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%[format]?argument
special texts%[format]o[*][mode]ISO6709:1983coordinate[,[+]mmmmhh:[mm]]
references the approximate time of sunrise by default,
%[format]s[*][mode]ISO6709:1983coordinate[,[+]mmmmhh:[mm]]
references the approximate time of sunset by default,
%[format]u[*][mode]ISO6709:1983coordinate[,[+]mmmmhh:[mm]]
references the approximate period of visibility of the Sun
(solar day length) by default,
%[format]z[*][mode]ISO6709:1983coordinate[,[+]mmmmhh:[mm]]
references the approximate period of nonvisibility of the Sun
(solar night length) by default.
All these special texts can be used for at pleasure any geographic point location, i.e. it is possible to determine different astronomical values for any location on the globe, and that for at pleasure any clocktime with a resolution of a single minute within the period of the years AD 1 until AD 9999, that is respected by Gcal.
The selection which value has to be calculated by these special texts is done by specifying the mode part of the preceding argument. Actually, exactly 54 different modes can be used that are represented by the ‘0’…‘9’, ‘a’…‘z’ and ‘A’…‘R’ characters, and which create different kind of results that are depending on the special text used. First of all, here is a table in which all usable modes are described and explained sufficiently. You can also see from this table, which Sun oriented special text or texts are corresponding to which mode, i.e. cause the determination of an astronomical value as it is described in the table:
Mode  Special text  Description 
0
 o , s  Calculates the approximate midnight time of the Sun. The astronomical midnight time of the Sun is at that clocktime, when the Sun holds an azimuth (horizontal angular distance between the vertical circle, that passes the Sun, and the North point) of either precisely 0 degrees of precisely 180 degrees (noon line), which depends on the season and the geographical location. At that clocktime, the Sun is close its lowest culmination point, i.e. close the lowest point below or above the horizontal plane the Sun transits during this day. 
1
 o , s  Calculates the approximate noon time of the Sun. The astronomical noon time of the Sun is at that clocktime, when the Sun holds an azimuth of either precisely 180 degrees of precisely 0 degrees (noon line), which depends on the season and the geographical location. At that clocktime, the Sun is close its highest culmination point, i.e. close the highest point above or below the horizontal plane the Sun transits during this day. People of Islamic faith normally pray for the second time on the day during the period, which is between the astronomical noon time of the Sun (or some minutes later) and the Islamic prayer time by the name of Asr. These people commonly use the term Zuhr for this prayer time. The timing of Asr depends on the length of the shadow cast by a vertical pole (gnomon). According to the Shafi school of jurisprudence, Asr begins when the length of the shadow of a vertical pole exceeds the length of the pole. According to the Hanafi school of jurisprudence, Asr begins when the length of the shadow exceeds twice the length of the vertical pole. In both cases, the minimum length of the shadow at astronomical noon time of the Sun is subtracted from the length of the shadow before comparing it with the length of the pole. See Islamic Asr1 prayer time, and Islamic Asr2 prayer time, for further details. 
2
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 0 degrees on a mathematicalgeocentric horizon in the morning; thus rising. A mathematical horizon is a purely geometricallybuilt horizon which disregards the phenomenon of refraction as it arises in reality by the influence of the Earth’s atmosphere. A geocentrical horizon is the horizontal plane that passes through the Earth’s center, orthogonal to the observer’s local vertical. In the further context, the shorter term mathematical horizon is used which actually means the mathematicalgeocentric horizon. 
2
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 0 degrees on a mathematical horizon in the evening; thus setting. 
2
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 0 degrees on a mathematical horizon; thus is visible. 
2
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 0 degrees on a mathematical horizon; thus is nonvisible. 
3
 o  Calculates the approximate time when the upper limb of the Sun passes a reference altitude of 0 degrees on a mathematical horizon in the morning; thus rising. The above mentioned reference altitude is computed from the value of the Sun’s semidiameter as it appear at that clocktime. If the reference altitude that is referring to the Sun’s upper limb is converted to a reference altitude that is referring to the Sun’s center, this results in a value of about 16 arcminutes below the geocentric horizon. 
3
 s  Calculates the approximate time when the upper limb of the Sun passes a reference altitude of 0 degrees on a mathematical horizon in the evening; thus setting. The above mentioned reference altitude is computed from the value of the Sun’s semidiameter as it appear at that clocktime. 
3
 u  Calculates the approximate period while the upper limb of the Sun is above a reference altitude of 0 degrees on a mathematical horizon; thus is visible. 
3
 z  Calculates the approximate period while the upper limb of the Sun is below a reference altitude of 0 degrees on a mathematical horizon; thus is nonvisible. 
4
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 34 arcminutes below the geocentric horizon in the morning; thus rising. The phenomenon of refraction is already respected in this as it arises in reality by the influence of the Earth’s atmosphere, and that with the standard value of 34 arcminutes, which can indirectly be changed by using the atmosphere option. Fixed dates option atmosphere=airpressure[,temperature], how to change the base data of the atmosphere, so that the atmospheric conditions as defined by it are used to calculate the amount of refraction. 
4
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 34 arcminutes below the geocentric horizon in the evening; thus setting. The phenomenon of refraction is already respected in this as it arises in reality by the influence of the Earth’s atmosphere, and that with the standard value of 34 arcminutes, which can indirectly be changed by using the atmosphere option. 
4
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 34 arcminutes below the geocentric horizon; thus is visible. 
4
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 34 arcminutes below the geocentric horizon; thus is nonvisible. 
5
 o  Calculates the approximate time when the upper limb of the Sun passes a reference altitude of 34 arcminutes below the geocentric horizon in the morning; thus rising. This kind of rise time calculation is done according to the standard calculation method as it is commonly used internationally. The phenomenon of refraction is already respected in this as it arises in reality by the influence of the Earth’s atmosphere, and that with the standard value of 34 arcminutes, which can indirectly be changed by using the atmosphere option. Fixed dates option atmosphere=airpressure[,temperature], how to change the base data of the atmosphere, so that the atmospheric conditions as defined by it are used to calculate the amount of refraction. The above mentioned reference altitude is computed from the respective values of the Sun’s semidiameter and (standard) refraction as they appear at that clocktime. If the reference altitude that is referring to the Sun’s upper limb is converted to a reference altitude that is referring to the Sun’s center, this results in a value of about 50 arcminutes below the geocentric horizon. 
5
 s  Calculates the approximate time when the upper limb of the Sun passes a reference altitude of 34 arcminutes below the geocentric horizon in the evening; thus setting. This kind of set time calculation is done according to the standard calculation method as it is commonly used internationally. The phenomenon of refraction is already respected in this as it arises in reality by the influence of the Earth’s atmosphere, and that with the standard value of 34 arcminutes, which can indirectly be changed by using the atmosphere option. The above mentioned reference altitude is computed from the respective values of the Sun’s semidiameter and (standard) refraction as they appear at that clocktime. People of Islamic faith normally pray for the secondlast time on the day at this clocktime, or some minutes later. These people commonly use the term Maghrib for this prayer time. 
5
 u  Calculates the approximate period while the upper limb of the Sun is above a reference altitude of 34 arcminutes below the geocentric horizon; thus is visible. This kind of visibility period calculation is done according to the standard calculation method as it is commonly used internationally. 
5
 z  Calculates the approximate period while the upper limb of the Sun is above a reference altitude of 34 arcminutes below the geocentric horizon; thus is nonvisible. This kind of nonvisibility period calculation is done according to the standard calculation method as it is commonly used internationally. 
6
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 6 degrees below a mathematical horizon in the morning; thus the beginning of civil twilight. The scattered light of the Sun that is remaining at the beginning of the civil twilight phase is in general not yet sufficient for reading outside without artificial illumination. 
6
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 6 degrees below a mathematical horizon in the evening; thus the ending of civil twilight. 
6
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 6 degrees below a mathematical horizon; thus the period, while the center of the Sun is always above 6 degrees. 
6
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 6 degrees below a mathematical horizon; thus the period, while the center of the Sun is always below 6 degrees. 
7
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 12 degrees below a mathematical horizon in the morning; thus the beginning of nautical twilight. The scattered light of the Sun that is remaining at the beginning of the nautical twilight phase is in general not yet sufficient for navigation using a sea horizon. 
7
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 12 degrees below a mathematical horizon in the evening; thus the ending of nautical twilight. 
7
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 12 degrees below a mathematical horizon; thus the period, while the center of the Sun is always above 12 degrees. 
7
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 12 degrees below a mathematical horizon; thus the period, while the center of the Sun is always below 12 degrees. 
8
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 15 degrees below a mathematical horizon in the morning; thus the beginning of amateurastronomical twilight. The scattered light of the Sun that is remaining at the beginning of the amateurastronomical twilight phase is in general yet so faint that most astronomical observations can be made. 
8
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 15 degrees below a mathematical horizon in the evening; thus the ending of amateurastronomical twilight. 
8
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 15 degrees below a mathematical horizon; thus the period, while the center of the Sun is always above 15 degrees. 
8
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 15 degrees below a mathematical horizon; thus the period, while the center of the Sun is always below 15 degrees. 
8
 o  Calculates the approximate time when the center of the Sun passes a reference altitude of 18 degrees below a mathematical horizon in the morning; thus the beginning of astronomical twilight. No appreciable scattered sunlight is remaining at the beginning of the astronomical twilight phase, the sky is completely dark yet. People of Islamic faith normally pray for the first time on the day during the period, which is between this clocktime and the time of standard sunrise. These people commonly use the term Fajr for this prayer time. See Standard rise time of the Sun, for further details. 
9
 s  Calculates the approximate time when the center of the Sun passes a reference altitude of 18 degrees below a mathematical horizon in the evening; thus the ending of astronomical twilight. People of Islamic faith normally pray for the last time on the day at this clocktime, or some minutes later. These people commonly use the term Isha for this prayer time. 
9
 u  Calculates the approximate period while the center of the Sun is above a reference altitude of 18 degrees below a mathematical horizon; thus the period, while the center of the Sun is always above 18 degrees. 
9
 z  Calculates the approximate period while the center of the Sun is below a reference altitude of 18 degrees below a mathematical horizon; thus the period, while the center of the Sun is always below 18 degrees. 
a
 o , s  Calculates the approximate topocentric, apparent elevation of the Sun, thus the vertical angular distance between the Sun’s center and the horizon, in degrees and arcminutes as it happen at civil midnight time. Results with a negative sign signify that the Sun’s center is below the horizon at the moment, and results with a positive sign mean that the momentary center of the Sun is above the horizon. Observations of celestial objects that are done from the surface of the Earth yield in topocentrically based data. The locations of the celestial bodies are often at another place if the data is topocentrically determined instead of determine it geocentrically, i.e. at the fictitious center of the Earth. This is mainly caused by the refraction, which raises a celestial body to another location as it is been in reality. Because the terrestrial globe flattens towards the pole caps and therefore cannot be taken as an ideally shaped sphere, the individual Earth radius between the observer’s location and the center of the Earth also affects the computation of topocentrically based data. 
b
 o , s  Calculates the approximate topocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at civil midnight time. 
c
 o , s  Calculates the approximate topocentric, apparent declination of the Sun, thus the vertical angular distance between the Sun’s center and the celestial equator, in degrees and arcminutes as it happen at civil midnight time. Results with a negative sign signify that the Sun’s center is below the celestial equator at the moment, and results with a positive sign mean that the momentary center of the Sun is below the celestial equator. 
d
 o , s  Calculates the approximate topocentric, apparent ecliptic longitude of the Sun, thus the horizontal angular distance between the Sun’s center and the vernal equinox point on the ecliptic (the zodiacal line or Sun’s orbit), in degrees and arcminutes as it happen at civil midnight time. 
e
 o , s  Calculates the approximate topocentric, apparent right ascension of the Sun, thus the horizontal angular distance between the Sun’s center and the hour circle that passes through the vernal equinox point on the ecliptic, as time value in hours and minutes as it happen at civil midnight time. 
f
 o , s  Calculates the approximate topocentric, apparent distance of the Sun from the Earth in astronomical units as it happen at civil midnight time. An astronomical unit, abbreviated by ae, is equal to the mean distance of the Sun from the Earth, which is about 149,597,870.691 kilometers. 
g
 o , s  Calculates the approximate topocentric, apparent horizontal parallax of the Sun in degrees and arcminutes as it happen at civil midnight time. The horizontal parallax of the Sun specifies the diameter of the Earth as it is seen from the surface of the Sun. 
h
 o , s  Calculates the approximate topocentric, apparent semidiameter of the Sun in degrees and arcminutes as it happen at civil midnight time. 
i
 o , s  Calculates the approximate refraction of the Earth’s atmosphere in degrees and arcminutes as it happen at civil midnight time. 
j
 o , s  Calculates the approximate geocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at civil midnight time. Results with a negative sign signify that the Sun’s center is below the horizon at the moment, and results with a positive sign mean that the momentary center of the Sun is above the horizon. 
k
 o , s  Calculates the approximate geocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at civil midnight time. 
l
 o , s  Calculates the approximate geocentric, apparent declination of the Sun in degrees and arcminutes as it happen at civil midnight time. Results with a negative sign signify that the Sun’s center is below the celestial equator at the moment, and results with a positive sign mean that the momentary center of the Sun is above the celestial equator. 
m
 o , s  Calculates the approximate geocentric, apparent ecliptic longitude of the Sun in degrees and arcminutes as it happen at civil midnight time. 
n
 o , s  Calculates the approximate geocentric, apparent right ascension of the Sun as time value in hours and minutes as it happen at civil midnight time. 
o
 o , s  Calculates the approximate geocentric, apparent distance of the Sun from the Earth in astronomical units as it happen at civil midnight time. 
p
 o , s  Calculates the approximate geocentric, apparent horizontal parallax of the Sun in degrees and arcminutes as it happen at civil midnight time. 
q
 o , s  Calculates the approximate geocentric, apparent semidiameter of the Sun in degrees and arcminutes as it happen at civil midnight time. 
r
 o , s  Calculates the approximate deltat in seconds as it happen at civil midnight time. Deltat is the difference between the Terrestrial Dynamical time (abbreviated by TDT), that was formerly known as Ephemeris time (abbreviated by ET), and the Universal time (UT). Thus, ‘deltat ≡ TDT  UT’. 
s
 o , s  Calculates the approximate, apparent location oriented sidereal time (local sidereal time (LAST), also known as local star time) in hours and minutes as it happen at civil midnight time. A star day is the period between two consecutive upper culminations of the vernal equinox point on the ecliptic in the meridian of the observer’s location. Therefore, the local star time is the momentary period, which is past between the last upper culmination of the vernal equinox point in the meridian of the observer’s location (the momentary hour angle of the vernal equinox point), thus the right ascension of the stars in the observer’s meridian at the moment. 
t
 o , s  Outputs the base time as time value in hours and minutes, for which the dynamical, i.e. depending on the respective clocktime, astronomical data and times of the Sun are calculated. Without a given timeoffset=argument option, the astronomical data and times of the Sun are always calculated for 0 o’clock Universal time (UTC/GMT). See Calendar option timeoffset=argument, for further details. 
u
 o , s  Calculates the approximate Julian date in days as it happen at civil midnight time. See Julian day number, for further information about the Julian date. 
v
 o , s  Calculates the approximate Julian Ephemeris date, thus a Julian date that is corrected by deltat, in days as it happen at civil midnight time. 
w
 o , s  Calculates the approximate difference between true solar time and mean solar time as time value in hours and minutes as it happen at civil midnight time. This socalled equation of time is a correction to be added to the true solar time —as read on a sundial— to obtain the mean solar time. A true solar day is the period between two consecutive lower culminations of the Sun. This entity is taken as the base for deriving the true solar time (as it is also shown by a sundial during the day). A star day is also known as a mean solar day. Because the Sun apparently shifts with respect to the vernal equinox point on the ecliptic due to the Earth’s orbit around the Sun, the star day and the true solar day have a different length. As the true Sun namely moves irregularly through the ecliptic, a fictitious mean Sun with a symmetrical motion through the celestial equator is used for deriving the mean solar time. So, this difference in time is a consequence of the ellipticity and tilt of the Earth’s orbit, causing the irregular apparent movement of the Sun across the sky. 
x
 o , s  Calculates the difference of the approximate topocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at civil midnight time. Results with a negative sign signify that the momentary center of the Sun is at an elevation that is below the momentary elevation of the Moon’s center; thus the Sun is lower than the Moon. Results with a positive sign signify that the momentary center of the Sun is at an elevation that is above the momentary elevation of the Moon’s center; thus the Sun is higher than the Moon. 
y
 o , s  Calculates the difference of the approximate topocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at civil midnight time. The result specifies the horizontal angular distance, by which the momentary center of the Sun is distant from the momentary Moon’s center, and that measured at the vertical circles that pass the Sun and the North point and the Moon and the North point. Results with a negative sign signify that the Moon is to the right (clockwise) of the Sun if one looks to the Sun — or alternatively expressed, that the Sun is to the left (anticlockwise) of the Moon. Results with a positive sign signify that the Moon is to the left (anticlockwise) of the Sun if one looks to the Sun — or alternatively expressed, that the Sun is to the right (clockwise) of the Moon. 
z
 o , s  Calculates the difference of the approximate geocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at civil midnight time. 
A
 o , s  Calculates the difference of the approximate geocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at civil midnight time. 
B
 o  Calculates the difference of the approximate topocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard rise time of the Sun. See Standard rise time of the Sun, for further details. 
B
 s  Calculates the difference of the approximate topocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard set time of the Sun. See Standard set time of the Sun, for further details. 
C
 o  Calculates the difference of the approximate topocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard rise time of the Sun. See Standard rise time of the Sun, for further details. 
C
 s  Calculates the difference of the approximate topocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard set time of the Sun. See Standard set time of the Sun, for further details. 
D
 o  Calculates the difference of the approximate geocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard rise time of the Sun. See Standard rise time of the Sun, for further details. 
D
 s  Calculates the difference of the approximate geocentric, apparent elevation of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard set time of the Sun. See Standard set time of the Sun, for further details. 
E
 o  Calculates the difference of the approximate geocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard rise time of the Sun. See Standard rise time of the Sun, for further details. 
E
 s  Calculates the difference of the approximate geocentric, apparent azimuth of Sun and Moon (delta), at which the Sun is used as the reference point, in degrees and arcminutes as it happen at standard set time of the Sun. See Standard set time of the Sun, for further details. 
F
 o , s  Calculates the difference of the approximate astronomical midnight times of Sun and Moon (delta), at which the Sun is used as the reference point, as time value in hours and minutes as it happen at astronomical midnight time of the Sun. Results with a negative sign signify that the astronomical midnight time of the Sun is earlier than the astronomical midnight time of the Moon; thus the solar midnight is before the lunar midnight. Results with a positive sign signify that the astronomical midnight time of the Sun is later than the astronomical midnight time of the Moon; thus the solar midnight is after the lunar midnight. See Astronomical midnight time of the Sun, and Astronomical midnight time of the Moon, for further details. 
G
 o , s  Calculates the difference of the approximate astronomical noon times of Sun and Moon (delta), at which the Sun is used as the reference point, as time value in hours and minutes as it happen at astronomical noon time of the Sun. Results with a negative sign signify that the astronomical noon time of the Sun is earlier than the astronomical noon time of the Moon; thus the solar noon is before the lunar noon. Results with a positive sign signify that the astronomical noon time of the Sun is later than the astronomical noon time of the Moon; thus the solar noon is after the lunar noon. See Astronomical noon time of the Sun, and Astronomical noon time of the Moon, for further details. 
H
 o  Calculates the difference of the approximate standard rise times of Sun and Moon (delta), at which the Sun is used as the reference point, as time value in hours and minutes as it happen at standard rise time of the Sun. Results with a negative sign signify that the standard rise time of the Sun is earlier than the standard rise time of the Moon; thus the sunrise is before the moonrise. Results with a positive sign signify that the standard rise time of the Sun is later than the standard rise time of the Moon; thus the sunrise is after the moonrise. See Standard rise time of the Sun, and Standard rise time of the Moon, for further details. 
H
 s  Calculates the difference of the approximate standard set times of Sun and Moon (delta), at which the Sun is used as the reference point, as time value in hours and minutes as it happen at standard set time of the Sun. Results with a negative sign signify that the standard set time of the Sun is earlier than the standard set time of the Moon; thus the sunset is before the moonset. Results with a positive sign signify that the standard set time of the Sun is later than the standard set time of the Moon; thus the sunset is after the moonset. See Standard set time of the Sun, and Standard set time of the Moon, for further details. 
I
 o , s  Calculates the approximate topocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at astronomical midnight time of the Sun (topocentric midnight height). See Astronomical midnight time of the Sun, for further details. 
J
 o , s  Calculates the approximate topocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at astronomical midnight time of the Sun (topocentric midnight height). See Astronomical noon time of the Sun, for further details. 
K
 o  Calculates the approximate topocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at standard rise time of the Sun (topocentric rise height). See Standard rise time of the Sun, for further details. 
K
 s  Calculates the approximate topocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at standard set time of the Sun (topocentric set height). See Standard set time of the Sun, for further details. 
L
 o  Calculates the approximate topocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at standard rise time of the Sun (topocentric rise azimuth). The horizontal angular distance between the topocentric rise azimuth and the East direction is also known as the topocentric morning width of the Sun. See Standard rise time of the Sun, for further details. 
L
 s  Calculates the approximate topocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at standard set time of the Sun (topocentric set azimuth). The horizontal angular distance between the topocentric set azimuth and the West direction is also known as the topocentric evening width of the Sun. See Standard set time of the Sun, for further details. 
M
 o , s  Calculates the approximate geocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at astronomical midnight time of the Sun (geocentric midnight height). See Astronomical midnight time of the Sun, for further details. 
N
 o , s  Calculates the approximate geocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at astronomical midnight time of the Sun (geocentric midnight height). See Astronomical noon time of the Sun, for further details. 
O
 o  Calculates the approximate geocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at standard rise time of the Sun (geocentric rise height). See Standard rise time of the Sun, for further details. 
O
 s  Calculates the approximate geocentric, apparent elevation of the Sun in degrees and arcminutes as it happen at standard set time of the Sun (geocentric set height). See Standard set time of the Sun, for further details. 
P
 o  Calculates the approximate geocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at standard rise time of the Sun (geocentric rise azimuth). The horizontal angular distance between the geocentric rise azimuth and the East direction is also known as the geocentric morning width of the Sun. See Standard rise time of the Sun, for further details. 
P
 s  Calculates the approximate geocentric, apparent azimuth of the Sun in degrees and arcminutes as it happen at standard set time of the Sun (geocentric set azimuth). The horizontal angular distance between the geocentric set azimuth and the West direction is also known as the geocentric evening width of the Sun. See Standard set time of the Sun, for further details. 
Q
 o  Calculates the approximate time when the length of the shadow cast by a vertical pole in the forenoon is equal the length of the pole. Nevertheless, the minimum length of the shadow is subtracted from the length of the shadow before comparing it with the length of the pole. See Fixed dates option adjustvalue=argument, how to change the shadow length factor. 
Q
 s  Calculates the approximate time when the length of the shadow cast by a vertical pole in the afternoon is equal the length of the pole. Nevertheless, the minimum length of the shadow is subtracted from the length of the shadow before comparing it with the length of the pole. People of Islamic faith, and that the people holding the Shafi school of jurisprudence, normally pray for the third time on the day at this clocktime, or some minutes later. These people commonly use the term Asr for this prayer time. See Astronomical noon time of the Sun, for more information. And note Fixed dates option adjustvalue=argument, how to change the shadow length factor. 
Q
 u  Calculates the approximate period while the center of the Sun is above a reference altitude, at which the length of the shadow cast by a vertical pole is of single or shorter length than the pole itself. 
Q
 z  Calculates the approximate period while the center of the Sun is below a reference altitude, at which a vertical pole either casts no shadow anymore, or casts a shadow that is longer than the single length of the pole itself. 
R
 o  Calculates the approximate time when the length of the shadow cast by a vertical pole at forenoon is twice the length of the pole. Nevertheless, the minimum length of the shadow is subtracted from the length of the shadow before comparing it with the length of the pole. See Fixed dates option adjustvalue=argument, how to change the shadow length factor. 
R
 s  Calculates the approximate time when the length of the shadow cast by a vertical pole in the afternoon is twice the length of the pole. Nevertheless, the minimum length of the shadow is subtracted from the length of the shadow before comparing it with the length of the pole. People of Islamic faith, and that the people holding the Hanafi school of jurisprudence, normally pray for the third time on the day at this clocktime, or some minutes later. These people commonly use the term Asr for this prayer time. See Astronomical noon time of the Sun, for more information. And note Fixed dates option adjustvalue=argument, how to change the shadow length factor. 
R
 u  Calculates the approximate period while the center of the Sun is above a reference altitude, at which the length of the shadow cast by a vertical pole is of double or shorter length than the pole itself. 
R
 z  Calculates the approximate period while the center of the Sun is below a reference altitude, at which a vertical pole either casts no shadow anymore, or casts a shadow that is longer than twice the length of the pole itself. 
If no mode is given, Gcal automatically uses that mode, which is enabled by the mode character ‘5’. If a mode character is given that is not according to one of the ‘0’…‘9’, ‘a’…‘z’ and ‘A’…‘R’ characters, Gcal also automatically uses that mode, which is enabled by the mode character ‘5’.
Gcal represents the Sun oriented special texts depending on the selected mode using the following types and styles:
n.n…
format by default.
A ‘*’ character that is directly given before some mode characters
causes Gcal to represent the value for another quantity. For the mode
characters, which
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
+n.n…
format by default.
A ‘*’ character that is directly given before a mode character
causes Gcal not to represent such values using another style.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
hh:mm
24hour format by default.
A ‘*’ character that is directly given before a mode character
causes Gcal to represent the clocktime value using the 12hour
format, thus to provide it with a time suffix.
See Actual localtime in hh:mm
format %t[argument]
special text,
for more details about the above mentioned time value template.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations:
??:??
text will be
created instead of the clocktime text.
**:**
text will
be created instead of the clocktime text.
++:++
text will be created instead of the
clocktime text.
:
text will be created instead of the
clocktime text.
hhhmm'
format by default.
A ‘*’ character that is directly given before a mode character
causes Gcal to represent the time value using another style, and that in
decimal hours, i.e. in the hh.h…
format.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
+hhhmm'
format by default.
A ‘*’ character that is directly given before a mode character
causes Gcal to represent the time value using another style, and that in
decimal hours, i.e. in the +hh.h…
format.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
ddddmm'
format by default.
A ‘*’ character that is directly given before a mode character causes
Gcal to represent the angular value using another style, and that in
decimal degrees, i.e. in the ddd.d…
format.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
+ddddmm'
format by default.
A ‘*’ character that is directly given before a mode character causes
Gcal to represent the angular value using another style, and that in
decimal degrees, i.e. in the +ddd.d…
format.
If definite events happen, Gcal displays special event oriented texts instead of using the previously described representations. See Event texts of the Sun oriented special texts, where you can find the event oriented texts that are created for clocktime values, which are schematically and analogously used for the type of representation as it is described here.
After the optional style and mode characters, the latitude and longitude of the geographic coordinates follows, for which the calculations must be made. They must be conform the ISO6709:1983 standard representation of latitude and longitude for geographic point locations, so that the coordinate has to be declared like this:
+
for North and on the equator,

for South of the equator.)
+dd[.dd]
Degrees (2 digits), and optionally decimal degrees
+ddmm[.mm]
Degrees (2 digits), arcminutes (2 digits), and optionally decimal minutes
+ddmmss[.ss]
Degrees (2 digits), arcminutes (2 digits), arcseconds (2 digits), and optionally decimal seconds
+
for East and on the prime meridian (Greenwich),

for West of Greenwich and up to the 180th meridian.)
+ddd[.dd]
Degrees (3 digits), and optionally decimal degrees
+dddmm[.mm]
Degrees (3 digits), arcminutes (2 digits), and optionally decimal minutes
+dddmmss[.ss]
Degrees (3 digits), arcminutes (2 digits), arcseconds (2 digits), and optionally decimal seconds
+
for heights above and on the sea level, 
for heights below
the sea level.)
[+n[n[n[n]]]]
Height in meters (integer number) in range
9999
…+9999
(1…4 digits)
All components of the coordinates must have leadings zeroes in case they have
less digits than the templates shown above. Declared decimal seconds are not
respected by Gcal. Heights which have a negative sign remain unrespected
if Gcal determinates Sun and Moon data and times, respectively. In such a
case, Gcal always uses the height +0
. Latitude and longitude
coordinates, and the height of the observer’s location are connected without
any separating characters, like ‘+40075+61’, ‘+401213.10750015.1’
or ‘+40.20361075.00417+0061’. See the pertinent literature
for more details.
A time value [+]mmmmhh:[mm]
,
which is separated by a ‘,’ character, may trail the coordinate. Such
a time value informs Gcal, about how many minutes mmmm respectively
hours hh and minutes mm the geographic location is displaced
from Universal time (UTC/GMT). This time displacement value defines
the timezone, which is actually valid for this location. If summer and
wintertimes are respected for the location, you should include that change
in time into the timezone value for the period in which the summertime is
valid, by which the clock is put on during the summertime period — such
a change is either subtracted from the timezone value for locations West
of the prime meridian (Greenwich), or it is added for locations East of
the prime meridian, because Gcal is actually unable to perform such
operations automatically!
See Actual local time in hh:mm
format %t[argument]
special text,
for more details about the above mentioned time value template.
If no time displacement value is specified for a given coordinate, Gcal
assumes a time displacement value of 0
, which is equal to the actual
Universal time (UTC/GMT).
The following table informs you about which type of representation is caused by a mode. The previously defined numbering scheme, as it has been used for the introduction of the types of representations, is used as key value in the column that holds the type of representation. The table also contains a column that shows whether a mode enables dynamical values, i.e. values that are depending on the respective clocktime (if you use the timeoffset=argument option, you can change the respective clocktime that is used for calculating such values). In a next table column, it is listed whether the given coordinate of the location influences the determination of a value, and the last column of the table gives you the information whether a given timezone value affects the values determination:
And now some examples to these special texts:
The text ‘Sunrise at %o+5158+00738,120 in MS, BRD’ will be expanded to
→ ‘Sunrise at 05:16 in MS, BRD’, in case the actual system date is the 1st June 1998.
The text ‘Sunset at %s*5+5158+00738,120 in MS, BRD’ will be expanded to
→ ‘Sunset at 09:39pm in MS, BRD’, in case the actual system date is the 1st June 1998.
The text ‘Sun visible %u5+5158+00738,120 in MS, BRD’ will be expanded to
→ ‘Sun visible 16h24' in MS, BRD’, in case the actual system date is the 1st June 1998.
The text ‘Sun nonvisible %z*+5158+00738,120 in MS, BRD’ will be expanded to
→ ‘Sun nonvisible 7.607 in MS, BRD’, in case the actual system date is the 1st June 1998.
The text ‘Sun azimuth 0 o'clock=%s*a+5158+00738,120 in MS, BRD’ will be expanded to
→ ‘Sun azimuth 0 o'clock=339d16' in MS, BRD’, in case the actual system date is the 1st June 1998.
The text ‘Equation of time %ot+00+000=%o*w+00+000,120 BRD’ will be expanded to
→ ‘Equation of time +16h00'=+00h02'13.201" BRD’, in case you call Gcal with the timeoffset=16: and precise options and the actual system date is the 1st June 1998.
The text ‘Julian date at %ot+00+000 =%ou+00+000’ will be expanded to
→ ‘Julian date at +10h15'=2450965.927’, in case you call Gcal with the timeoffset=10:15 option and the actual system date is the 1st June 1998.
Here is a list that reports about the used reference systems in a short manner, describes other aspects that are unmentioned now, and informs about the lacks and limitations that are existing for the Sun oriented special texts:
Please also note the following references:
All Sun oriented special texts must always be trailed by a whitespace character which is removed in output!
Next: Moon data, Previous: Geographical distance and course angle, Up: Replacements with other argument [Contents][Index]