Rotational properties of the Maria asteroid family

M. J. Kim, Y. J. Choi, H. K. Moon, Yong-Ik Byun, N. Brosch, M. Kaplan, S. Kaynar, Ö Uysal, E. Güzel, R. Behrend, J. N. Yoon, S. Mottola, S. Hellmich, T. C. Hinse, Z. Eker, J. H. Park

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

The Maria family is regarded as an old-type (3 ± 1 Gyr) asteroid family that has experienced substantial collisional and dynamical evolution in the main belt. It is located near the 3:1 Jupiter mean-motion resonance area that supplies near-Earth asteroids to the inner solar system. We carried out observations of Maria family asteroids during 134 nights from 2008 July to 2013 May and derived synodic rotational periods for 51 objects, including newly obtained periods of 34 asteroids. We found that there is a significant excess of fast and slow rotators in the observed rotation rate distribution. The one-sample Kolmogorov-Smirnov test confirms that the spin rate distribution is not consistent with a Maxwellian at a 92% confidence level. From correlations among rotational periods, amplitudes of light curves, and sizes, we conclude that the rotational properties of Maria family asteroids have been changed considerably by non-gravitational forces such as the YORP effect. Using a light-curve inversion method, we successfully determined the pole orientations for 13 Maria members and found an excess of prograde versus retrograde spins with a ratio (Np /Nr ) of 3. This implies that the retrograde rotators could have been ejected by the 3:1 resonance into the inner solar system since the formation of the Maria family. We estimate that approximately 37-75 Maria family asteroids larger than 1 km have entered near-Earth space every 100 Myr.

Original languageEnglish
Article number56
JournalAstronomical Journal
Volume147
Issue number3
DOIs
Publication statusPublished - 2014 Mar 1

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maria
asteroids
asteroid
solar system
light curve
Kolmogorov-Smirnov test
Jupiter (planet)
Jupiter
night
family
confidence
poles
inversions
estimates

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kim, M. J., Choi, Y. J., Moon, H. K., Byun, Y-I., Brosch, N., Kaplan, M., ... Park, J. H. (2014). Rotational properties of the Maria asteroid family. Astronomical Journal, 147(3), [56]. https://doi.org/10.1088/0004-6256/147/3/56
Kim, M. J. ; Choi, Y. J. ; Moon, H. K. ; Byun, Yong-Ik ; Brosch, N. ; Kaplan, M. ; Kaynar, S. ; Uysal, Ö ; Güzel, E. ; Behrend, R. ; Yoon, J. N. ; Mottola, S. ; Hellmich, S. ; Hinse, T. C. ; Eker, Z. ; Park, J. H. / Rotational properties of the Maria asteroid family. In: Astronomical Journal. 2014 ; Vol. 147, No. 3.
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Kim, MJ, Choi, YJ, Moon, HK, Byun, Y-I, Brosch, N, Kaplan, M, Kaynar, S, Uysal, Ö, Güzel, E, Behrend, R, Yoon, JN, Mottola, S, Hellmich, S, Hinse, TC, Eker, Z & Park, JH 2014, 'Rotational properties of the Maria asteroid family', Astronomical Journal, vol. 147, no. 3, 56. https://doi.org/10.1088/0004-6256/147/3/56

Rotational properties of the Maria asteroid family. / Kim, M. J.; Choi, Y. J.; Moon, H. K.; Byun, Yong-Ik; Brosch, N.; Kaplan, M.; Kaynar, S.; Uysal, Ö; Güzel, E.; Behrend, R.; Yoon, J. N.; Mottola, S.; Hellmich, S.; Hinse, T. C.; Eker, Z.; Park, J. H.

In: Astronomical Journal, Vol. 147, No. 3, 56, 01.03.2014.

Research output: Contribution to journalArticle

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T1 - Rotational properties of the Maria asteroid family

AU - Kim, M. J.

AU - Choi, Y. J.

AU - Moon, H. K.

AU - Byun, Yong-Ik

AU - Brosch, N.

AU - Kaplan, M.

AU - Kaynar, S.

AU - Uysal, Ö

AU - Güzel, E.

AU - Behrend, R.

AU - Yoon, J. N.

AU - Mottola, S.

AU - Hellmich, S.

AU - Hinse, T. C.

AU - Eker, Z.

AU - Park, J. H.

PY - 2014/3/1

Y1 - 2014/3/1

N2 - The Maria family is regarded as an old-type (3 ± 1 Gyr) asteroid family that has experienced substantial collisional and dynamical evolution in the main belt. It is located near the 3:1 Jupiter mean-motion resonance area that supplies near-Earth asteroids to the inner solar system. We carried out observations of Maria family asteroids during 134 nights from 2008 July to 2013 May and derived synodic rotational periods for 51 objects, including newly obtained periods of 34 asteroids. We found that there is a significant excess of fast and slow rotators in the observed rotation rate distribution. The one-sample Kolmogorov-Smirnov test confirms that the spin rate distribution is not consistent with a Maxwellian at a 92% confidence level. From correlations among rotational periods, amplitudes of light curves, and sizes, we conclude that the rotational properties of Maria family asteroids have been changed considerably by non-gravitational forces such as the YORP effect. Using a light-curve inversion method, we successfully determined the pole orientations for 13 Maria members and found an excess of prograde versus retrograde spins with a ratio (Np /Nr ) of 3. This implies that the retrograde rotators could have been ejected by the 3:1 resonance into the inner solar system since the formation of the Maria family. We estimate that approximately 37-75 Maria family asteroids larger than 1 km have entered near-Earth space every 100 Myr.

AB - The Maria family is regarded as an old-type (3 ± 1 Gyr) asteroid family that has experienced substantial collisional and dynamical evolution in the main belt. It is located near the 3:1 Jupiter mean-motion resonance area that supplies near-Earth asteroids to the inner solar system. We carried out observations of Maria family asteroids during 134 nights from 2008 July to 2013 May and derived synodic rotational periods for 51 objects, including newly obtained periods of 34 asteroids. We found that there is a significant excess of fast and slow rotators in the observed rotation rate distribution. The one-sample Kolmogorov-Smirnov test confirms that the spin rate distribution is not consistent with a Maxwellian at a 92% confidence level. From correlations among rotational periods, amplitudes of light curves, and sizes, we conclude that the rotational properties of Maria family asteroids have been changed considerably by non-gravitational forces such as the YORP effect. Using a light-curve inversion method, we successfully determined the pole orientations for 13 Maria members and found an excess of prograde versus retrograde spins with a ratio (Np /Nr ) of 3. This implies that the retrograde rotators could have been ejected by the 3:1 resonance into the inner solar system since the formation of the Maria family. We estimate that approximately 37-75 Maria family asteroids larger than 1 km have entered near-Earth space every 100 Myr.

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