Sun-synchronous orbit

A Sun-synchronous orbit (SSO, also called a heliosynchronous orbit[1]) is a nearly polar orbit around a planet, in which the satellite passes over any given point of the planet's surface at the same local mean solar time.[2][3] More technically, it is an orbit arranged so that it precesses through one complete revolution each year, so it always maintains the same relationship with the Sun.

Diagram showing the orientation of a Sun-synchronous orbit (green) at four points in the year. A non-Sun-synchronous orbit (magenta) is also shown for reference. Dates are shown in white: day/month.

Applications

A Sun-synchronous orbit is useful for imaging, spy, and weather satellites,[4] because every time that the satellite is overhead, the surface illumination angle on the planet underneath it will be nearly the same. This consistent lighting is a useful characteristic for satellites that image the Earth's surface in visible or infrared wavelengths, such as weather and spy satellites; and for other remote-sensing satellites, such as 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.

Diagram showing a Sun-synchronous orbit from a top view of the ecliptic plane with Local Solar Time (LST) zones for reference and a descending node of 10:30 am. The LST zones show how the local time beneath the satellite varies at different latitudes and different points on its orbit.

Special cases of the Sun-synchronous orbit are the noon/midnight orbit, where the local mean solar time of passage for equatorial latitudes is around noon or midnight, and the dawn/dusk orbit, where the local mean solar time of passage for equatorial latitudes is around sunrise or sunset, so that the satellite rides the terminator between day and night. Riding the terminator is useful for active radar satellites, as the satellites' solar panels can always see the Sun, without being shadowed by the Earth. It is also useful for some satellites with passive instruments that need to limit the Sun's influence on the measurements, as it is possible to always point the instruments towards the night side of the Earth. The dawn/dusk orbit has been used for solar-observing scientific satellites such as Yohkoh, TRACE, Hinode and PROBA2, affording them a nearly continuous view of the Sun.

Orbital precession

A Sun-synchronous orbit is achieved by having the osculating orbital plane precess (rotate) approximately one degree eastward each day with respect to the celestial sphere to keep pace with the Earth's movement around the Sun.[5] This precession is achieved by tuning the inclination to the altitude of the orbit (see Technical details) such that Earth's equatorial bulge, which perturbs inclined orbits, causes the 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 around Earth are about 600–800 km in altitude, with periods in the 96–100-minute range, and inclinations of around 98°. This is slightly retrograde compared to the direction of Earth's rotation: 0° represents an equatorial orbit, and 90° represents a polar orbit.[5]

Sun-synchronous orbits can happen around other oblate planets, such as Mars. A satellite around the almost spherical Venus, for example, will need an outside push to maintain a Sun-synchronous orbit.

Technical details

The angular precession per orbit for an Earth orbiting satellite is given by

\Delta \Omega =-3\pi {\frac {J_{2}R_{E}^{2}}{p^{2}}}\cos i,

where

J 2

is the coefficient for the second zonal term (1.08263×10⁻³) related to the oblateness of the Earth (see geopotential model),

R E

is the mean radius of the Earth, roughly 6378 km

p

is the semi-latus rectum of the orbit,

i

is the inclination of the orbit to the equator.

An orbit will be Sun-synchronous when the precession rate $ρ$ equals the mean motion of the Earth about the Sun, which is 360° per sidereal year (1.99096871×10⁻⁷ rad/s), so we must set $Δ Ω / T = ρ$ , where $T$ is the orbital period.

As the orbital period of a spacecraft is

2\pi {\sqrt {\frac {a^{3}}{\mu }}}

where $a$ is the semi-major axis of the orbit and $μ$ is the standard gravitational parameter of the planet (398600.440 km³/s² for Earth); as $p \approx a$ for a circular or almost circular orbit, it follows that

\rho \approx -{\frac {3J_{2}R_{E}^{2}{\sqrt {\mu }}\cos i}{2a^{\frac {7}{2}}}}=-\left(360^{\circ }{\text{ per year}}\right)\times \left({\frac {a}{12\,352{\text{ km}}}}\right)^{-{\frac {7}{2}}}\cos i=-\left(360^{\circ }{\text{ per year}}\right)\times \left({\frac {T}{3.795{\text{ h}}}}\right)^{-{\frac {7}{3}}}\cos i,

or when $ρ$ is 360° per year,

\cos i\approx -{\frac {2\rho }{3J_{2}R_{E}^{2}{\sqrt {\mu }}}}a^{\frac {7}{2}}=-\left({\frac {a}{12\,352{\text{ km}}}}\right)^{\frac {7}{2}}=-\left({\frac {T}{3.795{\text{ h}}}}\right)^{\frac {7}{3}}

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°.

Note that according to this approximation $cos i$ equals −1 when the semi-major axis equals 12352 km, which means that only smaller orbits can be Sun-synchronous. The period can be in the range from 88 minutes for a very low orbit ( $a$ = 6554 km, $i$ = 96°) to 3.8 hours ( $a$ = 12352 km, but this orbit would be equatorial with $i$ = 180°). A period longer than 3.8 hours may be possible by using an eccentric orbit with $p$ < 12352 km but $a$ > 12352 km.

If one wants a satellite to fly over some given spot on Earth every day at the same hour, it can do between 7 and 16 orbits per day, as shown in the following table. (The table has been calculated assuming the periods given. The orbital period that should be used is actually slightly longer. For instance, a retrograde equatorial orbit that passes over the same spot after 24 hours has a true period about 365/364 ≈ 1.0027 times longer than the time between overpasses. For non-equatorial orbits the factor is closer to 1.)

Orbits per day	Period (h)		Height above Earth's surface (km)	Maximal latitude	Incli- nation
16	1+1/2	= 1:30	000274	83.4°	096.6°
15	1+3/5	= 1:36	000567	82.3°	097.7°
14	1+5/7	≈ 1:43	000894	81.0°	099.0°
13	1+11/13	≈ 1:51	001262	79.3°	100.7°
12	2		001681	77.0°	103.0°
11	2+2/11	≈ 2:11	002162	74.0°	106.0°
10	2+2/5	= 2:24	002722	69.9°	110.1°
09	2+2/3	= 2:40	003385	64.0°	116.0°
08	3		004182	54.7°	125.3°
07	3+3/7	≈ 3:26	005165	37.9°	142.1°

When one says that a Sun-synchronous orbit goes over a spot on the Earth at the same local time each time, this refers to mean solar time, not to apparent solar time. The Sun will not be in exactly the same position in the sky during the course of the year (see Equation of time and Analemma).

Sun-synchronous orbits are mostly selected for Earth observation satellites, with an altitude typically between 600 and 1000 km over the Earth surface. Even if an orbit remains Sun-synchronous, however, other orbital parameters such as argument of periapsis and the orbital eccentricity will evolve, due to higher order perturbations in the Earth's gravitational field, the pressure of sunlight, and other causes. Earth observation satellites, in particular, prefer orbits with constant altitude when passing over the same spot. Careful selection of eccentricity and location of perigee reveals specific combinations where the perturbations largely cancel and hence the orbit is relatively stable – a frozen orbit. The ERS-1, ERS-2 and Envisat of European Space Agency, as well as the MetOp spacecraft of EUMETSATand RADARSAT-2 of the Canadian Space Agency, are all operated in such Sun-synchronous frozen orbits.[6]

gollark: It's not a huge obstacle if we just upscale humans to the size of galaxies or something.

gollark: Probably more.

gollark: I think that's probably around a solar system worth of mass.

gollark: If you do all 1024-long nucleotide sequences, you will need at least 32317006071311007300714876688669951960444102669715484032130345427524655138867890893197201411522913463688717960921898019494119559150490921095088152386448283120630877367300996091750197750389652106796057638384067568276792218642619756161838094338476170470581645852036305042887575891541065808607552399123930385521914333389668342420684974786564569494856176035326322058077805659331026192708460314150258592864177116725943603718461857357598351152301645904403697613233287231227125684710820209725157101726931323469678542580656697935045997268352998638215525166389437335543602135433229604645318478604952148193555853611059596230656 mRNA things.

gollark: FEAR cyanobacteria.

References

Tscherbakova, N. N.; Beletskii, V. V.; Sazonov, V. V. (1999). "Stabilization of heliosynchronous orbits of an Earth's artificial satellite by solar pressure". Cosmic Research. 37 (4): 393–403. Bibcode:1999KosIs..37..417S.
"SATELLITES AND ORBITS" (PDF).
"Types of Orbits". marine.rutgers.edu. Retrieved 2017-06-24.
Our Changing Planet: The View from Space (1st ed.). Cambridge University Press. 2007. pp. 339. ISBN 978-0521828703.
Rosengren, M. (November 1992). "ERS-1 - An Earth Observer that exactly follows its Chosen Path". ESA Bulletin (72). Bibcode:1992ESABu..72...76R.
Rosengren, Mats (1989). "Improved technique for Passive Eccentricity Control (AAS 89-155)". Advances in the Astronautical Sciences. 69. AAS/NASA. Bibcode:1989ommd.proc...49R.

External links

List of satellites in Sun-synchronous orbit

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[shcherbakova-1] Tscherbakova, N. N.; Beletskii, V. V.; Sazonov, V. V. (1999). "Stabilization of heliosynchronous orbits of an Earth's artificial satellite by solar pressure". Cosmic Research. 37 (4): 393–403. Bibcode:1999KosIs..37..417S.

[2] "SATELLITES AND ORBITS" (PDF).

[3] "Types of Orbits". marine.rutgers.edu. Retrieved 2017-06-24.

[4] Our Changing Planet: The View from Space (1st ed.). Cambridge University Press. 2007. pp. 339. ISBN 978-0521828703.

[me-5] Rosengren, M. (November 1992). "ERS-1 - An Earth Observer that exactly follows its Chosen Path". ESA Bulletin (72). Bibcode:1992ESABu..72...76R.

[6] Rosengren, Mats (1989). "Improved technique for Passive Eccentricity Control (AAS 89-155)". Advances in the Astronautical Sciences. 69. AAS/NASA. Bibcode:1989ommd.proc...49R.