec 1 rain 2 rain

Exposure Formula: t = f2 / (I x 2Q) where: t = exposure time (sec)

f = f/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. _- 2002

72 Annular and Total Solar Eclipses of 2003
REQUEST FORM YOn NASA ECLIPSE BULLETINS

NASA eclipse bulletins contain detailed predictions, maps and meteorology for future central solar eclipses of interest.

Published as part of NASA's Technical Publication (TP) series, the bulletins are prepared in cooperation with the Working

Group on Eclipses of the International Astronomical Union and are provided as a public service to both the professional

and lay communities, including educators and the media In order to allow a reasonable lead time for planning purposes,

subsequent bulletins will be published 12 to 24 months before each event. Comments, suggestions and corrections are

solicited to improve the content and layout in subsequent editions of this publication series.

Single copies of the bulletins are available at no cost and may be ordered by sending a 9 x 12 inch SASE (self

addressed stamped envelope) with sufficient postage for each bulletin (12 oz. or 340 g). Use stamps only since cash or

checks cannot be accepted. Requests within the U. S. may use the Postal Service's Priority Mail 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-2002-211618 -- Annular and Total Solar Eclipses of 2003

Name of Organization:

(in English, if necessary):

Name of Contact Person:

Address:

City/State/ZIP:

Country:

E-mail:

Type of organization:

(check all that apply)

Size of Organization: __

Activities:

__ University/College __ Observatory __ Library

Planetarium Publication Media

Professional Amateur Individual

(Number of Members)

Return Requests

and Comments to:

E-mail:

Fax:

Fred Espenak

NASA/GSFC

Code 693

Greenbelt, MD 20771

USA

espenak@ gsfc.nasa.gov

(301) 286-0212

or

E-mail:

Fax:

Jay Anderson

Environment Canada

123 Main Street, Suite 150

Winnipeg, MB,

CANADA R3C 4W2

jander @cc.umanitoba.ca

(204) 983-0109

2002 Oct

Annular and Total Solar Eclipses of 2003 75
J Form Approved

REPORT DOCUMENTATION PAGE OMB No. 0704-0188

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gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this

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1. AGENCY USE ONLY (Leave blank) 2. REPORT DATE

October 2002

4. TITLE AND SUBTITLE

Annular and Total Solar Eclipses of 2003

6. AUTHOR(S)

Fred Espenak and Jay Anderson

7.PERFORMINGORGANIZATIONNAME(S)ANDADDRESS(ES)

Goddard Space Flight Center

Greenbelt, Maryland 20771

9. SPONSORING / MONITORING AGENCY NAME(S) AND ADDRESS (ES)

National Aeronautics and Space Administration

Washington, DC 20546-0001

3. REPORT TYPE AND DATES COVERED

Technical Paper

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460

8. PEFORMING ORGANIZATION

REPORT NUMBER

2003-00184-0

10. SPONSORING / MONITORING

AGENCY REPORT NUMBER

2002--TP-211618

11. SUPPLEMENTARY NOTES

J. Anderson, Environment Canada, Winnepeg, Manitoba, Canada.

12a. DISTRIBUTION/AVAILABILITY STATEMENT 12b. DISTRIBUTION CODE

Unclassified-Unlimited

Subject Category: 89

Report available from the NASA Center for AeroSpace Information,

7121 Standard Drive, Hanover, MD 21076-1320. (301) 621-0390.

13. ABSTRACT (Maximum 200 words)

On 2003 May 31, an annular eclipse of the Sun will be visible from a large zone covering the North

Atlantic. The path of the Moon's antumbral shadow begins in northern Scotland, crosses Iceland and

central Greenland, and ends at sunrise in Baffin Bay (Canada). A partial eclipse will be seen within the

much broader path of the Moon's penumbral shadow, which includes most of Europe, the Middle East,

central and northern Asia, and northwestern North America. Six months later on 2003 November 23, a

total eclipse of the Sun will be visible from a broad corridor that traverses portions of the Southern

Hemisphere. The path of the Moon's umbral shadow begins in the Indian Ocean, crosses Antarctica,

and ends at sunrise near the edge of the southern continent. A partial eclipse will be seen within the

much larger path of the Moon's penumbral shadow, which includes Australia, New Zealand, Antarctica and southern South America. Detailed predictions for these two events are presented and include

besselian elements, geographic coordinates of the path of umbral eclipse, physical ephemeris of the

umbra, topocentric limb profile corrections, local circumstances for hundreds of cities, maps of the

eclipse paths, weather prospects, the lunar limb profiles and the sky during totality. Information on

safe eclipse viewint_ and additional web resources is included.

14. SUBJECT TERMS

Solar eclipse, celestial mechanics, ephemeris, Sun, Moon.

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OF REPORT

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