++ed by:
Tom Wyant
and 1 contributors

# NAME

Astro::Coord::ECI::Sun - Compute the position of the Sun.

# SYNOPSIS

`````` use Astro::Coord::ECI;
use Astro::Coord::ECI::Sun;

# 1600 Pennsylvania Ave, Washington DC USA
# latitude 38.899 N, longitude 77.038 W,
# altitude 16.68 meters above sea level
my \$alt = 16.68 / 1000;        # Kilometers
my \$sun = Astro::Coord::ECI::Sun->new ();
my \$sta = Astro::Coord::ECI->
universal (time ())->
geodetic (\$lat, \$long, \$alt);
my (\$time, \$rise) = \$sta->next_elevation (\$sun);
print "Sun @{[\$rise ? 'rise' : 'set']} is ",
scalar gmtime \$time, " UT\n";``````

Although this example computes the Sun rise or set in Washington D.C. USA, the time is displayed in Universal Time. This is because I did not want to complicate the example by adding machinery to convert the time to the correct zone for Washington D.C. (which is UT - 5 except when Summer Time is in effect, when it is UT - 4).

# DESCRIPTION

This module implements the position of the Sun as a function of time, as described in Jean Meeus' "Astronomical Algorithms," second edition. It is a subclass of Astro::Coord::ECI, with the id, name, and diameter attributes initialized appropriately, and the time_set() method overridden to compute the position of the Sun at the given time.

## Methods

The following methods should be considered public:

\$sun = Astro::Coord::ECI::Sun->new();

This method instantiates an object to represent the coordinates of the Sun. This is a subclass of Astro::Coord::ECI, with the id and name attributes set to 'Sun', and the diameter attribute set to 1392000 km per Jean Meeus' "Astronomical Algorithms", 2nd Edition, Appendix I, page 407.

Any arguments are passed to the set() method once the object has been instantiated. Yes, you can override the "hard-wired" id, name, and so forth in this way.

If \$Astro::Coord::ECI::Sun::Singleton is true, you get a singleton object; that is, only one object is instantiated and subsequent calls to new() just return that object. This only works if Scalar::Util exports weaken(). If it does not, the setting of \$Astro::Coord::ECI::Sun::Singleton is silently ignored. The default is true if Scalar::Util can be loaded and exports weaken(), and false otherwise.

@almanac = \$sun->almanac(\$location, \$start, \$end);

This method produces almanac data for the Sun for the given location, between the given start and end times. The location is assumed to be Earth-Fixed - that is, you can't do this for something in orbit.

The `\$location` argument may be omitted if the `station` attribute has been set. That is, this method can also be called as

`` @almanac = \$sun->almanac( \$start, \$end )``

The start time defaults to the current time setting of the \$sun object, and the end time defaults to a day after the start time.

The almanac data consists of a list of list references. Each list reference points to a list containing the following elements:

`````` [0] => time
[1] => event (string)
[2] => detail (integer)
[3] => description (string)``````

The @almanac list is returned sorted by time.

The following events, details, and descriptions are at least potentially returned:

`````` horizon: 0 = Sunset, 1 = Sunrise;
transit: 0 = local midnight, 1 = local noon;
twilight: 0 = end twilight, 1 = begin twilight;
quarter: 0 = spring equinox, 1 = summer solstice,
2 = fall equinox, 3 = winter solstice.``````

Twilight is calculated based on the current value of the twilight attribute of the \$sun object. This attribute is inherited from Astro::Coord::ECI, and documented there.

@almanac = \$sun->almanac_hash(\$location, \$start, \$end);

This convenience method wraps \$sun->almanac(), but returns a list of hash references, sort of like Astro::Coord::ECI::TLE->pass() does. The hashes contain the following keys:

``````  {almanac} => {
{event} => the event type;
{detail} => the event detail (typically 0 or 1);
{description} => the event description;
}
{body} => the original object (\$sun);
{station} => the observing station;
{time} => the time the quarter occurred.``````

The {time}, {event}, {detail}, and {description} keys correspond to elements 0 through 3 of the list returned by almanac().

\$elevation = \$tle->correct_for_refraction( \$elevation )

This override of the superclass' method simply returns the elevation passed to it. I have no algorithm for refraction at the surface of the photosphere or anywhere else in the environs of the Sun, and explaining why I make no correction at all seemed easier than explaining why I make an incorrect correction.

See the Astro::Coord::ECI `azel()` and `azel_offset()` documentation for whether this class' `correct_for_refraction()` method is actually called by those methods.

\$longitude = \$sun->ecliptic_longitude ();

This method returns the ecliptic longitude of the sun at its current time setting, in radians. It is really just a convenience method, since it is equivalent to (\$sun->ecliptic)[1], and in fact that is how it is implemented.

\$long = \$sun->geometric_longitude ()

This method returns the geometric longitude of the Sun in radians at the last time set.

(\$point, \$intens, \$central) = magnitude (\$theta, \$omega);

This method returns the magnitude of the Sun at a point \$theta radians from the center of its disk, given that the disk's angular radius (not diameter) is \$omega radians. The returned \$point is the magnitude at the given point (undef if \$theta > \$omega), \$intens is the ratio of the intensity at the given point to the central intensity (0 if \$theta > \$omega), and \$central is the central magnitude.

If this method is called in scalar context, it returns \$point, the point magnitude.

If the \$omega argument is omitted or undefined, it is calculated based on the geocentric range to the Sun at the current time setting of the object.

If the \$theta argument is omitted or undefined, the method returns the average magnitude of the Sun, which is taken to be -26.8.

The limb-darkening algorithm and the associated constants come from http://en.wikipedia.org/wiki/Limb_darkening.

(\$time, \$quarter, \$desc) = \$sun->next_quarter(\$want);

This method calculates the time of the next equinox or solstice after the current time setting of the \$sun object. The return is the time, which equinox or solstice it is as a number from 0 (vernal equinox) to 3 (winter solstice), and a string describing the equinox or solstice. If called in scalar context, you just get the time.

The optional \$want argument says which equinox or solstice you want.

As a side effect, the time of the \$sun object ends up set to the returned time.

The method of calculation is successive approximation, and actually returns the second after the calculated equinox or solstice.

Since we only calculate the Sun's position to the nearest 0.01 degree, the calculated solstice or equinox may be in error by as much as 15 minutes.

\$hash_reference = \$moon->next_quarter_hash(\$want);

This convenience method wraps \$moon->next_quarter(), but returns the data in a hash reference, sort of like Astro::Coord::ECI::TLE->pass() does. The hash contains the following keys:

``````  {body} => the original object (\$moon);
{almanac} => {
{event} => 'quarter',
{detail} => the quarter number (0 through 3);
{description} => the quarter description;
}
{time} => the time the quarter occurred.``````

The {time}, {detail}, and {description} keys correspond to elements 0 through 2 of the list returned by next_quarter().

\$period = \$sun->period ()

Although this method is attached to an object that represents the Sun, what it actually returns is the sidereal period of the Earth, per Appendix I (pg 408) of Jean Meeus' "Astronomical Algorithms," 2nd edition.

\$sun->time_set ()

This method sets coordinates of the object to the coordinates of the Sun at the object's currently-set universal time. The velocity components are arbitrarily set to 0. The 'equinox_dynamical' attribute is set to the object's currently-set dynamical time.

Although there's no reason this method can't be called directly, it exists to take advantage of the hook in the Astro::Coord::ECI object, to allow the position of the Sun to be computed when the object's time is set.

The algorithm comes from Jean Meeus' "Astronomical Algorithms", 2nd Edition, Chapter 25, pages 163ff.

# ACKNOWLEDGMENTS

The author wishes to acknowledge Jean Meeus, whose book "Astronomical Algorithms" (second edition) formed the basis for this module.

The Astro-MoonPhase package by Brett Hamilton, which contains a function-based module to compute the current phase, distance and angular diameter of the Moon, as well as the angular diameter and distance of the Sun.

The Astro-Sunrise package by Ron Hill, which contains a function-based module to compute sunrise and sunset for the given day and location.

The Astro-SunTime package by Rob Fugina, which provides functionality similar to Astro-Sunrise.

# AUTHOR

Thomas R. Wyant, III (wyant at cpan dot org)