# Earth trojan

An Earth trojan is an asteroid that orbits the Sun in the vicinity of the Earth–Sun Lagrange points L$_4$ (leading 60°) or L$_5$ (trailing 60°), thus having an orbit similar to Earth's. Only two Earth trojans have so far been discovered. The name "trojan" was first used in 1906 for the Jupiter trojans, the asteroids that were observed near the Lagrangian points of Jupiter's orbit.

## Members
### L$_4$ (leading)

* (706765) 2010 TK7: A 300-metre diameter asteroid, discovered using the Wide-field Infrared Survey Explorer (WISE) satellite in January 2010.
* (614689) 2020 XL5: Discovered by the Pan-STARRS survey in December 2020 and later recognised as an Earth trojan in January 2021. It is 1.2 km in diameter.

### L$_5$ (trailing)

* No known objects are currently thought to be L$_5$ trojans of Earth.

## Searches

An Earth-based search for L$_5$ objects was conducted in 1994, covering 0.35 square degrees of sky, under poor observing conditions. That search failed to detect any objects:
    "The limiting sensitivity of this search was magnitude ~22.8, corresponding to C-type asteroids ~350 m in diameter, or S-type asteroids ~175 m in diameter."
In February 2017, the OSIRIS-REx spacecraft performed a search from within the L$_4$ region on its way to asteroid Bennu. No additional Earth trojans were discovered.
In April 2017, the Hayabusa2 spacecraft searched the L$_5$ region while proceeding to asteroid Ryugu, but did not find any asteroids there.

## Giant-impact hypothesis

A hypothetical planet-sized Earth trojan the size of Mars, given the name Theia, is thought by proponents of the giant-impact hypothesis to be the origin of the Moon. The hypothesis states that the Moon formed after Earth and Theia collided, showering material from the two planets into space. This material eventually accreted around Earth and into a single orbiting body, the Moon.
At the same time, material from Theia mixed and combined with Earth's mantle and core. Supporters of the giant-impact hypothesis theorise that Earth's large core in relation to its overall volume is as a result of this combination.

## Continuing interest in near-Earth asteroids

Astronomy continues to retain interest in the subject. A publication describes these reasons thus:
   The survival to the present day of an ancient [Earth Trojan] population is reasonably assured provided Earth's orbit itself was not strongly perturbed since its formation. It is therefore pertinent to consider that modern theoretical models of planet formation find strongly chaotic orbital evolution during the final stages of assembly of the terrestrial planets and the Earth–Moon system.
   Such chaotic evolution may at first sight appear unfavorable to the survival of a primordial population of [Earth trojans]. However, during and after the chaotic assembly of the terrestrial planets, it is likely that a residual planetesimal population, of a few percent of Earth's mass, was present and helped to damp the orbital eccentricities and inclinations of the terrestrial planets to their observed low values, as well as to provide the so-called "late veneer" of accreting planetesimals to account for the abundance patterns of the highly siderophile elements in Earth's mantle.
   Such a residual planetesimal population would also naturally lead to a small fraction trapped in the Earth's Trojan zones as Earth's orbit circularized. In addition to potentially hosting an ancient, long-term stable population of asteroids, Earth's Trojan regions also provide transient traps for NEOs that originate from more distal reservoirs of small bodies in the solar system like the main asteroid belt.

## Other companions of Earth

Several other small objects have been found on an orbital path associated with Earth. Although these objects are in 1:1 orbital resonance, they are not Earth trojans, because they do not librate around a definite Sun–Earth Lagrangian point, neither L$_4$ nor L$_5$.
Earth has another noted companion, asteroid 3753 Cruithne. About 5 km across, it has a peculiar type of orbital resonance called an overlapping horseshoe, and is probably only a temporary liaison.
469219 Kamoʻoalewa, an asteroid discovered on 27 April 2016, is possibly the most stable quasi-satellite of 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 |

## Gallery

* Illustration of Trojan Asteroid 2020 XL5