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This page is about a class of orbits about the Earth. For class of orbits around the Sun, see heliosynchronous orbit.

Diagram showing the orientation of a Sun-synchronous orbit (green) in four points of the year. A non-sun-synchronous orbit (magenta) is also shown for reference

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A Sun-synchronous orbit (sometimes called a heliosynchronous orbit) is a geocentric orbit which combines altitude and inclination in such a way that an object on that orbit ascends or descends over any given point of the Earth's surface at the same local mean solar time. The surface illumination angle will be nearly the same every time. This consistent lighting is a useful characteristic for satellites that image the Earth's surface in visible or infrared wavelengths (e.g. weather and spy satellites) and for other remote sensing satellites (e.g. those carrying ocean and atmospheric remote sensing instruments that require sunlight). For example, a satellite in sun-synchronous orbit might ascend across the equator twelve times a day each time at approximately 15:00 mean local time. This is achieved by having the osculating orbital plane precess (rotate) approximately one degree each day with respect to the celestial sphere, eastward, to keep pace with the Earth's revolution around the Sun.

The uniformity of Sun angle is achieved by tuning the inclination to the altitude of the orbit (details in section "Technical details") such that the extra mass near the equator causes orbital plane of the spacecraft to precess with the desired rate: the plane of the orbit is not fixed in space relative to the distant stars, but rotates slowly about the Earth's axis. Typical sun-synchronous orbits are about 600–800 km in altitude, with periods in the 96–100 minute range, and inclinations of around 98° (i.e. slightly retrograde compared to the direction of Earth's rotation: 0° represents an equatorial orbit and 90° represents a polar orbit).

Sun-synchronous orbits are possible around other oblate planets, such as Mars. But for example Venus is too spherical for having a satellite in sun-synchronous orbit.

Technical details

Equation (20) of the article Orbital perturbation analysis (spacecraft) gives that the precession rate of an orbit around an oblate planet is:

$-2\pi \ {\frac {J_{2}}{\mu \ p^{2}}}\ {\frac {3}{2}}\ \cos i\,$

radians per orbit.

As the orbital period of a spacecraft is $2\pi \ a{\sqrt {\frac {a}{\mu }}}\,$ and as $a\approx p\,$ for a circular or almost circular orbit it follows that such an orbit is sun-synchronus if and only if

$\cos i\ =\ -{\frac {\rho \ {\sqrt {\mu }}}{{\frac {3}{2}}\ J_{2}}}\ a^{\frac {7}{2}}\,$

where

$\rho \,$ is the mean motion of the Earth in its orbit around the Sun ($1.99106\cdot 10^{-7}{\text{ radians}}/s\,$)

$\mu \,$ is the gravitational constant of the Earth ($398600.440{\text{ km}}^{3}/s^{2}\,$)

$J_{2}\,$ is the coefficient for the second zonal term ($1.7555\ 10^{10}{\text{ km}}^{5}/s^{2}\,$)

As an example, for a=7200 km (the spacecraft about 800 km over the Earth surface) one gets with this formula a sun-synchronous inclination of 98.696 deg.

The definition of the Local time of the ascending node concept for Sun-synchronous spacecraft is only related to the position of the Sun indirectly through Newcomb's formula which gives the angle between the Greenwich meridian and the Vernal equinox in the form:

$\alpha \ +t\ \ \beta \ +t^{2}\ \ \gamma$

where $t\,$ is the time in days from a reference epoch that corresponds to mid-night at the Greenwich meridian and $\gamma \,$ is an extremely small coefficient. Nowadays one uses 2000/01/01 00:00:00 corresponding to Modified Julian Day zero. This then means (counting angles in radians) that the angle from Vernal equinox to the direction away from the Sun projected down to the equatorial plane must be approximately

$S\ =\ \alpha \ +t\ \ (\beta -2\pi )\ +t^{2}\ \ \gamma$

The right ascension of the ascending node ($\Omega \,$) for a sun-synchronous orbit increases with precisely this rate:

$\beta -2\pi \,$ radian/day ($1.99106\cdot 10^{-7}\ {\text{radian/second}}\,$)

which is the "mean motion" of the Earth in its orbit around the Sun.

The local time of the ascending node in hours is then the constant value

$24\ {\frac {d}{2\pi }}\,$

where $d\,$ is $\Omega -S\,$ reduced modulo $2\pi \,$ to the interval

$0\leq d<2\pi \,$

The local time of the descending node is obtained by adding (or subtracting) 12 hours

The Sun-synchronous orbit is mostly selected for Earth observation satellites that should be operated at a relatively constant altitude suitable for its Earth observation instruments, this altitude typically being between 600 km and 1000 km over the Earth surface. Because of the deviations of the gravitational field of the Earth from that of a homogeneous sphere that are quite significant at such relatively low altitudes a strictly circular orbit is not possible for these satellites. Very often a frozen orbit is therefore selected that is slightly higher over the Southern hemisphere than over the Northern hemisphere. ERS-1, ERS-2 and Envisat of European Space Agency as well as the MetOp spacecraft of the European Organisation for the Exploitation of Meteorological Satellites are all operated in Sun-synchronous, "frozen" orbits.

See also

• Orbital perturbation analysis (spacecraft)
• Analemma
• Geosynchronous orbit
• Geostationary orbit
• List of orbits
• Polar orbit
• World Geodetic System

References

• Sandwell, David T., The Gravity Field of the Earth - Part 1 (2002) (p. 8)
• Sun-Synchronous Orbit dictionary entry, from U.S. Centennial of Flight Commission
• NASA Q&A