Open Access
Rotational Breakup as the Origin of Small Binary Asteroids
Kevin J. Walsh,Kevin J. Walsh,Derek C. Richardson,Patrick Michel +3 more
- Vol. 1405, pp 8138
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TLDR
It is found that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation.Abstract:
Many asteroids and trans-neptunian objects have satellites: the tally stands at over 150 on http://tinyurl.com/dweqf
. The smallest of these binary systems are main-belt and near-Earth asteroids, but the environments of these two types of object are very different, making it difficult to work out a common mechanism to explain their formation. Now Walsh et al. present a model that fits the bill. Properties of the observed main-belt and near-Earth asteroids with satellites are matched by simulations involving the slow spinup of a 'rubble pile' asteroid via the thermal YORP effect (where radiation from an irregular body exerts a net force on that body). The mass shed from the equator of a spinning body accretes into a satellite if the material consists of particles undergoing energy-dissipating collisions. Binary asteroids are created by the slow spin up of a 'rubble pile' asteroid via the thermal YORP effect (where radiation from an irregularly shaped body exerts a net force on the body). The mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative. Asteroids with satellites are observed throughout the Solar System, from subkilometre near-Earth asteroid pairs to systems of large and distant bodies in the Kuiper belt. The smallest and closest systems are found among the near-Earth and small inner main-belt asteroids, which typically have rapidly rotating primaries and close secondaries on circular orbits. About 15 per cent of near-Earth and main-belt asteroids with diameters under 10 km have satellites1,2. The mechanism that forms such similar binaries in these two dynamically different populations was hitherto unclear. Here we show that these binaries are created by the slow spinup of a ‘rubble pile’ asteroid by means of the thermal YORP (Yarkovsky–O’Keefe–Radzievskii–Paddack) effect. We find that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation. The satellite forms mostly from material originating near the primary’s surface and enters into a close, low-eccentricity orbit. The properties of binaries produced by our model match those currently observed in the small near-Earth and main-belt asteroid populations, including 1999 KW4 (refs 3, 4).read more
Citations
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The active asteroids
TL;DR: In this paper, the authors consider 11 dynamical asteroids losing mass, in nine of which the ejected material is spatially resolved, and address mechanisms for producing mass loss including rotational instability, impact ejection, electrostatic repulsion, radiation pressure sweeping, dehydration stresses, and thermal fracture, in addition to the sublimation of ice.
Detection of the YORP Effect on Asteroid (1620) Geographos
J. Durech,D. Vokrouchlicky,David Higgins,Yu. N. Krugly,N. Gaftonyuk,Vasilij G. Chiorny,Vasilij G. Shevchenko,Mikko Kaasalainen +7 more
TL;DR: In this article, the authors used the lightcurve inversion method to model the shape and spin state of Geographos and obtained an excellent agreement between the model and observations, with the best-fit value υ = (1.15 ± 0.15) × 10 −8 rad d −2.
The Influence of Global-Selfheating on the Yarkovsky and YORP Effects
Benjamin Rozitis,S. F. Green,S. R. Duddy,Alan Fitzsimmons,Michael D. Hicks,S. C. Lowry,Colin Snodgrass,Paul R. Weissman,S. D. Wolters +8 more
TL;DR: In this paper, the authors present an adaptation of the Advanced Thermophysical Model to simultaneously predict the Yarkovsky and YORP effects in the presence of global self-heating that occurs within the large concavities of irregularly shaped asteroids, which has been neglected or dismissed in all previous models.
The ESA Hera Mission: Detailed Characterization of the DART Impact Outcome and of the Binary Asteroid (65803) Didymos
Patrick Michel,Michael Küppers,A. Campo Bagatin,Benoit Carry,Sébastien Charnoz,J. de León,Alan Fitzsimmons,Paulo Gordo,Simon F. Green,Alain Herique,Martin Juzi,Özgür Karatekin,Tomas Kohout,Monica Lazzarin,Naomi Murdoch,Tatsuaki Okada,Ernesto Palomba,Petr Pravec,Colin Snodgrass,Paolo Tortora,Kleomenis Tsiganis,Stephan Ulamec,Jean-Baptiste Vincent,Kai Wünnemann,Yun Zhang,S.D. Raducan,E. Dotto,Nancy L. Chabot,Andrew F. Cheng,Andrew S. Rivkin,Olivier S. Barnouin,Carolyn M. Ernst,Angela Stickle,Derek C. Richardson,Cristina A. Thomas,Masahiko Arakawa,Hirdy Miyamoto,Akiko M. Nakamura,Seiji Sugita,Makoto Yoshikawa,Paul A. Abell,Erik Asphaug,Ronald-Louis Ballouz,William F. Bottke,Dante S. Lauretta,Kevin J. Walsh,Paolo De Martino,Ian Carnelli +47 more
TL;DR: Hera as discussed by the authors is a planetary defense mission under development in the Space Safety and Security Program of the European Space Agency for launch in 2024 October and rendezvous in late 2026 December with the binary asteroid (65803) Didymos and its moon, Dimorphos, which will be impacted by NASA's DART spacecraft on 2022 September 26 as the first asteroid deflection test.
Dissertation
Contraintes sur la structure interne de Mars et mesures de la marée de Phobos pour la mission INSIGHT
TL;DR: In 2018, the INSIGHT mission as discussed by the authors concerne la mission INSIGHT, which doit partir vers Mars en 2018, to determine l'etat du noyau de la planete (liquide ou solide), notamment avec les mesures du sismometre SEIS qui doit mesurer l'amplitude d'une des harmonique principales de la maree de Phobos.
References
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Journal ArticleDOI
The Rubble-Pile Asteroid Itokawa as Observed by Hayabusa
Akira Fujiwara,Jun'ichiro Kawaguchi,D. K. Yeomans,Masanao Abe,Tadashi Mukai,Tatsuaki Okada,Jun Saito,Hajime Yano,Makoto Yoshikawa,Daniel J. Scheeres,Olivier S. Barnouin-Jha,A. F. Cheng,Hirohide Demura,R. W. Gaskell,Naru Hirata,H. Ikeda,T. Kominato,Hirdy Miyamoto,Akiko M. Nakamura,Ryosuke Nakamura,Sho Sasaki,K. Uesugi +21 more
TL;DR: During the interval from September through early December 2005, the Hayabusa spacecraft was in close proximity to near-Earth asteroid Itokawa, and a variety of data were taken on its shape, mass, and surface topography as well as its mineralogic and elemental abundances.
Journal ArticleDOI
Radiative Spin-up and Spin-down of Small Asteroids
TL;DR: The Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect as mentioned in this paper may spin up or spin down 5-km-radius asteroids on a 108-year timescale.
Journal ArticleDOI
Density of asteroids
TL;DR: DeMeo et al. as mentioned in this paper presented a review of the current knowledge of the density of small bodies and compared with meteorite density, allowing to estimate the macroporosity (i.e., amount of voids) within these bodies.
Journal ArticleDOI
Hayabusa2 arrives at the carbonaceous asteroid 162173 Ryugu—A spinning top–shaped rubble pile
Sei-ichiro Watanabe,Sei-ichiro Watanabe,Masatoshi Hirabayashi,Naru Hirata,Na. Hirata,Rina Noguchi,Yuri Shimaki,H. Ikeda,Eri Tatsumi,Makoto Yoshikawa,Makoto Yoshikawa,Shota Kikuchi,Hikaru Yabuta,Tomoki Nakamura,Shogo Tachibana,Shogo Tachibana,Yoshiaki Ishihara,Tomokatsu Morota,Kohei Kitazato,Naoya Sakatani,Koji Matsumoto,Koji Wada,Hiroki Senshu,C. Honda,Tatsuhiro Michikami,Hiroshi Takeuchi,Hiroshi Takeuchi,Toru Kouyama,R. Honda,Shingo Kameda,Tetsuharu Fuse,Hideaki Miyamoto,Goro Komatsu,S. Sugita,Tatsuaki Okada,Tatsuaki Okada,Noriyuki Namiki,Masahiko Arakawa,Masateru Ishiguro,Masanao Abe,Masanao Abe,Robert Gaskell,Eric Palmer,Olivier S. Barnouin,Patrick Michel,A. S. French,Jay W. McMahon,Daniel J. Scheeres,Paul A. Abell,Yukio Yamamoto,Yukio Yamamoto,Satoshi Tanaka,Satoshi Tanaka,Kei Shirai,Moe Matsuoka,Manabu Yamada,Y. Yokota,Y. Yokota,H. Suzuki,Kosuke Yoshioka,Yuichiro Cho,Naoki Nishikawa,T. Sugiyama,Hideaki Kikuchi,Ryodo Hemmi,Tomohiro Yamaguchi,Naoko Ogawa,Go Ono,Yuya Mimasu,Kent Yoshikawa,T. Takahashi,Yuto Takei,Atsushi Fujii,Chikako Hirose,Takahiro Iwata,Takahiro Iwata,Masahiro Hayakawa,Satoshi Hosoda,Osamu Mori,Hirotaka Sawada,Takanobu Shimada,Stefania Soldini,Hajime Yano,Hajime Yano,Ryudo Tsukizaki,M. Ozaki,M. Ozaki,Yuichi Iijima,K. Ogawa,Masaki Fujimoto,T. M. Ho,Aurelie Moussi,Ralf Jaumann,J. P. Bibring,Christian Krause,Fuyuto Terui,Takanao Saiki,Satoru Nakazawa,Yoshiyuki Tsuda,Yoshiyuki Tsuda +99 more
TL;DR: The Hayabusa2 spacecraft measured the mass, size, shape, density, and spin rate of asteroid Ryugu, showing that it is a porous rubble pile, and observations of Ryugu's shape, mass, and geomorphology suggest that Ryugu was reshaped by centrifugally induced deformation during a period of rapid rotation.
Journal ArticleDOI
Fast and Slow Rotation of Asteroids
TL;DR: In this paper, the authors present an analysis of the distribution of asteroid spin rates vs. size, and find that significant populations of both slow and fast rotators among asteroids smaller than D =40 km, and especially below 10 km.