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Maria family

Asteroid family

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. It is also known as the Roma family, named after its alternative parent body, 472 Roma.

The family was initially identified by Japanese astronomer Kiyotsugu Hirayama in 1918. Asteroids in this family typically have a semi-major axis between 2.52−2.62 AU, and an inclination of 12 to 17°.

Members

The family consists of 2940 known members based on the HCM method. Its largest members are the asteroids 170 Maria and 472 Roma. A complete synthetic HCM-listing for all members can be obtained by using the Ferret Interactive Search.

Name	a	e	i		SBDB
170 Maria	2.553	0.065	14.40°
472 Roma	2.545	0.094	15.80°

Name	a	e	i
292 Ludovica	2.529	0.034	14.92°
652 Jubilatrix	2.554	0.127	15.77°
714 Ulula	2.535	0.058	14.27°
787 Moskva	2.539	0.129	14.84°
875 Nymphe	2.552	0.151	14.59°
879 Ricarda	2.531	0.155	13.68°
897 Lysistrata	2.541	0.094	14.32°
1158 Luda	2.564	0.112	14.85°
1215 Boyer	2.578	0.133	15.91°
2089 Cetacea	2.533	0.156	15.39°
3066 McFadden	2.527	0.133	15.57°

Interlopers

Although 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.

References

|access-date= 25 April 2018}}

|archive-url = https://web.archive.org/web/20170802210005/http://sbntools.psi.edu/ferret/PropertySearch/familyForm.action |archive-date = 2 August 2017 |url-status = dead

References

[http://www.easysky.de/eng/screenshots/index.htm EasySky – Screenshots]

Info: Wikipedia Source

This article was imported from Wikipedia and is available under the Creative Commons Attribution-ShareAlike 4.0 License. Content has been adapted to SurfDoc format. Original contributors can be found on the article history page.

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