View source for 2002 AA29

{{Short description|Near-Earth asteroid}}
{{DISPLAYTITLE:{{mp|2002 AA|29}}}}
{{Infobox planet
| minorplanet=yes
| background=#FFC2E0
| name={{mp|2002 AA|29}}
| image= 2002AA29.gif
| image_scale =
| discovery_ref=<ref name="MPEC2002-A92"/>
| discoverer=[[LINEAR]]
| discovered=January 9, 2002
| alt_names=''none''
| mp_category=[[Aten asteroid]]
| orbit_ref=<ref name="jpldata"/>
| epoch=13 January 2016 ([[Julian day|JD]] 2457400.5)
| semimajor={{Convert|0.99259|AU|Gm|abbr=on}}
| perihelion={{Convert|0.97963|AU|Gm|abbr=on}}
| aphelion={{Convert|1.0055|AU|Gm|abbr=on|lk=on}}
| eccentricity=0.013047
| period=0.99 [[Julian year (astronomy)|yr]] (361.2 [[Julian year (astronomy)|d]])
| inclination=10.748°
| asc_node=106.38°
| arg_peri=101.75°
| mean_anomaly=310.32[[Degree (angle)|°]]
| avg_speed=29.784 km/[[second|s]]
| dimensions=~0.06 km<br /><100 metres<ref name=Connors2002/><br />25±5 metres<ref name="Icarus2"/>
| mass=~2.3×10<sup>8</sup> kg
| density=2 ? g/cm<sup>3</sup>
| surface_grav=~0.000 017 m/s<sup>2</sup>
| escape_velocity=~0.000 032 km/s
| rotation={{Convert|0.55|h|min|abbr=on|lk=on}}<ref name="jpldata"/>
| spectral_type=[[S-type asteroid]]<ref name="Icarus2"/>
| abs_magnitude=24.1
| albedo=0.2 ?
| single_temperature=~279 [[kelvin|K]]
| mean_motion={{Deg2DMS|0.99667|sup=ms}} /day
| observation_arc=736 days (2.02 yr)
| uncertainty=0
| moid={{Convert|0.0116565|AU|Gm|abbr=on}}
| jupiter_moid={{Convert|3.96814|AU|Gm|abbr=on}}
}}
'''{{mp|2002 AA|29}}''' ([[Astronomical naming conventions#Minor planets|also written]] '''2002 AA29''') is a small [[near-Earth asteroid]] that was discovered on January 9, 2002 by the [[Lincoln Near-Earth Asteroid Research|LINEAR]] ''(Lincoln Near Earth Asteroid Research)'' automatic sky survey. The diameter of the [[asteroid]] is only about {{convert|20|-|100|m|ft|sigfig=1}}. It revolves about the [[Sun]] on an almost circular orbit very similar to that of the [[Earth]]. This lies for the most part inside the Earth's orbit, which it crosses near the asteroid's furthest point from the Sun, the [[aphelion]]. Because of this orbit, the asteroid is classified as [[Aten asteroid|Aten type]],<ref name=jpldata/> named after the asteroid [[2062 Aten]].

A further characteristic is that its mean [[orbital period]] about the Sun is exactly one [[sidereal year]]. This means that it is locked into a relationship with the Earth, since such an orbit is only stable under particular conditions. As yet only a few asteroids of this sort are known, locked into a 1:1 [[Orbital resonance|resonance]] with the Earth. The first was [[3753 Cruithne]], discovered in 1986.

Asteroids that have a 1:1 orbital resonance with a planet are also called [[Co-orbital configuration|co-orbital objects]], because they follow the orbit of the planet. The most numerous known co-orbital asteroids are the so-called [[Trojan (astronomy)|trojans]], which occupy the L4 and L5 [[Lagrangian points]] of the relevant planet. However, {{mp|2002 AA|29}} does not belong to these. Instead, it follows a so-called [[horseshoe orbit]] along the path of the Earth.

== Orbit ==
=== Orbital data ===
Shortly after the discovery by LINEAR, Scientists at the [[Jet Propulsion Laboratory]] (JPL), the [[Athabasca University]] ([[Canada]]), the [[Queen's University at Kingston|Queen's University]] in [[Kingston, Ontario|Kingston (Ontario, Canada)]], the [[York University]] in [[Toronto]] and the [[Tuorla Observatory]] of the [[University of Turku]] in [[Finland]] determined the unusual orbit of {{mp|2002 AA|29}}, and through further observations at the [[Canada–France–Hawaii Telescope]] in Hawaii it was confirmed that:

[[image:2002aa29-orbit-3.png|thumb|Orbits of {{mp|2002 AA|29}} and Earth about the Sun, looking down on the ecliptic plane from above the Sun's North Pole; Image: [[Jet Propulsion Laboratory|JPL]]]]
* Its orbit lies for the most part inside Earth's orbit. The orbits of most asteroids lie in the [[asteroid belt]] between [[Mars]] and [[Jupiter]]. Through orbital disturbances by the gas giant planets, mainly Jupiter and the [[Kirkwood gap]]s, and through the [[Yarkovsky effect]] (force due to asymmetrical absorption and emission of infrared radiation) asteroids are diverted into the inner [[Solar System]], where their orbits are further influenced by close approaches with the inner planets. {{mp|2002 AA|29}} has probably been brought in the same way from the outer Solar System into Earth's influence. However, it is also suggested that the asteroid has always been on a near-Earth orbit and thus that it or a precursor body was formed near Earth's orbit. In this case one possibility is that it could be a fragment from a collision of a middle-sized asteroid with Earth or the [[Moon]].<ref name="lpsc2004">M. Connors, C. Veillet, R. Brasser, P. Wiegert, P. W. Chodas, S. Mikkola, K. Innanen: ''[http://www.lpi.usra.edu/meetings/lpsc2004/pdf/1565.pdf Horseshoe Asteroids and Quasi-satellites in Earth-like Orbits.]'' in: ''35th Lunar and Planetary Science Conference, 15.–19. März 2004.'' League City Texas 2004, 3., Abstract Nr. 1565 (PDF).</ref>
* Its mean orbital period is one [[sidereal year]]. After it was diverted into the inner Solar System – or formed on a path near Earth's orbit – the asteroid must have been moved into an orbit corresponding with Earth. In this orbit it was repeatedly pulled by Earth in such a way that its own orbital period became the same as that of Earth. In the current orbit, Earth thus holds the asteroid in synchronicity with its own orbit.

[[image:2002aa29-orbit-2.png|thumb|Orbits of {{mp|2002 AA|29}} and Earth about the Sun, seen from the side; Image: [[Jet Propulsion Laboratory|JPL]]]]
* The orbit of the asteroid is almost circular, with an [[orbital eccentricity|eccentricity]] of 0.012 which is even lower than that of the Earth at 0.0167. The other near-Earth asteroids have on average a significantly higher eccentricity of 0.29. Also, all other asteroids in 1:1 resonance with Earth known before 2002 have very strongly elliptical orbits – e.g. the eccentricity of (3753) Cruithne is 0.515. At the time of its discovery the orbit of {{mp|2002 AA|29}} was unique, because of which the asteroid is often called the first true co-orbital companion of Earth, since the paths of previously discovered asteroids are not very similar to Earth's orbit. The very low orbital eccentricity of {{mp|2002 AA|29}} is also an indication that it must always have been on a near-Earth orbit, or the Yarkovsky effect must have comparatively strongly caused it to spiral into the inner Solar System over billions of years, since as a rule asteroids which have been steered by planets have orbits with higher eccentricity.
* The orbital inclination with respect to the [[ecliptic]] (orbital plane of Earth) of {{mp|2002 AA|29}} is a moderate 10.739°. Hence its orbit is slightly tilted compared with that of Earth.

=== Shape of the orbit ===
[[Image:2002aa29-orbit.png|thumb|[[Horseshoe orbit]] of 2002 AA29. The graphic shows a full revolution of 95 years. The position of {{mp|2002 AA|29}} along the orbit is that of year 2003 (last nearest approach to Earth). Image: [[Jet Propulsion Laboratory|JPL]]]]
If one looks at the orbit of {{mp|2002 AA|29}} from a point moving with the Earth around the Sun (the [[Frame of reference|reference frame]] of the Earth–Sun system), it describes over the course of 95 years an arc of almost 360°, which during the next 95 years it retraces in reverse. The shape of this arc is reminiscent of a horseshoe, from which comes the name "[[horseshoe orbit]]". As it moves along the Earth's orbit, it winds in a spiral about it, in which each loop of the spiral takes one year. This spiral motion (in the Earth–Sun reference frame) arises from the slightly lower eccentricity and the tilt of the orbit: the inclination relative to the Earth's orbit is responsible for the vertical component of the spiral loop, and the difference in eccentricity for the horizontal component.

When {{mp|2002 AA|29}} is approaching the Earth from in front (i.e. it is moving slightly slower, and the Earth is catching it up), the gravitational attraction of the Earth shifts it onto a slightly faster orbit, a little nearer the Sun. It now hurries ahead of the Earth along its new orbit, until after 95 years it has almost lapped the Earth and is coming up from behind. Again it comes under the Earth's gravitational influence; this time it is lifted onto a slower orbit, further from the Sun. On this orbit it can no longer keep pace with the Earth, and it falls behind until in 95 years it is once again approaching the Earth from in front. The Earth and {{mp|2002 AA|29}} chase each other in turn around the Sun, but do not get close enough to break the pattern.

On 8 January 2003, the asteroid approached the Earth from in front to a distance of {{convert|0.0391|AU|km mi|abbr=on|lk=on}},<ref name=jpl-close/> its closest approach for nearly a century. Since that date, it has been hurrying ahead (with a [[semi-major axis]] less than 1 AU), and will continue to do so until it has reached its closest approach from behind on 11 July 2097 at a distance of {{convert|0.037712|AU|km mi|abbr=on|lk=off}}.<ref name=jpl-close/> As a result of this subtle exchange with the Earth, unlike other Earth orbit crossing asteroids, we need have no fear that it could ever collide with the Earth. Calculations indicate that in the next few thousand years it will never come closer than 4.5 million kilometres, or about twelve times the distance from the Earth to the Moon.<ref name=Connors2002/>

[[Image:2002aa29-orbit-4.png|thumb|[[Quasi-satellite]] orbit of {{mp|2002 AA|29}} in the year 2589, looking vertically down on the ecliptic. Left, orbits of Asteroid and Earth in the reference frame of the [[fixed stars]]; right, in the reference frame of the Earth–Sun system. Image: [[Jet Propulsion Laboratory|JPL]]]]
Because of its orbital inclination of 10.739° to the ecliptic, {{mp|2002 AA|29}} is not always forced by the Earth on its horseshoe orbit however but can sometimes slip out of this pattern. It is then caught for a while in the neighbourhood of the Earth. This will next happen in about 600 years i.e. in the 26th century. It will then stay within the small gap in the Earth's orbit which it does not reach in its previous horseshoe orbit, and will be no further than 0.2 [[astronomical unit]]s (30 million km) away from the Earth. There it will slowly circle the Earth almost like a second moon, although it takes one year for a circuit. After 45 years it finally switches back into the horseshoe orbit, until it again stays near the Earth for 45 years around the year 3750 and again in 6400. In these phases in which it stays outside its horseshoe orbit it oscillates in the narrow region along the Earth's orbit where it is caught, moving back and forth in 15 years. Because it is not bound to the Earth like the Moon but is mainly under the gravitational influence of the Sun, it belongs to the bodies called [[quasi-satellite]]s. This is somewhat analogous to two [[Automobile|cars]] travelling side by side at the same speed and repeatedly overtaking one another but which are however not attached to each other. Orbital calculations show that {{mp|2002 AA|29}} was in this quasi-satellite orbit for 45 years from about 520 AD but because of its tiny size was too dim to have been seen. It switches approximately cyclically between the two orbital forms, but always stays for 45 years in the quasi-satellite orbit. Outside the time frame from about 520-6500 AD, the calculated orbits become [[chaos theory|chaotic]] i.e. not predictable, and thus for periods outside this time frame no exact statements can be made.<ref name="Icarus1">R. Brasser, K. A. Innanen, M. Connors, C. Veillet, P. Wiegert, Seppo Mikkola, P. W. Chodas: ''Transient co-orbital asteroids.'' in: ''[[Icarus (journal)|Icarus]].'' Elsevier, San Diego 171.2004, 9, p102–109. {{ISSN|0019-1035}} (online on the Icarus Server: {{doi|10.1016/j.icarus.2004.04.019}})</ref> {{mp|2002 AA|29}} was the first known [[heavenly body]] that switches between horseshoe and quasi-satellite orbits.
{{multiple image | align = left | direction = horizontal | width = 300
| header = Animation of 2002 AA29 orbit from 1900 to 2140
| image1 = Animation of 2002 AA29 orbit.gif
| caption1 = Relative to Sun and Earth
| image2 = Animation of 2002 AA29 orbit around Earth.gif 
| caption2 = Around Earth
| image3 = Animation of 2002 AA29 orbit around Sun.gif 
| caption3 = Around Sun
| footer ={{legend2| Yellow| Sun}}{{·}}{{legend2| RoyalBlue| Earth}}{{·}}{{legend2|Magenta| 2002 AA29}}
}}
{{clear}}

== Physical nature ==
=== Brightness and size ===
Relatively little is known about {{mp|2002 AA|29}} itself. With a size of about {{convert|20|-|100|m|ft|sigfig=1}} it is very small, on account of which it is seen from the Earth as a small point even with large [[telescope]]s, and can only be observed using highly sensitive [[Charge-coupled device|CCD]] cameras. At the time of its closest approach in January 2003 it had an [[apparent magnitude]] of about 20.4.<ref name="MPEC2003-A17"/>

So far nothing concrete is known about the composition of {{mp|2002 AA|29}}. Because of its nearness to the Sun, it cannot however consist of [[Volatile (astrogeology)|volatile substances]] such as [[ice|water ice]], since these would [[evaporation|evaporate]] or [[Sublimation (chemistry)|sublime]]; one can clearly observe this happening to a [[comet]] as this forms the visible tail. Presumably it will have a dark, [[carbon]]-bearing or somewhat lighter [[silicate minerals|silicate]]-rich surface; in the former case the [[albedo]] would be around 0.05, in the latter somewhat higher at 0.15 to 0.25. It is due to this uncertainty that the figures for its diameter cover such a wide range.

A further uncertainty arises from [[radar astronomy|radar]] echo measurements at the [[Arecibo Observatory|Arecibo]] [[Radio Telescope]], which could only pick up an unexpectedly weak radar echo, implying that {{mp|2002 AA|29}} is either smaller than estimated or reflects radio waves only weakly. In the former case it would have to have an unusually high albedo.<ref name="Icarus2">Steven J. Ostro, Jon D. Giorgini, Lance A. M. Benner, Alice A. Hine, Michael C. Nolan, Jean-Luc Margot, Paul W. Chodas, Christian Veillet: [http://echo.jpl.nasa.gov/asteroids/ostro+2003_aa29_icarus.pdf ''Radar detection of Asteroid 2002 AA29''] in: ''[[Icarus (journal)|Icarus]].'' Elsevier, San Diego 166.2003, 12, p271–275. {{ISSN|0019-1035}} (online on the Icarus Server: {{doi|10.1016/j.icarus.2003.09.001}})</ref> This would be evidence in support of the speculation that it, or at least the material of which it is composed, is different from most other asteroids so far discovered on near-Earth orbits, or represents a fragment thrown off by the collision of a medium-sized asteroid with the Earth or the Moon.<ref name="lpsc2004" />

=== Rotational period ===
Using radar echo measurements at the Arecibo radio telescope the rotational period of {{mp|2002 AA|29}} could be determined. In this radar astronomy procedure [[radio waves]] of known [[wavelength]] are emitted from a radio telescope aimed at an asteroid. There they are reflected, and because of the [[Doppler effect]] the part of the surface that is moving towards the observer (because of the asteroid's rotation) shortens the wavelength of the reflected waves, whilst the other part which is turning away from the observer lengthens the reflected wavelength. As a result, the wavelength of the reflected waves is "smeared out". The extent of the wavelength smearing and the diameter of the asteroid allow the rotational period to be narrowed down. 33 minutes is thus calculated as the upper limit of the rotational period for {{mp|2002 AA|29}}; it probably rotates more quickly. This rapid rotation together with the small diameter and therefore low mass leads to some interesting conclusions:

* The asteroid rotates so quickly that the [[centrifugal force]] on its surface exceeds its gravitational pull. It is therefore under [[tension (physics)|tension]] and so cannot be composed of an agglomeration of loosely bound debris or of fragments circling each other – as is supposed for several other asteroids and for example has been determined for the asteroid [[69230 Hermes|(69230) Hermes]]. Instead the body must be made of a single relatively strong block of rock or of pieces baked together. However, its tensile strength is probably considerably lower than terrestrial [[rock (geology)|rock]] and the asteroid also very [[porous]].<ref name="Icarus2"/>
* {{mp|2002 AA|29}} cannot possibly have been built up from individual small pieces, as these would be thrown apart by the rapid rotation. Therefore, it must be a fragment blown off in the collision of two heavenly bodies. [[J. Richard Gott]] and [[Edward Belbruno]] from [[Princeton University]] have speculated that {{mp|2002 AA|29}} might have formed together with Earth and [[Theia (planet)|Theia]], the postulated planet that, according to the [[giant impact hypothesis]], collided with Earth in its early history.<ref name="NewScientist20040814"/>

== Outlook ==
Because its orbit is very similar to the Earth's, the asteroid is relatively easily reachable by [[space probes]]. {{mp|2002 AA|29}} would therefore be a suitable object of study for more precise research into the structure and formation of asteroids and the evolution of their orbits around the Sun. Meanwhile, further co-orbital companions of the Earth of this type on horseshoe orbits or on orbits as quasi-satellites have already been found, such as the quasi-satellite {{mpl|2003 YN|107}}. Furthermore, it is assumed that there are small trojan companions of the Earth with diameters in the region of 100 metres located at the L4 and L5 Lagrangian points of the Earth–Sun system.

==Related objects==
*[[6Q0B44E]]
*{{mpl|2006 RH|120}}
*{{mpl|2003 YN|107}} – quasi-satellite of Earth
*{{mpl|2010 TK|7}} – Trojan co-orbital companion of Earth
* [[3753 Cruithne]] (1986 TO)
* {{mpl|2001 GO|2}}
* {{mpl|2006 JY|26}}
* {{mpl|2010 SO|16}}
* {{mpl|2012 FC|71}}

==See also==
* [[Natural satellite]]
* [[Quasi-satellite]]
* [[List of asteroids]]
* [[Astronomical naming conventions#Minor planets|Naming of Asteroids]]
*[[Orbital resonance]]

==References==
<references>

<ref name="MPEC2002-A92">{{cite web
  |title=MPEC 2002-A92 : 2002 AA29
  |publisher=[[IAU Minor Planet Center]]
  |date=2002-01-15
  |url=http://www.minorplanetcenter.org/mpec/K02/K02A92.html}} (K02A29A)</ref>

<ref name=jpldata>{{cite web
  |type=last observation: 2004-01-15; [[Observation arc|arc]]: 2.02 yr
  |title=JPL Small-Body Database Browser: (2002 AA29)
  |url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2002AA29
  |publisher=Jet Propulsion Laboratory
  |accessdate=30 March 2016}}</ref>

<ref name=jpl-close>{{cite web
  |type=last observation: 2004-01-15; [[Observation arc|arc]]: 2.02 yr
  |title=JPL Close-Approach Data: (2002 AA29)
  |url=http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2002AA29;cad=1#cad
  |accessdate=2015-02-28}}</ref>

<ref name=Connors2002>{{cite journal
  |last1=Connors |first1=Colin
  |last2=Chodas |first2=Paul.
  |last3=Mikkola |first3=Seppo
  |last4=Wiegert |first4=Paul
  |title=Discovery of an asteroid and quasi-satellite in an Earth-like horseshoe orbit
  |journal=[[Meteoritics & Planetary Science]]
  |volume=37 |issue=10 |pages=1435–1441 |date=2002
  |doi=10.1111/j.1945-5100.2002.tb01039.x
  |bibcode=2002M&PS...37.1435C|doi-access=free}}</ref>

<ref name="MPEC2003-A17">{{cite web
  |title=MPEC 2003-A17 : 2002 AA29
  |publisher=IAU Minor Planet Center
  |date=2003-01-04
  |url=http://www.minorplanetcenter.net/mpec/K03/K03A17.html}}</ref>

<ref name="NewScientist20040814">{{cite web
  |title=The planet that stalked the Earth
  |publisher=[[New Scientist]]
  |author=Marcus Chown
  |date=2004-08-14
  |url=https://www.newscientist.com/article/mg18324605.200-the-planet-that-stalked-the-earth.html}} [https://www.newscientist.com/data/images/archive/2460/24605201.jpg JPG]</ref>

</references>

*Tilmann Althaus: ''Ein zweiter Begleiter des Blauen Planeten.'' in: ''[[Sterne und Weltraum]].'' Spektrum der Wiss., Heidelberg 42.2003, 2, S. 22–24. {{ISSN|0039-1263}}

== External links ==
{{Commons}}

=== Articles ===
* [http://cfa-www.harvard.edu/mpec/K03/K03A17.html MPEC 2003-A17]
* [http://www.astro.uwo.ca/~wiegert/AA29/AA29.html Earth coorbital asteroid {{mp|2002 AA|29}}]
* [http://www.scielo.br/pdf/cam/v24n1/06v24n1.pdf Research paper describing horseshoe orbits.] Recommend starting at page 105!

=== Databases ===
* [http://cfa-www.harvard.edu/mpec/K03/K03A17.html Orbital data for {{mp|2002 AA|29}} from the MPEC database]
* [https://web.archive.org/web/20141207143224/http://earn.dlr.de/nea/K02A29A.htm Physical data for {{mp|2002 AA|29}} from the EARN Database]
* [http://ftp.lowell.edu/pub/elgb/astorb.html Asteroid Orbital Elements Database] of the [[Lowell Observatory]]
* {{JPL small body}}

<!--use upon numbering: {{Minor planets navigator | |number=? |PageName={{mp|(?) 2002 AA|29}} | }} -->
{{Small Solar System bodies}}
{{Authority control}}

{{DEFAULTSORT:2002 AA29}}
[[Category:Aten asteroids|#]]
[[Category:Minor planet object articles (unnumbered)]]
[[Category:Earth co-orbital asteroids|#]]
[[Category:Earth-crossing asteroids]]
[[Category:Astronomical objects discovered in 2002|20020109]]
[[Category:Horseshoe orbit]]