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Padua family

From Wikipedia, the free encyclopedia

The Padua family (FIN: 507), also known as the Lydia family, is a mid-sized family of asteroids of more than a thousand members.

The family is at least 25 million years old. Its members were previously associated to 110 Lydia, and are predominantly X-type asteroids with an albedo of approximately 0.1. Together with the Agnia family, the Padua family is the only other family to have most of its members in a nonlinear secular resonance configuration with more than 75% of its members in a z1 librating state.[1][2][3]: 23 

The Paduan (Lydian) asteroids are located in the outer part of the central asteroid belt having a semi-major axis of approximately 2.75. The family's namesake is the asteroid 363 Padua, while 110 Lydia is now a suspected interloper, despite having the same spectral type.[1][3]: 23 

Members

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Some prominent members with known spectral type.[1]: 364  A list of all Paduan asteroids is given at the "Small Bodies Data Ferret".[4]

Name Type Diameter Albedo Catalog Refs
110 Lydia X 86 0.1808 list JPL · MPC · LCDB
363 Padua X 88 0.057 list JPL · MPC · LCDB
1517 Beograd X 36 0.0448 list JPL · MPC · LCDB
1766 Slipher C 20 0.057 list JPL · MPC · LCDB
2306 Bauschinger X 21 0.0526 list JPL · MPC · LCDB
2560 Siegma Xc 20 0.057 list JPL · MPC · LCDB
3020 Naudts Sl 16 0.057 list JPL · MPC · LCDB
3670 Northcott X 19 0.045 list JPL · MPC ·
5087 Emelʹyanov X 13 0.057 list JPL · MPC · LCDB
5103 Diviš X 12 0.074 list JPL · MPC ·
8450 Egorov C 11 0.058 list JPL · MPC ·
12281 Chaumont X 16 0.032 list JPL · MPC ·
Diameter and albedo figures taken from the LCDB, or, if not available, from JPL's SBDB. Also see category.

Lydia former namesake and potential interloper

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In previous works (Zappala et al. 1995), this family was named Lydia after 110 Lydia, which is an X-type asteroid in the SMASS classification (Tholen: M-type). While Lydia is still a member of the now-called Padua family (Nesvorny 2005, AstDyS), it has been suspected that it might be an interloper in its "own" family despite its matching spectral type (Carruba 2009; Mothe-Diniz et al. 2005).[1]: 369 

Also, the asteroid 308 Polyxo was formerly considered the family's largest member.[5] This T-type asteroid is no-longer considered a family member and is categorized as a background asteroid on AstDyS.[4][6]

References

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  1. ^ a b c d Carruba, V. (May 2009). "The (not so) peculiar case of the Padua family". Monthly Notices of the Royal Astronomical Society. 395 (1): 358–377. Bibcode:2009MNRAS.395..358C. doi:10.1111/j.1365-2966.2009.14523.x.
  2. ^ Carruba, V.; Domingos, R. C.; Nesvorný, D.; Roig, F.; Huaman, M. E.; Souami, D. (August 2013). "A multidomain approach to asteroid families' identification". Monthly Notices of the Royal Astronomical Society. 433 (3): 2075–2096. arXiv:1305.4847. Bibcode:2013MNRAS.433.2075C. doi:10.1093/mnras/stt884. S2CID 118511004.
  3. ^ a b 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. S2CID 119280014.
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Archived from the original on 16 August 2017. Retrieved 22 July 2017.
  5. ^ Ridpath, Ian (2003). Oxford Dictionary of Astronomy. Oxford University Press. ISBN 0199609055. Retrieved 25 January 2016.
  6. ^ "AstDyS-2 data for (308) Polyxo". AstDyS – Asteroids Dynamic Site. Retrieved 30 August 2017.