Spin Rate of Asteroid (54509) YORP Increasing due to the YORP Effect

Patrick A. Taylor; J. L. Margot; D. Vokrouhlicky; D. J. Scheeres; P. Pravec; S. C. Lowry; A. Fitzsimmons; M. C. Nolan; S. J. Ostro; L. A. Benner; J. D. Giorgini; C. Magri

Spin Rate of Asteroid (54509) YORP Increasing due to the YORP Effect

Patrick A. Taylor
, J. L. Margot
, D. Vokrouhlicky
, D. J. Scheeres
, P. Pravec
, S. C. Lowry
, A. Fitzsimmons
, M. C. Nolan
, S. J. Ostro
, L. A. Benner
, J. D. Giorgini
, C. Magri

Research output: Contribution to conference › Abstract › peer-review

Abstract

Arecibo S-band (2380 MHz, 13 cm) and Goldstone X-band (8560 MHz, 3.5 cm) radar observations from 2001, 2004, and 2005 [1] along with precise optical observations [2] reveal that the observed change in spin rate of near-Earth asteroid (54509) YORP, formerly 2000 PH5, is due to the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, a torque due to sunlight. The increase in sidereal spin rate of (2.0 ± 0.2) x 10-4 deg/day2 [2], equivalently a shortening of the sidereal spin period by just over one millisecond per year, is in reasonable agreement with theoretical predictions for the YORP acceleration of a body with the radar-determined size, shape, and spin state of asteroid (54509) YORP. The detection of asteroid spin-up supports the YORP effect as an explanation for the anomalous distribution of spin rates for asteroids under 10 km in diameter and as a binary formation mechanism. [1] P. A. Taylor et al., Science, 316, 2007. [2] S. C. Lowry et al., Science, 316, 2007.

Original language	English
Publication status	Published - 01 Oct 2007

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http://adsabs.harvard.edu/abs/2007DPS....39.0503T

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@conference{fc1b6a7e9f764a7b8a9b41eb0a2b020c,

title = "Spin Rate of Asteroid (54509) YORP Increasing due to the YORP Effect",

abstract = "Arecibo S-band (2380 MHz, 13 cm) and Goldstone X-band (8560 MHz, 3.5 cm) radar observations from 2001, 2004, and 2005 [1] along with precise optical observations [2] reveal that the observed change in spin rate of near-Earth asteroid (54509) YORP, formerly 2000 PH5, is due to the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, a torque due to sunlight. The increase in sidereal spin rate of (2.0 ± 0.2) x 10-4 deg/day2 [2], equivalently a shortening of the sidereal spin period by just over one millisecond per year, is in reasonable agreement with theoretical predictions for the YORP acceleration of a body with the radar-determined size, shape, and spin state of asteroid (54509) YORP. The detection of asteroid spin-up supports the YORP effect as an explanation for the anomalous distribution of spin rates for asteroids under 10 km in diameter and as a binary formation mechanism. [1] P. A. Taylor et al., Science, 316, 2007. [2] S. C. Lowry et al., Science, 316, 2007.",

author = "Taylor, \{Patrick A.\} and Margot, \{J. L.\} and D. Vokrouhlicky and Scheeres, \{D. J.\} and P. Pravec and Lowry, \{S. C.\} and A. Fitzsimmons and Nolan, \{M. C.\} and Ostro, \{S. J.\} and Benner, \{L. A.\} and Giorgini, \{J. D.\} and C. Magri",

year = "2007",

month = oct,

day = "1",

language = "English",

}

TY - CONF

T1 - Spin Rate of Asteroid (54509) YORP Increasing due to the YORP Effect

AU - Taylor, Patrick A.

AU - Margot, J. L.

AU - Vokrouhlicky, D.

AU - Scheeres, D. J.

AU - Pravec, P.

AU - Lowry, S. C.

AU - Fitzsimmons, A.

AU - Nolan, M. C.

AU - Ostro, S. J.

AU - Benner, L. A.

AU - Giorgini, J. D.

AU - Magri, C.

PY - 2007/10/1

Y1 - 2007/10/1

N2 - Arecibo S-band (2380 MHz, 13 cm) and Goldstone X-band (8560 MHz, 3.5 cm) radar observations from 2001, 2004, and 2005 [1] along with precise optical observations [2] reveal that the observed change in spin rate of near-Earth asteroid (54509) YORP, formerly 2000 PH5, is due to the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, a torque due to sunlight. The increase in sidereal spin rate of (2.0 ± 0.2) x 10-4 deg/day2 [2], equivalently a shortening of the sidereal spin period by just over one millisecond per year, is in reasonable agreement with theoretical predictions for the YORP acceleration of a body with the radar-determined size, shape, and spin state of asteroid (54509) YORP. The detection of asteroid spin-up supports the YORP effect as an explanation for the anomalous distribution of spin rates for asteroids under 10 km in diameter and as a binary formation mechanism. [1] P. A. Taylor et al., Science, 316, 2007. [2] S. C. Lowry et al., Science, 316, 2007.

AB - Arecibo S-band (2380 MHz, 13 cm) and Goldstone X-band (8560 MHz, 3.5 cm) radar observations from 2001, 2004, and 2005 [1] along with precise optical observations [2] reveal that the observed change in spin rate of near-Earth asteroid (54509) YORP, formerly 2000 PH5, is due to the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, a torque due to sunlight. The increase in sidereal spin rate of (2.0 ± 0.2) x 10-4 deg/day2 [2], equivalently a shortening of the sidereal spin period by just over one millisecond per year, is in reasonable agreement with theoretical predictions for the YORP acceleration of a body with the radar-determined size, shape, and spin state of asteroid (54509) YORP. The detection of asteroid spin-up supports the YORP effect as an explanation for the anomalous distribution of spin rates for asteroids under 10 km in diameter and as a binary formation mechanism. [1] P. A. Taylor et al., Science, 316, 2007. [2] S. C. Lowry et al., Science, 316, 2007.

M3 - Abstract

ER -

Spin Rate of Asteroid (54509) YORP Increasing due to the YORP Effect

Abstract

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