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A heliosynchronous orbit, or more commonly a sun-synchronous orbit, is also a geocentric orbit which combines altitude and inclination in such a way that an object on that orbit passes over any given point of the Earth's surface at the same local 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, spy and remote sensing satellites). There is, of course, a yearA year is the time between two recurrences of an event related to the orbit of the Earth around the Sun. By extension, this can be applied to any planet: for example, "Martian year". Seasonal year A seasonal year is the time between successive recurrencesly oscillation of the actual solar time of passage because of the eccentricity of the Earth's orbit (see analemmaMars Earth The analemma is a plot of the different positions of the Sun in the celestial sphere recorded at a certain point in time(at 24 hour intervals) and from the same location along the calendar year. Due to the earth's tilt on its axis (23. 5°) and).
For example, a satellite's heliosynchronous orbit might cross the equator twelve times a day each time at 15:00 local time. This is achieved by having the orbital plane of the orbit precess (rotate) approximately one degree each day, eastward, to keep pace with the Earth's revolution around the sun.
This is possible for a range of altitudes (typically 600–800 km, for periods in the 96–100 minA minute is: a unit of time equal to 1/60th of an hour and to 60 seconds. Some rare minutes have 59 or 61 seconds; see leap second. a unit of angle, 1/60th of a degree. It is then also known as a minute of angle or minute of arc and can further be divided range) because the Earth's equatorIn geography, the equator is an imaginary line drawn around a planet, halfway between the poles, where the surface of the roughly spherical planet is parallel to the axis of rotation. The equator divides the surface into the Northern Hemisphere and the Soial bulge causes a satellite's orbit to precess at a rate which depends on the orbit's inclination (about 98 ° for the aforementioned altitudes), allowing one to pick an inclination that will cause just the right amount of precession (360° per year). Variations on this type of orbit are possible; a satellite could have a highly eccentric heliosynchronous orbit, in which case the "fixed solar time of passage" only holds for a chosen point of the orbit (typically the perigee). The orbital period chosen depends on the desired revisit rate; the satellite crosses the equator at the same solar time on every passage, but it'll usually be at a different longitude since the Earth rotates underneath it. For example, an orbital period of 96 min, which divides evenly into the Earth solar day (15 times) means the satellite will cross at fifteen different longitudes on consecutive orbits, looping back to the first longitude every fifteenth passage, once per day.
Special cases of heliosynchronous orbit are the noon/midnight orbit, where the local solar time of passage for equatorial longitudes is around noon or midnight, and the dawn/dusk orbit, where the local solar time of passage for equatorial longitudes is around sunrise or sunset.
As the satellite's altitude increases, so does the required inclination, so that the usefulness of the orbit decreases doubly: first because the satellite's photographs are taken from ever farther away, and second because the increasing inclination means the satellite won't fly over higher latitudes. A heliosynchronous satellite designed to fly over the continental United States, for example, would need its inclination to be 132° or less, which means an altitude of ~4600 km or less.
Heliosynchronous orbits are possible around other planets, such as Mars.