Arjuna asteroid: Difference between revisions
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|date = July 2013 |
|date = July 2013 |
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|title = A resonant family of dynamically cold small bodies in the near-Earth asteroid belt |
|title = A resonant family of dynamically cold small bodies in the near-Earth asteroid belt |
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|url = https://arxiv.org/pdf/1305.2825.pdf |
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|journal = [[Monthly Notices of the Royal Astronomical Society: Letters]] |
|journal = [[Monthly Notices of the Royal Astronomical Society: Letters]] |
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|volume = 434 |
|volume = 434 |
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|doi = 10.1093/mnrasl/slt062 |
|doi = 10.1093/mnrasl/slt062 |
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|arxiv = 1305.2825 |
|arxiv = 1305.2825 |
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}}</ref> |
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<ref name="Fuente-2015">{{Cite journal |
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|date = January 2015 |
|date = January 2015 |
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|title = Geometric characterization of the Arjuna orbital domain |
|title = Geometric characterization of the Arjuna orbital domain |
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|url = https://arxiv.org/pdf/1410.4104.pdf |
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|journal = [[Astronomische Nachrichten]] |
|journal = [[Astronomische Nachrichten]] |
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|volume = 336 |
|volume = 336 |
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|doi = 10.1002/asna.201412133 |
|doi = 10.1002/asna.201412133 |
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|arxiv = 1410.4104 |
|arxiv = 1410.4104 |
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Revision as of 00:59, 2 May 2020
The Arjuna asteroids (also known as "Arjunas") are a dynamical group of asteroids in the Solar System. Arjunas are near-Earth objects (NEOs) whose orbits are very Earth-like in character, having low inclination, orbital periods close to one year, and low eccentricity. The group is named after Arjuna, a central hero in Hindu mythology. The definition is somewhat vague and overlaps the definition of the three well-established Apollo, Amor and Aten groups. They constitute a dynamically cold group of small NEOs that experience repeated trappings in the 1:1 mean-motion resonance with the Earth.[1][2]
Members
Potential members of the Arjuna group with their Apollo (APO) or Aten (ATE) group classification in parenthesis, include:
- 1991 VG (APO)
- 2003 YN107 (ATE)
- 2006 JY26 (APO)
- 2009 SH2 (ATE)
- 2013 BS45 (ATE)
References
- ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (July 2013). "A resonant family of dynamically cold small bodies in the near-Earth asteroid belt". Monthly Notices of the Royal Astronomical Society: Letters. 434 (1): L1–L5. arXiv:1305.2825. Bibcode:2013MNRAS.434L...1D. doi:10.1093/mnrasl/slt062.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ de la Fuente Marcos, C.; de la Fuente Marcos, R. (January 2015). "Geometric characterization of the Arjuna orbital domain". Astronomische Nachrichten. 336 (1): 5. arXiv:1410.4104. Bibcode:2015AN....336....5D. doi:10.1002/asna.201412133.
Further reading
- Evidence for a near-Earth asteroid belt Rabinowitz, David L.; Gehrels, Tom; Scotti, James V.; McMillan, Robert S.; Perry, Marcus L.; Wiśniewski, Wiesław Z.; Larson, Stephen M.; Howell, Ellen S.; & Mueller, Beatrice E. A. (1993), Nature, Volume 363, no. 6431, pp. 704-706.
- The Near-Earth Object Population Gladman, Brett J.; Michel, Patrick; & Froeschlé, Claude (2000), Icarus, Volume 146, Issue 1, pp. 176-189.
- A resonant family of dynamically cold small bodies in the near-Earth asteroid belt de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (2013), Monthly Notices of the Royal Astronomical Society: Letters, Volume 434, Issue 1, pp. L1-L5.
- Geometric characterization of the Arjuna orbital domain de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (2015), Astronomische Nachrichten, Volume 336, Issue 1, pp. 5–22.
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