A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion
The rubble pile spin barrier is an upper limit on the rotation rate of asteroids larger than ~200-300. m. Among thousands of asteroids with diameters larger than ~300. m, only a handful of asteroids are known to rotate faster than 2.0. h, all are in the sub-km range (≤0.6. km). Here we present photo...
| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Article |
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Elsevier BV
2018
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| Online Access: | http://hdl.handle.net/1721.1/114833 https://orcid.org/0000-0003-0000-0572 |
| _version_ | 1826194629159026688 |
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| author | Polishook, D. Moskovitz, N. Hinkle, M.L. Lockhart, M. Mommert, M. Thirouin, A. Thomas, C.A. Trilling, D. Willman, M. Aharonson, O. Binzel, Richard P Burt, Brian DeMeo, Francesca E Person, Michael J. |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Polishook, D. Moskovitz, N. Hinkle, M.L. Lockhart, M. Mommert, M. Thirouin, A. Thomas, C.A. Trilling, D. Willman, M. Aharonson, O. Binzel, Richard P Burt, Brian DeMeo, Francesca E Person, Michael J. |
| author_sort | Polishook, D. |
| collection | MIT |
| description | The rubble pile spin barrier is an upper limit on the rotation rate of asteroids larger than ~200-300. m. Among thousands of asteroids with diameters larger than ~300. m, only a handful of asteroids are known to rotate faster than 2.0. h, all are in the sub-km range (≤0.6. km). Here we present photometric measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt asteroid with a relatively large diameter of 2.3-0.7+0.6km, completes one rotation in 1.9529. ±. 0.0002. h. Its unique diameter and rotation period allow us to examine scenarios about asteroid internal structure and evolution: a rubble pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic structure; an asteroid experiencing mass shedding; an asteroid experiencing YORP spin-up/down; and an asteroid with a unique octahedron shape results with a four-peak lightcurve and a 3.9. h period. We find that the most likely scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from disrupting without requiring a monolithic structure or a unique shape. Due to the uniqueness of (60716) 2000 GD65, we suggest that most asteroids typically have smaller cohesion than that of lunar regolith. Keywords: Asteroids; Asteroids, rotation; Rotational dynamics; Photometry |
| first_indexed | 2024-09-23T09:58:53Z |
| format | Article |
| id | mit-1721.1/114833 |
| institution | Massachusetts Institute of Technology |
| last_indexed | 2024-09-23T09:58:53Z |
| publishDate | 2018 |
| publisher | Elsevier BV |
| record_format | dspace |
| spelling | mit-1721.1/1148332024-05-15T05:30:37Z A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion Polishook, D. Moskovitz, N. Hinkle, M.L. Lockhart, M. Mommert, M. Thirouin, A. Thomas, C.A. Trilling, D. Willman, M. Aharonson, O. Binzel, Richard P Burt, Brian DeMeo, Francesca E Person, Michael J. Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Binzel, Richard P Burt, Brian DeMeo, Francesca E Person, Michael J The rubble pile spin barrier is an upper limit on the rotation rate of asteroids larger than ~200-300. m. Among thousands of asteroids with diameters larger than ~300. m, only a handful of asteroids are known to rotate faster than 2.0. h, all are in the sub-km range (≤0.6. km). Here we present photometric measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt asteroid with a relatively large diameter of 2.3-0.7+0.6km, completes one rotation in 1.9529. ±. 0.0002. h. Its unique diameter and rotation period allow us to examine scenarios about asteroid internal structure and evolution: a rubble pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic structure; an asteroid experiencing mass shedding; an asteroid experiencing YORP spin-up/down; and an asteroid with a unique octahedron shape results with a four-peak lightcurve and a 3.9. h period. We find that the most likely scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from disrupting without requiring a monolithic structure or a unique shape. Due to the uniqueness of (60716) 2000 GD65, we suggest that most asteroids typically have smaller cohesion than that of lunar regolith. Keywords: Asteroids; Asteroids, rotation; Rotational dynamics; Photometry United States. National Aeronautics and Space Administration (Grant NNX12AL26G) 2018-04-20T20:17:34Z 2018-04-20T20:17:34Z 2015-12 2015-12 2018-04-19T18:59:30Z Article http://purl.org/eprint/type/JournalArticle 0019-1035 1090-2643 http://hdl.handle.net/1721.1/114833 Polishook, D. et al. “A 2 Km-Size Asteroid Challenging the Rubble-Pile Spin Barrier – A Case for Cohesion.” Icarus 267 (March 2016): 243–254 © 2015 Elsevier Inc https://orcid.org/0000-0003-0000-0572 http://dx.doi.org/10.1016/J.ICARUS.2015.12.031 Icarus Creative Commons Attribution-NonCommercial-NoDerivs License http://creativecommons.org/licenses/by-nc-nd/4.0/ application/pdf Elsevier BV arXiv |
| spellingShingle | Polishook, D. Moskovitz, N. Hinkle, M.L. Lockhart, M. Mommert, M. Thirouin, A. Thomas, C.A. Trilling, D. Willman, M. Aharonson, O. Binzel, Richard P Burt, Brian DeMeo, Francesca E Person, Michael J. A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title | A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title_full | A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title_fullStr | A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title_full_unstemmed | A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title_short | A 2km-size asteroid challenging the rubble-pile spin barrier – A case for cohesion |
| title_sort | 2km size asteroid challenging the rubble pile spin barrier a case for cohesion |
| url | http://hdl.handle.net/1721.1/114833 https://orcid.org/0000-0003-0000-0572 |
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