The Maria family (adj. Marian; FIN: 506; also known as the Roma family) is a collisional asteroid family located in the inner parts of the intermediate asteroid belt, near the 1:3 Kirkwood gap. The family consist of several thousand stony S-type asteroids. It is named after its parent body and lowest numbered member, the asteroid 170 Maria.[1][2]: 23 It is also known as the Roma family, named after its alternative parent body, 472 Roma.[3]
The family was initially identified by Japanese astronomer Kiyotsugu Hirayama in 1918.[1] Asteroids in this family typically have a semi-major axis between 2.52−2.62 AU, and an inclination of 12 to 17°.[4]
Members
editThe family consists of 2940 known members based on the HCM method. Its largest members are the asteroids 170 Maria and 472 Roma.[2]: 23 A complete synthetic HCM-listing for all members can be obtained by using the Ferret Interactive Search.[5]
| Name | a | e | i | SBDB |
|---|---|---|---|---|
| 170 Maria | 2.553 | 0.065 | 14.40° | JPL |
| 472 Roma | 2.545 | 0.094 | 15.80° | JPL |
| Name | a | e | i | SBDB |
|---|---|---|---|---|
| 292 Ludovica | 2.529 | 0.034 | 14.92° | JPL |
| 652 Jubilatrix | 2.554 | 0.127 | 15.77° | JPL |
| 714 Ulula | 2.535 | 0.058 | 14.27° | JPL |
| 787 Moskva | 2.539 | 0.129 | 14.84° | JPL |
| 875 Nymphe | 2.552 | 0.151 | 14.59° | JPL |
| 879 Ricarda | 2.531 | 0.155 | 13.68° | JPL |
| 897 Lysistrata | 2.541 | 0.094 | 14.32° | JPL |
| 1158 Luda | 2.564 | 0.112 | 14.85° | JPL |
| 1215 Boyer | 2.578 | 0.133 | 15.91° | JPL |
| 2089 Cetacea | 2.533 | 0.156 | 15.39° | JPL |
| 3066 McFadden | 2.527 | 0.133 | 15.57° | JPL |
Interlopers
editAlthough asteroid 695 Bella has orbital properties that make it a candidate for this family, the spectral properties of the object indicate it is most likely an interloper. Instead, it may have been spalled off from 6 Hebe, or its parent body.[1]
References
edit- ^ a b c d Fieber-Beyer, Sherry K.; Gaffey, Michael J.; Kelley, Michael S.; Reddy, Vishnu; Reynolds, Chalbeth M.; Hicks, Tony (June 2011). "The Maria asteroid family: Genetic relationships and a plausible source of mesosiderites near the 3:1 Kirkwood Gap". Icarus. 213 (2): 524–537. Bibcode:2011Icar..213..524F. doi:10.1016/j.icarus.2011.03.009. Retrieved 25 April 2018.
- ^ a b c Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
- ^ Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Grav, T.; Nugent, C. R.; Stevenson, R. (June 2013). "Asteroid Family Identification Using the Hierarchical Clustering Method and WISE/NEOWISE Physical Properties". The Astrophysical Journal. 770 (1): 22. arXiv:1305.1607. Bibcode:2013ApJ...770....7M. doi:10.1088/0004-637X/770/1/7.
- ^ EasySky – Screenshots
- ^ "Small Bodies Data Ferret". Synthetic Family (170) Maria – Nesvorny HCM Asteroid Families V3.0. Archived from the original on 2 August 2017. Retrieved 22 July 2017. (Query)