Jump to content

Mars trojan: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
Updated reference
(29 intermediate revisions by 21 users not shown)
Line 1: Line 1:
[[Image:Minor Planets - Martian L5.svg|thumb|right|300px|The {{L5}} group (shown in green) and the {{L4}} group (light blue) of Mars trojans on the orbit of [[Mars]]. Mars is shown in red. The outer orbit is that of Jupiter.]]
{{Short description|Celestial bodies that share the orbit of Mars}}[[Image:Minor Planets - Martian L5.svg|thumb|right|300px|The {{L5}} group (shown in green) and the {{L4}} group (light blue) of [[Mars]] and [[Jupiter]] [[Trojan (celestial body)|trojan asteroids]] shown along with the orbits of Jupiter and the inner planets. Mars is shown in red. The outer orbit is that of Jupiter.]]
[[File:Animation of 1999 UJ7 relative to Sun and Mars 1600-2500.gif|thumb|Animation of 1999 UJ7 relative to Sun and Mars 1600-2500<br>{{legend2| Yellow | Sun}}{{·}}{{legend2| magenta |1999 UJ7}}{{·}}{{legend2| lime |Mars}}]]
[[File:Animation of 2007 NS2 relative to Sun and Mars 1600-2500.gif|thumb|Animation of 2007 NS2 relative to Sun and Mars 1600-2500<br>{{legend2| Yellow | Sun}}{{·}}{{legend2| magenta |2007 NS2}}{{·}}{{legend2| lime |Mars}}]]
⚫
The '''Mars trojans''' are a group of [[Trojan (celestial body)|trojan objects]] that share the [[orbit]] of the [[planet]] [[Mars]] around the [[Sun]]. They can be found around the two [[Lagrangian point]]s 60° ahead of and behind Mars. The origin of the Mars trojans is not well understood. One theory suggests that they were primordial objects left over from the formation of Mars that were captured in its Lagrangian points as the [[Solar System]] was forming. However, spectral studies of the Mars trojans indicate this may not be the case.<ref name=MTArivkin/><ref name=MTAtrilling/> Another explanation involves asteroids chaotically wandering into the [[Mars]] Lagrangian points later in the Solar System's formation. This is also questionable considering the short dynamical lifetimes of these objects.<ref name="MTAsholl"/><ref name="MTAschwarz"/> The spectra of Eureka and two other Mars trojans indicates an [[olivine]]-rich composition.<ref name="Borisov" /> Since olivine-rich objects are rare in the asteroid belt it has been suggested that some of the Mars trojans are captured debris from a large orbit-altering impact on Mars when it encountered a planetary embryo.<ref name="Polishook" /><ref name="MTAsholl"/>


⚫
Presently, this group contains 17 asteroids confirmed to be stable Mars trojans by long-term numerical simulations but only nine of them are accepted by the [[Minor Planet Center]].<ref name=MPC/><ref name="MTAsholl"/><ref name="MTAschwarz"/><ref name="MTAmarcos"/><ref name="MTAchristou"/><ref name="MTAchristou2"/><ref name="MTAmarcos2"/>
⚫
The '''Mars trojans''' are a group of [[Trojan (astronomy)|objects]] that share the [[orbit]] of the [[planet]] Mars around the [[Sun]]. They can be found around the two [[Lagrangian point]]s 60° ahead of and behind Mars. The origin of the Mars trojans is not well understood. One theory suggests that they were primordial objects leftover from the formation of Mars that were captured in its Lagrangian points as the [[Solar System]] was forming. However, spectral studies of the Mars trojans indicate this may not be the case.<ref name=MTArivkin/><ref name=MTAtrilling/> Another explanation involves asteroids chaotically wandering into the [[Mars]] Lagrangian points later in the Solar System's formation. This is also questionable considering the short dynamical lifetimes of these objects.<ref name="MTAsholl"/><ref name="MTAschwarz"/> The spectra of Eureka and two other Mars Trojan indicates an olivine-rich composition.<ref name="Borisov" /> Since olivine-rich objects are rare in the asteroid belt it has been suggested that some of the Mars trojans are debris from a large impact on Mars that was captured when the orbit of Mars was altered when it encountered a planetary embryo.<ref name="Polishook" /><ref name="MTAsholl"/>


⚫
Due to close orbital similarities, most of the smaller members of the L<sub>5</sub> group are hypothesized to be fragments of [[5261 Eureka|Eureka]] that were detached after it was spun up by the [[YORP effect]] (Eureka's rotational period is 2.69 h). The L<sub>4</sub> trojan [[(121514) 1999 UJ7|1999 UJ<sub>7</sub>]] has a much longer rotational period of ~50 h, apparently due to a chaotic rotation that prevents YORP spinup.<ref name="Lovett2017">{{cite journal|last1= Lovett|first1= R.|title= Sun's light touch explains asteroids flying in formation behind Mars|journal= Science|date= 2017-10-20|doi= 10.1126/science.aar2794}}</ref> The spectrum of 121514 show a certain resemblance to that of [[2023 FW14 | 2023 FW<sub>14</sub>]] and a common origin cannot be discarded.<ref name="spectrum2023FW14"/> The spectra of 121514 and 2023 FW<sub>14</sub> are very different from those of the Eureka asteroid family members.
⚫
Presently, this group contains seven asteroids confirmed to be stable Mars trojans by long-term numerical simulations but only four of them are accepted by the [[Minor Planet Center]] (†)<ref name=MPC/> and there is one candidate:<ref name="MTAsholl"/><ref name="MTAschwarz"/><ref name="MTAmarcos"/><ref name="MTAchristou"/>


{|class="wikitable sortable"
⚫
Due to close orbital similarities, most of the smaller members of the L<sub>5</sub> group are hypothesized to be fragments of [[5261 Eureka|Eureka]] that were detached after it was spun up by the [[YORP effect]] (Eureka's rotational period is 2.69 h). The L<sub>4</sub> trojan [[(121514) 1999 UJ7|1999 UJ<sub>7</sub>]] has a much longer rotational period of ~50 h, apparently due to a chaotic rotation that prevents YORP spinup.<ref name="Lovett2017">{{cite journal|last1= Lovett|first1= R.|title= Sun’s light touch explains asteroids flying in formation behind Mars|journal= Science|date= 2017-10-20|doi= 10.1126/science.aar2794}}</ref>
|+List of Mars trojans

!Designation
'''{{L4}} (''leading''):
!Cloud
* {{mpl|(121514) 1999 UJ|7}} †
!Semimajor axis<br />(AU)

!Perihelion<br />(AU)
'''{{L5}} (''trailing''):
!Eccentricity
* [[5261 Eureka]] †
!Inclination<br />(°)
* {{mpl|(101429) 1998 VF|31}} †
!([[Absolute magnitude#Solar System bodies (H)|H]])
* {{mpl|(311999) 2007 NS|2}} †
! Diameter<br />([[meter|m]])
* {{mpl|(385250) 2001 DH|47}}
|-
* {{mpl|2011 SC|191}}
|[[5261 Eureka]] || L5 || 1.52356 || 1.42477 || 0.06484 || 20.2820 || 16.13 || {{val|1880|230}}
* {{mpl|2011 UN|63}}
|-

|{{mpl|(101429) 1998 VF|31}} || L5 || 1.52429 || 1.37150 || 0.10024 || 31.2987 || 17.26 || {{val|1210|890|350}}
'''Candidates'''
|-
* {{mpl|2011 SL|25}}
|{{mpl|(121514) 1999 UJ|7}} || L4 || 1.52455 || 1.46491 || 0.03912 || 16.7493 || 17.19 || {{val|2450|490}}
|-
|{{mpl|(311999) 2007 NS|2}} || L5 || 1.52379 || 1.44155 || 0.05397 || 18.6194 || 18.18 || {{val|790|580|230}}
|-
|{{mpl|(385250) 2001 DH|47}} || L5 || 1.52385 || 1.47111 || 0.03461 || 24.4006 || 18.89 || {{val|570|420|170}}
|-
|[[2009 SE]] || L5 || 1.52451 || 1.42524 || 0.06512 || 20.6263 || 19.9 || {{val|360|260|110}}
|-
|{{mpl|2011 SL|25}} || L5 || 1.52391 || 1.34938 || 0.11453 || 21.4953 || 19.5 || {{val|430|320|120}}
|-
|{{mpl|2011 SP|189}} || L5 || 1.52386 || 1.46247 || 0.04029 || 19.8994 || 20.9 || {{val|230|160|70}}
|-
|{{mpl|2011 SC|191}} || L5 || 1.52390 || 1.45678 || 0.04405 || 18.7451 || 19.4 || {{val|450|330|130}}
|-
|{{mpl|2011 UN|63}} || L5 || 1.52378 || 1.42521 || 0.06469 || 20.3635 || 19.7 || {{val|390|290|110}}
|-
|{{mpl|2011 UB|256}} || L5 || 1.52370 || 1.41550 || 0.07101 || 24.3023 || 19.9 || {{val|360|260|110}}
|-
|{{mpl|2016 AA|165}} || L5 || 1.52299 || 1.38650 || 0.08962 || 18.7202 || 20.39 || {{val|290|210|90}}
|-
|{{mpl|2016 CP|31}} || L5 || 1.52365 || 1.43425 || 0.05867 || 23.1314 || 19.4 || {{val|450|330|130}}
|-
|{{mpl|2018 EC|4}} || L5 || 1.52365 || 1.43138 || 0.06056 || 21.8362 || 20.0 || {{val|340|250|100}}
|-
|{{mpl|2018 FC|4}} || L5 || 1.52388 || 1.49781 || 0.01711 || 22.1466 || 21.2 || {{val|200|140|60}}
|-
|{{mpl|2018 FM|29}} || L5 || 1.52391 || 1.45196 || 0.04722 || 21.5004 || 21.11 || {{val|210|150|60}}
|-
|{{mpl|2023 FW|14}} || L4 || 1.52377 || 1.28284 || 0.15811 || 13.27271 || 21.59 || {{val|318|493|199}}
|}


== See also ==
== See also ==
* [[Trojan (astronomy)]]
* [[Trojan (celestial body)]]
* Minor planets that orbit near trojan points
* Minor planets that orbit near trojan points
** [[Earth trojan]]
** [[Earth trojan]]
Line 33: Line 66:
| refs =
| refs =


<ref name="MPC">{{cite web |url=http://www.minorplanetcenter.org/iau/lists/MarsTrojans.html |title=List Of Martian Trojans |work=Minor Planet Center |accessdate = 2013-03-04}}</ref>
<ref name="MPC">{{cite web |url=https://www.minorplanetcenter.net/iau/lists/MarsTrojans.html |title=List Of Martian Trojans |work=Minor Planet Center |access-date = 2021-01-12}}</ref>

<ref name="MTAtrilling">{{cite journal |author1=Trilling, David |author2=Rivking, Andrew |author3=Stansberry, John |author4=Spahr, Timothy |author5=Crudo, Richard |author6=Davies, John | title= Albedos and diameters of three Mars Trojan asteroids | journal=Icarus | volume=192 | issue=2 | pages=442–447 | date=2007 | doi=10.1016/j.icarus.2007.08.002 | bibcode=2007Icar..192..442T |arxiv = 0709.1921 |s2cid=16618044 }}</ref>

<ref name="MTArivkin">{{cite journal |author1=Rivkin, Andrew |author2=Trilling, David |author3=Thomas, Cristina |author4=DeMeo, Fancesca |author5=Spahr, Timoth |author6=Binzel, Richard | title= Composition of the L5 Mars Trojans: Neighbors, not siblings | journal= Icarus | volume=192 | issue=2 | pages=434–441 | date=2007 | doi=10.1016/j.icarus.2007.06.026| bibcode=2007Icar..192..434R |arxiv = 0709.1925 |s2cid=15118710 }}</ref>

<ref name="MTAsholl">{{cite journal |author1=Scholl, H. |author2=Marzari, F. |author3=Tricarico, P. | title= Dynamics of Mars Trojans | journal= Icarus | volume=175 | issue=2 | pages=397–408 | date=2005 | doi=10.1016/j.icarus.2005.01.018| bibcode=2005Icar..175..397S }}</ref>


<ref name="MTAtrilling">{{cite journal |author1=Trilling, David |author2=Rivking, Andrew |author3=Stansberry, John |author4=Spahr, Timothy |author5=Crudo, Richard |author6=Davies, John | title= Albedos and diameters of three Mars Trojan asteroids | journal=Icarus | volume=192 | issue=2 | pages=442–447 | date=2007 | doi=10.1016/j.icarus.2007.08.002 | bibcode=2007Icar..192..442T |arxiv = 0709.1921 }}</ref>
<ref name="MTAschwarz">{{cite journal |author1=Schwarz, R. |author2=Dvorak, R. | title= Trojan capture by terrestrial planets | journal= Celestial Mechanics and Dynamical Astronomy | volume=113 | issue=1 | pages=23–34 | date=2012 | doi=10.1007/s10569-012-9404-4| bibcode=2012CeMDA.113...23S |arxiv =1611.07413 |s2cid=254375599 }}</ref>


<ref name="MTArivkin">{{cite journal |author1=Rivkin, Andrew |author2=Trilling, David |author3=Thomas, Cristina |author4=DeMeo, Fancesca |author5=Spahr, Timoth |author6=Binzel, Richard | title= Composition of the L5 Mars Trojans: Neighbors, not siblings | journal= Icarus | volume=192 | issue=2 | pages=434–441 | date=2007 | doi=10.1016/j.icarus.2007.06.026| bibcode=2007Icar..192..434R |arxiv = 0709.1925 }}</ref>
<ref name="MTAmarcos">{{Cite journal|title=Three new stable L<sub>5</sub> Mars Trojans |first1=Carlos |last1=de la Fuente Marcos |last2=de la Fuente Marcos |first2=Raúl |date=April 2013|journal=[[Monthly Notices of the Royal Astronomical Society|Monthly Notices of the Royal Astronomical Society: Letters]]|volume=432|issue=1|pages=L31–L35|doi=10.1093/mnrasl/slt028|arxiv = 1303.0124 |bibcode = 2013MNRAS.432L..31D }}</ref>


<ref name="MTAsholl">{{cite journal |author1=Scholl, H. |author2=Marzari, F. |author3=Tricarico, P. | title= Dynamics of Mars Trojans | journal= Icarus | volume=175 | issue=2 | pages=397–408 | date=2005 | doi=10.1016/j.icarus.2005.01.018| bibcode=2005Icar..175..397S |arxiv = }}</ref>
<ref name="MTAchristou">{{cite journal | author=Christou, A. A. | title= Orbital clustering of Martian Trojans: An asteroid family in the inner solar system? | journal= Icarus | volume=224 | issue=1 | pages=144–153 | date=2013 | doi=10.1016/j.icarus.2013.02.013 | bibcode=2013Icar..224..144C |arxiv= 1303.0420| s2cid= 119186791 }}</ref>


<ref name="MTAschwarz">{{cite journal |author1=Schwarz, R. |author2=Dvorak, R. | title= Trojan capture by terrestrial planets | journal= Celestial Mechanics and Dynamical Astronomy | volume=113 | issue=1 | pages=23–34 | date=2012 | doi=10.1007/s10569-012-9404-4| bibcode=2012CeMDA.113...23S |arxiv =1611.07413 }}</ref>
<ref name="Borisov">{{cite journal|last1=Borisov|first1=G.|last2=Christou|first2=A.|last3=Bagnulo|first3=S.|last4=Cellino|first4=A.|last5=Kwiatkowski|first5=T.|last6=Dell'Oro|first6=A.|title=he olivine-dominated composition of the Eureka family of Mars Trojan asteroids|journal=Monthly Notices of the Royal Astronomical Society|date=2017|volume=466|issue=1|pages=489–495|arxiv=1701.07725|doi=10.1093/mnras/stw3075|bibcode = 2017MNRAS.466..489B }}</ref>


<ref name="MTAmarcos">{{Cite journal|title=Three new stable L<sub>5</sub> Mars Trojans |first=Carlos |last=de la Fuente Marcos |last2=de la Fuente Marcos |first2=Raúl |date=April 2013|journal=[[Monthly Notices of the Royal Astronomical Society|Monthly Notices of the Royal Astronomical Society: Letters]]|volume=432|issue=1|pages=L31-L35|doi=10.1093/mnrasl/slt028|url=http://adsabs.harvard.edu/abs/2013MNRAS.432L..31D|arxiv = 1303.0124 |bibcode = 2013MNRAS.432L..31D }}</ref>
<ref name="Polishook">{{cite journal|last1=Polishook|first1=D.|last2=Jacobson|first2=S. A.|last3=Morbidelli|first3=A.|last4=Aharonson|first4=O.|title=A Martian origin for the Mars Trojan asteroids|journal=Nature Astronomy|date=2017|volume=1|issue=8 |page=0179|doi=10.1038/s41550-017-0179|bibcode = 2017NatAs...1E.179P| arxiv=1710.00024|s2cid=119432820 }}</ref>


<ref name="MTAchristou">{{cite journal | author=Christou, A. A. | title= Orbital clustering of Martian Trojans: An asteroid family in the inner solar system? | journal= Icarus | volume=224 | issue=1 | pages=144–153 | date=2013 | doi=10.1016/j.icarus.2013.02.013 | bibcode=2013Icar..224..144C |arxiv= 1303.0420}}</ref>
<ref name="MTAchristou2">{{cite journal | last1=Christou | first1=Apostolos A. | last2=Borisov | first2=Galin | last3=Dell'Oro | first3=Aldo | last4=Cellino | first4=Alberto | last5=Devogèle | first5=Maxime | title= Composition and origin of L<sub>5</sub> Trojan asteroids of Mars: Insights from spectroscopy | journal= Icarus | volume=354 | issue=1 | pages=113994 (22 pages)| date=January 2021 | doi=10.1016/j.icarus.2020.113994 | bibcode=2021Icar..35413994C | arxiv=2010.10947 | s2cid=224814529 }}</ref>


<ref name="Borisov">{{cite journal|last1=Borisov|first1=G.|last2=Christou|first2=A.|last3=Bagnulo|first3=S.|last4=Cellino|first4=A.|last5=Kwiatkowski|first5=T.|last6=Dell'Oro|first6=A.|title=he olivine-dominated composition of the Eureka family of Mars Trojan asteroids|journal=Monthly Notices of the Royal Astronomical Society|date=2017|volume=466|issue=1|pages=489--495|arxiv=1701.07725|doi=10.1093/mnras/stw3075|bibcode = 2017MNRAS.466..489B }}</ref>
<ref name="MTAmarcos2">{{Cite journal|title=Using Mars co-orbitals to estimate the importance of rotation-induced YORP break-up events in Earth co-orbital space |first1=Carlos |last1=de la Fuente Marcos |last2=de la Fuente Marcos |first2=Raúl |date=March 2021|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=501|issue=4|pages=6007–6025|doi=10.1093/mnras/stab062 |arxiv = 2101.02563| bibcode = 2021MNRAS.501.6007D |url=https://academic.oup.com/mnras/article-abstract/501/4/6007/6081058}}</ref>


<ref name="spectrum2023FW14">{{cite journal
<ref name="Polishook">{{cite journal|last1=Polishook|first1=D.|last2=Jacobson|first2=S. A.|last3=Morbidelli|first3=A.|last4=Aharonson|first4=O.|title=A Martian origin for the Mars Trojan asteroids|journal=Nature Astronomy|date=2017|volume=1|page=0179|doi=10.1038/s41550-017-0179|bibcode = 2017NatAs...1E.179P| arxiv=1710.00024}}</ref>
|last1=de la Fuente Marcos|first1=Raúl
|first2=Julia |last2=de León
|last3=de la Fuente Marcos|first3=Carlos
|first4=Miguel R. |last4=Alarcon
|first5=Javier |last5=Licandro
|first6=Miquel |last6=Serra-Ricart
|first7=Stefan |last7=Geier
|first8=Antonio |last8=Cabrera-Lavers
|title=Dynamics of 2023 FW<sub>14</sub>, the second L<sub>4</sub> Mars trojan, and a physical characterization using the 10.4 m Gran Telescopio Canarias
|journal=[[Astronomy & Astrophysics]], Letters to the Editor |year=2024
|volume=683 |issue=1 |pages=L14 (6 pages)
|arxiv=2403.04061|bibcode=2024A&A...683L..14D
|doi=10.1051/0004-6361/202449688
|date=2024-03-21
|url=https://www.aanda.org/articles/aa/full_html/2024/03/aa49688-24/aa49688-24.html
|doi-access=free}}</ref>


}}
}}
Line 55: Line 110:
{{Small Solar System bodies}}
{{Small Solar System bodies}}
{{Mars}}
{{Mars}}
{{portal bar|Mars}}
{{Portal bar|Solar System}}


[[Category:Mars trojans| ]]
[[Category:Mars trojans| ]]
[[Category:Near-Mars objects]]
[[Category:Trojan minor planets|4]]
[[Category:Trojan minor planets|4]]

Revision as of 20:04, 3 April 2024

The L5 group (shown in green) and the L4 group (light blue) of Mars and Jupiter trojan asteroids shown along with the orbits of Jupiter and the inner planets. Mars is shown in red. The outer orbit is that of Jupiter.
Animation of 1999 UJ7 relative to Sun and Mars 1600-2500
   Sun ·   1999 UJ7 ·   Mars
Animation of 2007 NS2 relative to Sun and Mars 1600-2500
   Sun ·   2007 NS2 ·   Mars

The Mars trojans are a group of trojan objects that share the orbit of the planet Mars around the Sun. They can be found around the two Lagrangian points 60° ahead of and behind Mars. The origin of the Mars trojans is not well understood. One theory suggests that they were primordial objects left over from the formation of Mars that were captured in its Lagrangian points as the Solar System was forming. However, spectral studies of the Mars trojans indicate this may not be the case.[1][2] Another explanation involves asteroids chaotically wandering into the Mars Lagrangian points later in the Solar System's formation. This is also questionable considering the short dynamical lifetimes of these objects.[3][4] The spectra of Eureka and two other Mars trojans indicates an olivine-rich composition.[5] Since olivine-rich objects are rare in the asteroid belt it has been suggested that some of the Mars trojans are captured debris from a large orbit-altering impact on Mars when it encountered a planetary embryo.[6][3]

Presently, this group contains 17 asteroids confirmed to be stable Mars trojans by long-term numerical simulations but only nine of them are accepted by the Minor Planet Center.[7][3][4][8][9][10][11]

Due to close orbital similarities, most of the smaller members of the L5 group are hypothesized to be fragments of Eureka that were detached after it was spun up by the YORP effect (Eureka's rotational period is 2.69 h). The L4 trojan 1999 UJ7 has a much longer rotational period of ~50 h, apparently due to a chaotic rotation that prevents YORP spinup.[12] The spectrum of 121514 show a certain resemblance to that of 2023 FW14 and a common origin cannot be discarded.[13] The spectra of 121514 and 2023 FW14 are very different from those of the Eureka asteroid family members.

List of Mars trojans
Designation Cloud Semimajor axis
(AU) 		Perihelion
(AU) 		Eccentricity Inclination
(°) 		(H) Diameter
(m)
5261 Eureka L5 1.52356 1.42477 0.06484 20.2820 16.13 1880±230
(101429) 1998 VF31 L5 1.52429 1.37150 0.10024 31.2987 17.26 1210+890
−350
(121514) 1999 UJ7 L4 1.52455 1.46491 0.03912 16.7493 17.19 2450±490
(311999) 2007 NS2 L5 1.52379 1.44155 0.05397 18.6194 18.18 790+580
−230
(385250) 2001 DH47 L5 1.52385 1.47111 0.03461 24.4006 18.89 570+420
−170
2009 SE L5 1.52451 1.42524 0.06512 20.6263 19.9 360+260
−110
2011 SL25 L5 1.52391 1.34938 0.11453 21.4953 19.5 430+320
−120
2011 SP189 L5 1.52386 1.46247 0.04029 19.8994 20.9 230+160
−70
2011 SC191 L5 1.52390 1.45678 0.04405 18.7451 19.4 450+330
−130
2011 UN63 L5 1.52378 1.42521 0.06469 20.3635 19.7 390+290
−110
2011 UB256 L5 1.52370 1.41550 0.07101 24.3023 19.9 360+260
−110
2016 AA165 L5 1.52299 1.38650 0.08962 18.7202 20.39 290+210
−90
2016 CP31 L5 1.52365 1.43425 0.05867 23.1314 19.4 450+330
−130
2018 EC4 L5 1.52365 1.43138 0.06056 21.8362 20.0 340+250
−100
2018 FC4 L5 1.52388 1.49781 0.01711 22.1466 21.2 200+140
−60
2018 FM29 L5 1.52391 1.45196 0.04722 21.5004 21.11 210+150
−60
2023 FW14 L4 1.52377 1.28284 0.15811 13.27271 21.59 318+493
−199

See also

References

  1. ^ Rivkin, Andrew; Trilling, David; Thomas, Cristina; DeMeo, Fancesca; Spahr, Timoth; Binzel, Richard (2007). "Composition of the L5 Mars Trojans: Neighbors, not siblings". Icarus. 192 (2): 434–441. arXiv:0709.1925. Bibcode:2007Icar..192..434R. doi:10.1016/j.icarus.2007.06.026. S2CID 15118710.
  2. ^ Trilling, David; Rivking, Andrew; Stansberry, John; Spahr, Timothy; Crudo, Richard; Davies, John (2007). "Albedos and diameters of three Mars Trojan asteroids". Icarus. 192 (2): 442–447. arXiv:0709.1921. Bibcode:2007Icar..192..442T. doi:10.1016/j.icarus.2007.08.002. S2CID 16618044.
  3. ^ a b c Scholl, H.; Marzari, F.; Tricarico, P. (2005). "Dynamics of Mars Trojans". Icarus. 175 (2): 397–408. Bibcode:2005Icar..175..397S. doi:10.1016/j.icarus.2005.01.018.
  4. ^ a b Schwarz, R.; Dvorak, R. (2012). "Trojan capture by terrestrial planets". Celestial Mechanics and Dynamical Astronomy. 113 (1): 23–34. arXiv:1611.07413. Bibcode:2012CeMDA.113...23S. doi:10.1007/s10569-012-9404-4. S2CID 254375599.
  5. ^ Borisov, G.; Christou, A.; Bagnulo, S.; Cellino, A.; Kwiatkowski, T.; Dell'Oro, A. (2017). "he olivine-dominated composition of the Eureka family of Mars Trojan asteroids". Monthly Notices of the Royal Astronomical Society. 466 (1): 489–495. arXiv:1701.07725. Bibcode:2017MNRAS.466..489B. doi:10.1093/mnras/stw3075.
  6. ^ Polishook, D.; Jacobson, S. A.; Morbidelli, A.; Aharonson, O. (2017). "A Martian origin for the Mars Trojan asteroids". Nature Astronomy. 1 (8): 0179. arXiv:1710.00024. Bibcode:2017NatAs...1E.179P. doi:10.1038/s41550-017-0179. S2CID 119432820.
  7. ^ "List Of Martian Trojans". Minor Planet Center. Retrieved 2021-01-12.
  8. ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (April 2013). "Three new stable L5 Mars Trojans". Monthly Notices of the Royal Astronomical Society: Letters. 432 (1): L31–L35. arXiv:1303.0124. Bibcode:2013MNRAS.432L..31D. doi:10.1093/mnrasl/slt028.
  9. ^ Christou, A. A. (2013). "Orbital clustering of Martian Trojans: An asteroid family in the inner solar system?". Icarus. 224 (1): 144–153. arXiv:1303.0420. Bibcode:2013Icar..224..144C. doi:10.1016/j.icarus.2013.02.013. S2CID 119186791.
  10. ^ Christou, Apostolos A.; Borisov, Galin; Dell'Oro, Aldo; Cellino, Alberto; Devogèle, Maxime (January 2021). "Composition and origin of L5 Trojan asteroids of Mars: Insights from spectroscopy". Icarus. 354 (1): 113994 (22 pages). arXiv:2010.10947. Bibcode:2021Icar..35413994C. doi:10.1016/j.icarus.2020.113994. S2CID 224814529.
  11. ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (March 2021). "Using Mars co-orbitals to estimate the importance of rotation-induced YORP break-up events in Earth co-orbital space". Monthly Notices of the Royal Astronomical Society. 501 (4): 6007–6025. arXiv:2101.02563. Bibcode:2021MNRAS.501.6007D. doi:10.1093/mnras/stab062.
  12. ^ Lovett, R. (2017-10-20). "Sun's light touch explains asteroids flying in formation behind Mars". Science. doi:10.1126/science.aar2794.
  13. ^ de la Fuente Marcos, Raúl; de León, Julia; de la Fuente Marcos, Carlos; Alarcon, Miguel R.; Licandro, Javier; Serra-Ricart, Miquel; Geier, Stefan; Cabrera-Lavers, Antonio (2024-03-21). "Dynamics of 2023 FW14, the second L4 Mars trojan, and a physical characterization using the 10.4 m Gran Telescopio Canarias". Astronomy & Astrophysics, Letters to the Editor. 683 (1): L14 (6 pages). arXiv:2403.04061. Bibcode:2024A&A...683L..14D. doi:10.1051/0004-6361/202449688.{{cite journal}}: CS1 maint: date and year (link)
Retrieved from "https://en.wikipedia.org/w/index.php?title=Mars_trojan&oldid=1217092194"