winner: 0.998305 arcmin : 228 [ 37 63 60 58 6 4]
This script keeps running the ray search followed by the nudge search.
If it finds a better solution that the existing one, it replaces it.
Found the above solution after about 30 minutes.
Relax apparent angular error threshold from 0.4 to 1.0 arcminutes.
No longer compare TOP2013 to NOVAS while optimizing.
Use worst-case distance between Earth and Pluto:
Pluto radius from Sun, minus Earth aphelion distance.
Sample 503 points intead of 293.
Measure 2 full orbits before J2000 and 2 full orbits after J2000.
Statistics for output/8.top :
OptimizeTop: 268 terms [ 34 57 72 90 9 6]
Use much tighter pruning to figure out when a transit might be
possible, based on a smaller angle between the planet and Sun
at the moment of inferior conjunction.
Including aberration makes little difference in the transit calculations,
so I turned that off to be a little more efficient.
To be consistent, when calculating the geocentric position of the Sun,
we do need to correct for light travel time just like we would for any
other object. This reduces the maximum time error for predicting transits
from 25 minutes to 11 minutes.
Also had to disable aberration when calculating moon phases
(longitude from Sun) in order to keep a good fit with test data.
Does not pass unit test yet.
I had to rework norm.py because I misunderstood the data format.
The date given is not for the beginning of the transit, but
for the peak. This means the normalized data files need to
keep the start time, peak date/time, and finish time.
The unit test needs to adjust start time and finish time
to make sense with respect to the peak time, by adding/subtracting
a day as needed.
Wrote stub C functions for finding transits.
Updated html files containing Espenak test data for Mercury, Venus.
Updated norm.py to convert the html files to easy-to-use text files.
Added global/local solar eclipse functions to topic indexes for
C#, JavaScript, and Python.
Revised wording "eclipse found may be" --> "eclipse may be".
Python:
- Added missing Attributes section in class GlobalSolarEclipseInfo.
- Added classes EclipseEvent, LocalSolarEclipseInfo.
- Added stub functions SearchLocalSolarEclipse, NextLocalSolarEclipse.
I decided it made more sense to report the Sun's altitude
at each solar eclipse event than reporting sunrise and sunset.
Sunrise and sunset are ambiguous because it's not clear which pair
should be reported. It's also harder to interpret than knowing
whether the Sun is above/below the horizon at each interesting time.
This motivated me to create a new type astro_eclipse_event_t that
holds the (time, altitude) pair for each event.
Defined data structure astro_local_solar_eclipse_t.
Created stubs for functions to find local solar eclipses.
Renamed lunar eclipse 'center' to 'peak' to be consistent.
In all 4 supported languages, use consistent constant names for
Earth and Moon radii.
Use Moon's equatorial radius for rise/set timing.
Use Moon's mean radius for calculating Moon's umbra radius for
detecting solar eclipses.
Also use Moon's mean radius for determining whether the Earth's shadow
touches the Moon, for finding lunar eclipses.
Use the Moon's polar radius for distinguishing between total
and annular eclipses, with a 14 meter bias (instead of 1420 meters!)
to match Espenak data.
Use consistent unit test error threshold of 0.57 minutes for rise/set.
Updated demo test data for slight changes to rise/set prediction times.
Updated doxygen options to issue an error on any warnings.
Fixed the incorrect function name link that doxygen was warning me about.
Refactored the shadow calculator so that the abstract logic is centralized
in a new function CalcShadow. Use that function to calculate the umbra
radius at the peak observation site. Theoretically, any positive value
indicates a total eclipse, but I had to fudge a little to get my calculations
to match the test data.
Documented C versions of SearchGlobalSolarEclipse and NextGlobalSolarEclipse.
Removed ECLIPSE_HYBRID enumeration value. Not going to use it.
Reworded structure documentation to indicate that the eclipse
kind refers to the peak observer only.
Use sidereal time to calculate the longitude of the point
on the Earth's surface where the Moon's shadow ray strikes it.
In the unit test, ignore glancing blows, but if the shadow
ray passes within 6100 km of the Earth's center, verify that
the total angular error is within about a quarter degree.
When there is a total or annular eclipse at the peak time and location,
I am calculating the geographic latitude of that peak within
1.006 degrees. I am disappointed by how sloppy that is, so I
will have to double-check all the math, especially related
to correcting for the Earth's oblateness.
There is no need to use absolute value, and it makes the logic
easier for me to understand if I express each of the inequalities
in terms of addition rather than subtraction.
