Solar and Sidereal Times relationship

Fundamentals
Title	Solar and Sidereal Times relationship
Author(s)	J. Sanz Subirana, J.M. Juan Zornoza and M. Hernández-Pajares, Technical University of Catalonia, Spain.
Level	Basic
Year of Publication	2011

There is a slight difference between a sidereal day and a solar (or synodic day) due to the relative movement between the sun and the earth as a consequence of its annual translation. Figure 1 illustrates the concept.

As it is shown in Figure 1, the Aries reference point ([math]\displaystyle{ \gamma }[/math]), as seen from the earth, apparently moves clockwise during the course of one year (with respect to the sun reference). After one year, the sun and Aries directions coincide again, but the number of laps relative to the sun (solar days) is one less than those relative to Aries (sidereal days).

Figure 1: Solar and Sidereal Time.

The difference between the mean sidereal day and mean solar day can be derived approximately as follows: As in a Solar Tropic year , the mean solar time delayed 1 day respect to the mean sidereal time, thence:

[math]\displaystyle{ \frac{24^h}{365.2422}\simeq 3^m56^s \qquad \mbox{(1)} }[/math]

Thence, a sidereal day is shorter than the solar day for about [math]\displaystyle{ 3^m56 }[/math].

The conversion between UT1 and Apparent and Mean Sidereal Time is given by equations (2) and (3) (see CEP to ITRF article)

[math]\displaystyle{ \Theta_{_G}=\theta_{_G} +\alpha _E \qquad \mbox{(2)} }[/math]

[math]\displaystyle{ \theta_{G_0}=6^h41^m 50^s_{\cdot}54841+8640184_{\cdot}^s812866\,T_u+0_{\cdot}^s093104\,T_u^2-6^s_{\cdot}2 \, 10^{-6}\, T_u^3 \qquad \mbox{(3)} }[/math]