# Quasi-satellite

A quasi-satellite is an object in a specific type of co-orbital configuration (1:1 orbital resonance) with a planet (or dwarf planet) where the object stays close to that planet over many orbital periods.
A quasi-satellite's orbit around the Sun takes the same time as the planet's, but has a different eccentricity (usually greater), as shown in the diagram. When viewed from the perspective of the planet by an observer facing the Sun, the quasi-satellite will appear to travel in an oblong retrograde loop around the planet. (See Analemma § Of quasi-satellites).
In contrast to true satellites, quasi-satellite orbits lie outside the planet's Hill sphere, and are unstable. Over time they tend to evolve to other types of resonant motion, where they no longer remain in the planet's neighborhood, then possibly later move back to a quasi-satellite orbit, etc.
Other types of orbit in a 1:1 resonance with the planet include horseshoe orbits and tadpole orbits around the Lagrangian points, but objects in these orbits do not stay near the planet's longitude over many revolutions about the star. Objects in horseshoe orbits are known to sometimes periodically transfer to a relatively short-lived quasi-satellite orbit, and are sometimes confused with them. An example of such an object is 2002 AA29.
A quasi-satellite is similar to an object in a distant retrograde orbit, in a different context. The latter term is usually used for a space probe or artificial satellite in a retrograde orbit around a moon, and the period may be much shorter than that of the moon, whereas the term "quasi-satellite" usually refers to an object like an asteroid whose period is similar to that of the planet of which it is considered to be a quasi-satellite. But in both cases, the object (asteroid, space probe) viewed in a reference frame that rotates with the two main objects (once a year for Sun-Earth, once a month for Earth-Moon) appears to move retrograde compared to that rotation, thus lengthening its sidereal period. So a quasi-satellite (with low inclination) tends to stay in certain constellations rather than going through the whole zodiac. Quasi-satellites with high eccentricity can get quite far from their planet, more than an astronomical unit for quasi-satellites of Earth such as 2014 OL339.
The word "geosynchronous" is sometimes used to describe quasi-satellites of the Earth, because their motion around the Sun is synchronized with Earth's. However, this usage is unconventional and confusing. Conventionally, geosynchronous satellites revolve in the prograde sense around the Earth, with orbital periods that are synchronized to the Earth's rotation.

## Examples
### Venus

Venus has one known quasi-satellite, 524522 Zoozve. This asteroid is also a Mercury- and Earth-crosser; it seems to have been a "companion" to Venus for approximately the last 7,000 years only, and is destined to be ejected from this orbital arrangement about 500 years from now.

### Earth

As of 2023, Earth had seven known quasi-satellites:
* 164207 Cardea
* (277810) 2006 FV35
* 2013 LX28
* 2014 OL339
* 469219 Kamoʻoalewa
* 2020 PP1
* 2023 FW13
On the longer term, asteroids can transfer between quasi-satellite orbits and horseshoe orbits, which circulate around Lagrangian points L4 and L5. By 2016, orbital calculations showed that all five of Earth's then known quasi-satellites repeatedly transfer between horseshoe and quasi-satellite orbits. 3753 Cruithne, 2002 AA29, 2003 YN107 and 2015 SO2 are minor planets in horseshoe orbits that might evolve into a quasi-satellite orbit. The time spent in the quasi-satellite phase differs from asteroid to asteroid. Quasi-satellite 2016 HO$_3$ is predicted to be stable in this orbital state for several hundred years, in contrast to 2003 YN$_{107}$ which was a quasi-satellite from 1996 to 2006 but then departed Earth's vicinity on a horseshoe orbit.
469219 Kamoʻoalewa (2016 HO$_3$) is thought to be one of the most stable quasi-satellites found yet of Earth. It stays between 38 and 100 lunar distances from the Earth.
Known and suspected companions of Earth vte :
| Name | Eccentricity | Diameter (m) | Discoverer | Date of Discovery | Type | Current Type |
| Moon | 0.055 | 3474800 | ? | Prehistory | Natural satellite | Natural satellite |
| 1913 Great Meteor Procession | ? | ? | ? | 1913-02-09 | Possible Temporary satellite | Destroyed |
| 3753 Cruithne | 0.515 | 5000 | Duncan Waldron | 1986-10-10 | Quasi-satellite | Horseshoe orbit |
| 1991 VG | 0.053 | 5–12 | Spacewatch | 1991-11-06 | Temporary satellite | Apollo asteroid |
| (85770) 1998 UP1 | 0.345 | 210–470 | Lincoln Lab's ETS | 1998-10-18 | Horseshoe orbit | Horseshoe orbit |
| 54509 YORP | 0.230 | 124 | Lincoln Lab's ETS | 2000-08-03 | Horseshoe orbit | Horseshoe orbit |
| 2001 GO2 | 0.168 | 35–85 | Lincoln Lab's ETS | 2001-04-13 | Possible Horseshoe orbit | Possible Horseshoe orbit |
| 2002 AA29 | 0.013 | 20–100 | LINEAR | 2002-01-09 | Quasi-satellite | Horseshoe orbit |
| 2003 YN107 | 0.014 | 10–30 | LINEAR | 2003-12-20 | Quasi-satellite | Horseshoe orbit |
| (164207) 2004 GU9 | 0.136 | 160–360 | LINEAR | 2004-04-13 | Quasi-satellite | Quasi-satellite |
| (277810) 2006 FV35 | 0.377 | 140–320 | Spacewatch | 2006-03-29 | Quasi-satellite | Quasi-satellite |
| 2006 JY26 | 0.083 | 6–13 | Catalina Sky Survey | 2006-05-06 | Horseshoe orbit | Horseshoe orbit |
| 2006 RH120 | 0.024 | 2–3 | Catalina Sky Survey | 2006-09-13 | Temporary satellite | Apollo asteroid |
| (419624) 2010 SO16 | 0.075 | 357 | WISE | 2010-09-17 | Horseshoe orbit | Horseshoe orbit |
| (706765) 2010 TK7 | 0.191 | 150–500 | WISE | 2010-10-01 | Earth trojan | Earth trojan |
| 2013 BS45 | 0.083 | 20–40 | Spacewatch | 2010-01-20 | Horseshoe orbit | Horseshoe orbit |
| 2013 LX28 | 0.452 | 130–300 | Pan-STARRS | 2013-06-12 | Quasi-satellite temporary | Quasi-satellite temporary |
| 2014 OL339 | 0.461 | 70–160 | EURONEAR | 2014-07-29 | Quasi-satellite temporary | Quasi-satellite temporary |
| 2015 SO2 | 0.108 | 50–110 | Črni Vrh Observatory | 2015-09-21 | Quasi-satellite | Horseshoe orbit temporary |
| 2015 XX169 | 0.184 | 9–22 | Mount Lemmon Survey | 2015-12-09 | Horseshoe orbit temporary | Horseshoe orbit temporary |
| 2015 YA | 0.279 | 9–22 | Catalina Sky Survey | 2015-12-16 | Horseshoe orbit temporary | Horseshoe orbit temporary |
| 2015 YQ1 | 0.404 | 7–16 | Mount Lemmon Survey | 2015-12-19 | Horseshoe orbit temporary | Horseshoe orbit temporary |
| 469219 Kamoʻoalewa | 0.104 | 40-100 | Pan-STARRS | 2016-04-27 | Quasi-satellite stable | Quasi-satellite stable |
| DN16082203 | ? | ? | ? | 2016-08-22 | Possible Temporary satellite | Destroyed |
| 2020 CD3 | 0.017 | 1–6 | Mount Lemmon Survey | 2020-02-15 | Temporary satellite | Apollo asteroid |
| 2020 PN1 | 0.127 | 10–50 | ATLAS-HKO | 2020-08-12 | Horseshoe orbit temporary | Horseshoe orbit temporary |
| 2020 PP1 | 0.074 | 10–20 | Pan-STARRS | 2020-08-12 | Quasi-satellite stable | Quasi-satellite stable |
| (614689) 2020 XL5 | 0.387 | 1100-1260 | Pan-STARRS | 2020-12-12 | Earth trojan | Earth trojan |
| 2022 NX1 | 0.025 | 5-15 | Moonbase South Observatory | 2020-07-02 | Temporary satellite | Apollo asteroid |
| 2023 FW13 | 0.177 | 10-20 | Pan-STARRS | 2023-03-28 | Quasi-satellite | Quasi-satellite |
| 2024 PT5 | 0.021 | 7–13 | ATLAS South Africa, Sutherland | 2024-08-07 | Temporary satellite | Temporary satellite |

### Ceres

The dwarf-planet asteroid 1 Ceres is believed to have a quasi-satellite, the as-yet-unnamed (76146) 2000 EU16.

### Neptune

(309239) 2007 RW10 is a temporary quasi-satellite of Neptune. The object has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years.

### Other planets

Based on simulations, it is believed that Uranus and Neptune could potentially hold quasi-satellites for up to the age of the Solar System (about 4.5 billion years), but a quasi-satellite's orbit would remain stable for only 10 million years near Jupiter and 100,000 years near Saturn. Jupiter and Saturn are known to have quasi-satellites. 2015 OL106, a co-orbital to Jupiter, intermittently becomes a quasi satellite of the planet, and will next become one between 2380 and 2480.

### Artificial quasi-satellites

In early 1989, the Soviet Phobos 2 spacecraft was injected into a quasi-satellite orbit around the Martian moon Phobos, with a mean orbital radius of about 100 kilometres (62 mi) from Phobos. According to computations, it could have then stayed trapped in the vicinity of Phobos for many months. The spacecraft was lost due to a malfunction of the on-board control system.
In 2005, aerospace engineer Thomas Gangale proposed a quasi-satellite orbit for spacecraft to provide communications relays between Earth and crews on Mars when Mars is in solar conjunction and direct communication is blocked by the Sun for several weeks.

### Accidental quasi-satellites

Some objects are known to be accidental quasi-satellites, which means that they are not forced into the configuration by the gravitational influence of the body of which they are quasi-satellites. The dwarf planets Ceres and Pluto are known to have accidental quasi-satellites. In the case of Pluto, the known accidental quasi-satellite, 15810 Arawn, is, like Pluto, a plutino, and is forced into this configuration by the gravitational influence of Neptune. This dynamical behavior is recurrent where Arawn becomes a quasi-satellite of Pluto every 2.4 Myr and remains in that configuration for nearly 350,000 years.