Solar Eclipse Prime Page
Total Solar Eclipse of -1718 Apr 27 (1719 Apr 27 BCE)
Fred Espenak
Introduction
The
Total Solar Eclipse of -1718 Apr 27 (1719 Apr 27 BCE)
is visible from the geographic regions shown on the map to the right.
Click on the map to enlarge it.
For an explanation of the features appearing in the map,
see Key to Solar Eclipse Maps.
The instant of greatest eclipse takes place on -1718 Apr 27 at 04:57:06 TD (17:53:31 UT1).
This is 0.8 days after the Moon reaches perigee.
During the eclipse, the Sun is in the constellation Taurus.
The synodic month in which the eclipse takes place has a Brown Lunation Number of -45029.
The eclipse belongs to Saros 1 and is number 65 of 72 eclipses in the series.
All eclipses in this series occur at the Moon’s ascending node.
The Moon moves southward with respect to the node with each succeeding eclipse in the series and gamma decreases.
This total eclipse is very unusual in that it is NON-CENTRAL and does NOT have a central line nor a southern path limit.
Instead , over half of the umbral shadow falls off into space throughout the eclipse.
Gamma has a value of -0.9986.
The total solar eclipse of -1718 Apr 27 is followed two weeks later by a total lunar eclipse on -1718 May 12.
Another solar eclipse occurs one synodic month after the -1718 Apr 27 eclipse. It is the partial solar eclipse of -1718 May 26.
These eclipses all take place during a single eclipse season.
The eclipse predictions are given in both Terrestrial Dynamical Time (TD)
and Universal Time (UT1).
The parameter ΔT is used to convert between these two times (i.e., UT1 = TD - ΔT).
ΔT has a value of
39814.8
seconds for this eclipse.
The uncertainty in ΔT is
2631.4 seconds corresponding to a standard error in longitude of the eclipse path of ± 10.99°.
The following links provide maps and data for the eclipse.
The tables below contain detailed predictions and additional information on the
Total Solar Eclipse of -1718 Apr 27
.
Umbral Shadow Contacts and Extremes: Total Solar Eclipse of -1718 Apr 27
| Contacts of Umbral Shadow with Earth |
| Contact Event |
Contact |
Time
TD |
Time
UT1 |
Latitude |
Longitude |
| First External Contact | U1 | 04:40:10.4 | 17:36:35.6 | 69°44.7'S | 017°20.6'W |
| Last External Contact | U4 | 05:14:33.2 | 18:10:58.4 | 51°45.2'S | 013°42.8'W |
| Extreme Northern and Southern Path Limits of Umbra |
| Contact Event |
Contact |
Time
TD |
Time
UT1 |
Latitude |
Longitude |
| North Extreme Path Limit 1 | N1 | 04:55:55.1 | 17:52:20.3 | 63°23.6'S | 001°14.7'E |
| South Extreme Path Limit 1 | S1 | 04:58:50.3 | 17:55:15.5 | 61°45.4'S | 000°30.9'E |
Non-Central Total Solar Eclipse
Explanation of Umbral Shadow Contacts and Extremes Tables
Non-Central Total Solar Eclipse
Explanation of Central Line Extremes Table
Non-Central Total Solar Eclipse
Polynomial Besselian Elements: Total Solar Eclipse of -1718 Apr 27
| Polynomial Besselian Elements |
| -1718 Apr 27 at 05:00:00.0 TD (=t0) |
| n |
x |
y |
d |
l1 |
l2 |
μ |
| 0 | 0.49485 | -0.86781 | 8.0787 | 0.53120 | -0.01489 | 256.0436 |
| 1 | 0.51300 | 0.27366 | 0.0146 | 0.00004 | 0.00004 | 15.0053 |
| 2 | -0.00001 | 0.00000 | -0.0000 | -0.00001 | -0.00001 | -0.0000 |
| 3 | -0.00001 | -0.00000 | - | - | - | - |
| Tan ƒ1 | 0.0045968 |
| Tan ƒ2 | 0.0045739 |
At time t1 (decimal hours), each besselian element is evaluated by:
x = x0 + x1*t + x2*t2 + x3*t3 (or x = Σ [xn*tn]; n = 0 to 3)
where: t = t1 - t0 (decimal hours) and t0 = 5.000
Explanation of Polynomial Besselian Elements
Calendar
The Gregorian calendar (also called the Western calendar) is internationally the most widely used civil calendar.
It is named for Pope Gregory XIII, who introduced it in 1582.
On this website, the Gregorian calendar is used for all calendar dates from 1582 Oct 15 onwards.
Before that date, the Julian calendar is used.
For more information on this topic, see Calendar Dates.
The Julian calendar does not include the year 0.
Thus the year 1 BCE is followed by the year 1 CE (See: BCE/CE Dating Conventions).
This is awkward for arithmetic calculations.
Years in this catalog are numbered astronomically and include the year 0.
Historians should note there is a difference of one year between astronomical dates and BCE dates.
Thus, the astronomical year 0 corresponds to 1 BCE, and astronomical year -1 corresponds to 2 BCE, etc..
Eclipse Predictions
Predictions for the
Total Solar Eclipse of -1718 Apr 27
were generated using the
JPL DE406
solar and lunar ephemerides.
The lunar coordinates were calculated with respect to the Moon's Center of Mass.
The predictions are given in both Terrestrial Dynamical Time (TD)
and Universal Time (UT1).
The parameter ΔT is used to convert between these two times (i.e., UT1 = TD - ΔT).
ΔT has a value of
39814.8
seconds for this eclipse.
The uncertainty in ΔT is
2631.4 seconds corresponding to a standard error in longitude of the eclipse path of ± 10.99°.
Acknowledgments
Some of the content on this website is based on the book Thousand Year Canon of Solar Eclipses 1501 to 2500.
All eclipse calculations are by Fred Espenak, and he assumes full responsibility for their accuracy.
Permission is granted to reproduce eclipse data when accompanied by a link to this page and an acknowledgment:
"Eclipse Predictions by Fred Espenak, www.EclipseWise.com"
The use of diagrams and maps is permitted provided that they are NOT altered (except for re-sizing) and the embedded credit line is NOT removed or covered.
