If you need an introduction to the solar eclipse functionality in Photo Ephemeris Web, please see Solar Eclipse Planning.
Solar eclipse data is derived from Besselian elements provided by Fred Espenak and published by NASA (Acknowledgement: Eclipse Predictions by Fred Espenak, NASA/Goddard Space Flight Center Emeritus)
Where observer elevation above sea level is used as an input to the calculation, this is obtained from the elevation data source in the app (e.g. SRTM3, AsterGDEM, Google Elevation), which may optionally be adjusted by a user provided offset.
DeltaT values used in all eclipse calculations are those provided in the Besselian elements. Otherwise, DeltaT is obtained from the following sources:
- For years up to 2006: values are taken from Jean Meeus Astronomical Algorithms, 2nd Ed., p.79 Table 10.A
- For years 2006 - 2024, values are from http://maia.usno.navy.mil/ser7/deltat.data
- For years 2024 - 2034, values are from http://maia.usno.navy.mil/ser7/deltat.preds:
- For years beyond 2034, we implement these expressions: https://eclipse.gsfc.nasa.gov/SEhelp/deltatpoly2004.html
- Calculation of general eclipse characteristics is based on Jean Meeus, Astronomical Algorithms, 2nd Ed.
- Calculation of eclipse local circumstances and eclipse paths is based on Jean Meeus, Elements of Solar Eclipses 1951 - 2200; The Astronomical Almanac 2023; The Explanatory Supplement to the Astronomical Almanac, 3rd Ed.
- Eclipse paths are shown with a resolution of 0.1 degrees in longitude calculated for an observer at sea level (see Limitations below)
- Azimuth, altitude and semidiameters of the Sun and Moon are derived from the Besselian elements for the purposes of the eclipse paths, simulator, and contact times. Elsewhere in the app, these values are calculated independently. The ephemerides used to derive the Besselian elements are not necessarily the same algorithms as used by the app and so minor discrepancies may be observed (in the order of 0.01 degrees or less).
- Contact times are calculated assuming a smooth spherical moon. No correction is made for the lunar limb profile, which typically affects the timing of C2 and C3 by a few seconds, but up to ~15s in extreme cases. The lunar limb also affects the appearance of Baily's Beads, especially at locations on the edge of the path of totality, and also the observed position angle of C2 and C3.
- The assumption of a smooth moon restricts accuracy of the northern and southern eclipse path limits to within ±1-2km
- Eclipse path points are calculated at intervals of 0.1° longitude (11.1km intervals at the equator, 7.8km at ±45° latitude), including path end points. Always check the local circumstances by placing the primary (red) map pin - the timeline and simulator are unaffected by any approximations or inaccuracies in the calculated path
- Eclipse paths are calculated assuming an observer at sea level. For northern hemisphere observers located above sea level, the path will move southwards by some amount based on the circumstances of the eclipse, the height above sea level and the azimuth of the sea-level derived eclipse path. The adjustment is typically of the order of ~500m per 1000m of elevation, but becomes more extreme at locations towards the extreme of the eclipse path (i.e. when the sun/moon are low above the horizon)
- Eclipse paths are currently incomplete in polar regions (latitude > ~|66°|). We hope to complete implementation of polar eclipse paths in the future.
- For general planning and for locations well within the displayed path limits (i.e. > ~10km from path ends and northern/southern limits) the data provided is expected to be more than adequate for planning purposes
- If you are planning to observe an eclipse from a location near the edge of the path of totality or annularity, or from a location high above sea level, you should consult multiple reliable sources in your planning, and in particular those which consider the lunar limb profile. We recommend:
- Weather is a key consideration in observing an eclipse: for recommendations, historical research and more, see eclipsophile.com
The simulation accounts for:
- Passage of the moon in front of the sun, with positions and semidiameters derived from the Besselian elements
- Display of the diamond ring effect at the predicted contact position angles
- A simulation of the corona, chromosphere and solar prominences
- Darkening and lightening of the sky (illustrative, non-rigorous)
- The position of the horizon for eclipses near sunrise or sunset
- Changes in the parallactic angle and the physical ephemeris of the sun over time
The simulation does NOT account for:
- Libration and variations in the lunar limb profile
- Baily's beads
- Differential refraction effects near the horizon
- The images used for the simulation come from the 2017 total solar eclipse (credit: Alison Craig and Stephen Trainor).
- The actual appearance of the corona and solar prominences varies over time and will not exactly match the simulation.
- The appearance, shape, and brightness of both the diamond ring and corona vary significantly based on your shot exposure and exact timing.
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