Close to a million asteroids have been discovered to date, almost all of them outside the orbit of the Earth. Of the tiny majority that break this rule, the vast majority are Apollo Asteroids, which have Earth-orbit crossing orbits, but spend most of their time outside the orbit of the Earth. Much rarer are the Aten Asteroids, which have Earth-orbit crossing orbits, but are closer to the Sun than the Earth is for the majority of the time. Rarer still, are the Atira Asteroids, which orbit entirely inside of the orbit of the Earth. Theoretically, a small subset of these asteroids will orbit entirely inside the orbit of Venus, although to date no such asteroid has been discovered.
In a paper published on the online arXiv database at Cornell University and accepted for publication in the Monthly Notices of the Royal Astronomical Society, Bryce Bolin of the Division of Physics, Mathematics and Astronomy and Infrared Processing and Analysis Center at the California Institute of Technology, Tomas Ahumada of the Department of Astronomy at the University of Maryland, Pieter van Dokkum of the Department of Astronomy at Yale University, Christoffer Fremling, also of the Division of Physics, Mathematics and Astronomy at the California Institute of Technology, Mikael Granvik of the Department of Physics at the University of Helsinki and the Asteroid Engineering Lab at the Luleå University of Technology, Kevin Hardegree-Ullman of the Steward Observatory of the University of Arizona, Yuichi Harikane of the Institute for Cosmic Ray Research at the University of Tokyo and the National Astronomical Observatory of Japan, Josiah Purdum of the Caltech Optical Observatories of the California Institute of Technology, Eugene Serabyn, of the Jet Propulsion Laboratory at the California Institute of Technology, John Southworth of the Astrophysical Research Institute at Liverpool John Moores University, and Chengxing Zhai, also of the Jet Propulsion Laboratory at the California Institute of Technology, describe the discovery of the first known asteroid orbiting entirely within the orbit of Venus.
The object was discovered by the Zwicky Transient Facility at the Palomar Observatory, which used the Samuel Oschin Schmidt Telescope to detect transients (short lived phenomena) in the Northern Hemisphere sky. Specifically, a portion of the Zwicky Transient Facility's activities, the Twilight Survey, is dedicated to looking at objects and events close to the Sun, alternating between evening and morning observing twilight on clear nights.
This survey covered approximately 40 000 square degrees of sky between September 2019 and January 2020, covering an area with a solar elongation of between 35 and 60 degrees. Objects orbiting entirely within the orbit of Venus should have solar elongations of less than 46 degrees, and calculations suggest that about 85% of such objects should have a maximum solar elongation which falls within the range covered by the Zwicky Transient Facility's Twilight Survey.
On 4 January 2020 the Zwicky Transient Facility detected an object about 40 degrees from the Sun. This object was given the designation 2020 AV2, which implies that it was the 71st asteroid (asteroid V2 - in numbering asteroids the letters A-Z, excluding I, are assigned numbers from 1 to 25, with a number added to the end each time the alphabet is ended, so that A = 1, A1 = 25, A2 = 49, etc., which means that V2 = (25 x 2) + 21 = 71) discovered in the first half of January 2020 (period 2020 A; the year being split into 24 half-months represented by the letters A-Y, with I being excluded).
Following this initial discovery follow-up observations were made with the Kitt Peak Electron Multiplying Charge Coupled Device Demonstrator on 9 January 2020, and the Southern Astrophysical Research Telescope and Magellan Telescope on 17-19 July 2020. These observations enabled the calculation of the orbit of 2020 AV2, establishing that it has an aphelion distance (the point on its orbit which is furthest from the Sun) of 0.65 AU (65% of the distance at which the Earth orbit's the Sun). This places the orbit of 2020 AV2 entirely inside the orbit of Venus, which has a perihelion distance (point on its orbit closest to the Sun) of 0.71 AU.
This conformation led to the International Astronomical Union's Minor Planet Centre giving the asteroid the designation (594913), indicating that it is the 594 913rd confirmed asteroid. This conformation gives its discoverers the right to name the asteroid (a right which is not always exercised, given the very large number of asteroids discovered, and the fact that the majority of these are discovered by automated surveys), with the International Astronomical Union's Working Group on Small Body Nomenclature accepting the name 'Ayló'chaxnim, which means 'Venus girl' in the Luiseño language indigenous to southern California, on 8 November 2021. Bolin et al. further propose that the term 'Ayló'chaxnim be used as a generic name for all asteroids orbiting inside the orbit of Venus.
Bolin et al. calculate that (594913) 2020 AV2 'Ayló'chaxnim will enter a 3:2 orbital resonance with Venus (orbit locked to that of Venus on which it will orbit three times for every two orbits of Venus) in approximately 60 000 years time, and that 10 000 years later repeated close encounters with Mercury will have caused it to have lost much of the variation in its orbital path. This resonant orbit will protect the asteroid from close encounters with Venus, in the same way that the resonant orbit between Pluto and Neptune protects Pluto from close encounters with Neptune. (594913) 2020 AV2 'Ayló'chaxnim should remain locked into this orbital resonance for 10 000 years, then move in and out of it for another 100 000 years.
Bolin et al. further estimate that (594913) 2020 AV2 'Ayló'chaxnim has migrated to within the orbit of Venus within the past million years, and is likely to remain within this area for about 2 million years from now; earlier calculations of this residence time were shorter, however Bolin et al.'s is based on more data, and therefore presumably more accurate.
The currently available data prevents the accurate calculation of the evolution of (594913) 2020 AV2 'Ayló'chaxnim's orbit into the tens of millions of years scale. However, a model developed by Bolin et al. suggests that (594913) 2020 AV2 'Ayló'chaxnim has a 50% chance of colliding with the Sun or a planet within the next 10 million years, and a 90% chance of undergoing such a collision in the next 90 million years. The model also suggests that (594913) 2020 AV2 'Ayló'chaxnim has a 13% chance of eventually colliding with the Sun, a 52% chance of eventually colliding with Venus, a 16% chance of colliding with the Earth, a 13% chance of colliding with Mercury, and a 2% chance of colliding with Mars, leaving the asteroid with a 4% chance of either surviving on approximately its current orbit for more than 50 million years (the limit of the simulation) or being ejected from the Solar System.
Spectroscopic data on (594913) 2020 AV2 'Ayló'chaxnim collected by the Keck telescope suggests that it has a reddish surface, probably indicative of a silicate S-type asteroid-like composition. Such asteroids are most abundant in the Main Asteroid Belt, the probable point of origin of (594913) 2020 AV2 'Ayló'chaxnim; Bolin et al. calculate an approximately 77% chance that the asteroid originated in the inner Main Asteroid Belt, an 18% chance that it derives from the Hungaria Asteroid Group, which orbit just inside the Main Asteroid Belt, and a 4% chance that it derives from a group of asteroids within the Main Asteroid Belt which have a 3:1 orbital resonance with Jupiter.
Based upon the albedo of (594913) 2020 AV2 'Ayló'chaxnim (i.e. the amount of light it reflects), Bolin et al. calculate that it has a diameter of about 1.6 km.
There are estimated to be about 1000 Near Earth Asteroids with diameters in excess of 1 km, although only about 0.3% of these (i.e. three km-scale asteroids) are estimated to remain permanently inside the orbit of Venus. Thus (594913) 2020 AV2 'Ayló'chaxnim appears to be a significant (if predicted) discovery of an unusual Solar System body. However, this region of the Solar System is relatively underexplored, leaving us with no independent test of the models of this area at this time.
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