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Journal ArticleDOI

In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model

TL;DR: In this paper, the authors used a suite of numerical simulations to determine the ages of the families above, how Bennu reached its current orbit, and the most probable source family for Bennu.
About: This article is published in Icarus.The article was published on 2015-02-01. It has received 144 citations till now. The article focuses on the topics: Asteroid family & Asteroid.
Citations
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Journal ArticleDOI
TL;DR: The OSIRIS-REx spacecraft departed for near-Earth asteroid (101955) Bennu via an United Launch Alliance Atlas V 411 evolved expendable launch vehicle at 7:05 p.m. EDT on September 8, 2016, on a seven-year journey to return samples from Bennu as discussed by the authors.
Abstract: In May of 2011, NASA selected the Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer (OSIRIS-REx) asteroid sample return mission as the third mission in the New Frontiers program. The other two New Frontiers missions are New Horizons, which explored Pluto during a flyby in July 2015 and is on its way for a flyby of Kuiper Belt object 2014 MU69 on January 1, 2019, and Juno, an orbiting mission that is studying the origin, evolution, and internal structure of Jupiter. The spacecraft departed for near-Earth asteroid (101955) Bennu aboard an United Launch Alliance Atlas V 411 evolved expendable launch vehicle at 7:05 p.m. EDT on September 8, 2016, on a seven-year journey to return samples from Bennu. The spacecraft is on an outbound-cruise trajectory that will result in a rendezvous with Bennu in November 2018. The science instruments on the spacecraft will survey Bennu to measure its physical, geological, and chemical properties, and the team will use these data to select a site on the surface to collect at least 60 g of asteroid regolith. The team will also analyze the remote-sensing data to perform a detailed study of the sample site for context, assess Bennu’s resource potential, refine estimates of its impact probability with Earth, and provide ground-truth data for the extensive astronomical data set collected on this asteroid. The spacecraft will leave Bennu in 2021 and return the sample to the Utah Test and Training Range (UTTR) on September 24, 2023.

440 citations

Journal ArticleDOI
Seiji Sugita1, Seiji Sugita2, Rie Honda3, Tomokatsu Morota4, Shingo Kameda5, Hirotaka Sawada6, Eri Tatsumi1, Manabu Yamada2, C. Honda7, Yasuhiro Yokota3, Yasuhiro Yokota6, Toru Kouyama8, Naoya Sakatani6, K. Ogawa9, H. Suzuki10, Tatsuaki Okada1, Tatsuaki Okada6, Noriyuki Namiki11, Satoshi Tanaka6, Satoshi Tanaka11, Yuichi Iijima6, Kosuke Yoshioka1, Masahiro Hayakawa6, Yuichiro Cho1, Moe Matsuoka6, Naru Hirata7, Hideaki Miyamoto1, Deborah L. Domingue12, Masatoshi Hirabayashi13, Tomoki Nakamura14, Takahiro Hiroi15, Tatsuhiro Michikami16, Patrick Michel17, Ronald-Louis Ballouz18, Ronald-Louis Ballouz6, Olivier S. Barnouin19, Carolyn M. Ernst19, Stefan Schröder20, Hideaki Kikuchi1, Ryodo Hemmi1, Goro Komatsu2, Goro Komatsu12, T. Fukuhara5, Makoto Taguchi5, Takehiko Arai, Hiroki Senshu2, Hirohide Demura7, Yoshiko Ogawa7, Yuri Shimaki6, Tomohiko Sekiguchi21, T. G. Müller22, Axel Hagermann23, Takahide Mizuno6, Hirotomo Noda, Koji Matsumoto11, R. Yamada7, Yoshiaki Ishihara6, H. Ikeda, Hiroshi Araki, K. Yamamoto, Shinsuke Abe24, Fumi Yoshida2, A. Higuchi, Sho Sasaki25, S. Oshigami, Seiitsu Tsuruta, Kazuyoshi Asari, Seiichi Tazawa, M. Shizugami, J. Kimura25, Toshimichi Otsubo26, Hikaru Yabuta27, Sunao Hasegawa6, Masateru Ishiguro28, Shogo Tachibana1, Eric Palmer12, Robert Gaskell12, L. Le Corre12, Ralf Jaumann20, Katharina A. Otto20, Nicole Schmitz20, Paul A. Abell, M. A. Barucci29, Michael E. Zolensky, Faith Vilas12, Florian Thuillet17, C. Sugimoto1, N. Takaki1, Yutaka Suzuki1, Hiroaki Kamiyoshihara1, Masato Okada1, Kenji Nagata8, Masaki Fujimoto6, Makoto Yoshikawa6, Makoto Yoshikawa11, Yukio Yamamoto11, Yukio Yamamoto6, Kei Shirai6, Rina Noguchi6, Naoko Ogawa6, Fuyuto Terui6, Shota Kikuchi6, Tomohiro Yamaguchi6, Yusuke Oki1, Yuki Takao1, Hiroshi Takeuchi6, Go Ono, Yuya Mimasu6, Kent Yoshikawa, T. Takahashi6, Yuto Takei6, Atsushi Fujii6, Chikako Hirose, Satoru Nakazawa6, Satoshi Hosoda6, Osamu Mori6, Takanobu Shimada6, Stefania Soldini6, Takahiro Iwata11, Takahiro Iwata6, Masanao Abe6, Masanao Abe11, Hajime Yano6, Hajime Yano11, Ryudo Tsukizaki6, M. Ozaki6, M. Ozaki11, Kazutaka Nishiyama6, Takanao Saiki6, Sei-ichiro Watanabe6, Sei-ichiro Watanabe4, Yoshiyuki Tsuda11, Yoshiyuki Tsuda6 
19 Apr 2019-Science
TL;DR: Spectral observations and a principal components analysis suggest that Ryugu originates from the Eulalia or Polana asteroid family in the inner main belt, possibly via more than one generation of parent bodies.
Abstract: Additional co-authors: N Namiki, S Tanaka, Y Iijima, K Yoshioka, M Hayakawa, Y Cho, M Matsuoka, N Hirata, N Hirata, H Miyamoto, D Domingue, M Hirabayashi, T Nakamura, T Hiroi, T Michikami, P Michel, R-L Ballouz, O S Barnouin, C M Ernst, S E Schroder, H Kikuchi, R Hemmi, G Komatsu, T Fukuhara, M Taguchi, T Arai, H Senshu, H Demura, Y Ogawa, Y Shimaki, T Sekiguchi, T G Muller, T Mizuno, H Noda, K Matsumoto, R Yamada, Y Ishihara, H Ikeda, H Araki, K Yamamoto, S Abe, F Yoshida, A Higuchi, S Sasaki, S Oshigami, S Tsuruta, K Asari, S Tazawa, M Shizugami, J Kimura, T Otsubo, H Yabuta, S Hasegawa, M Ishiguro, S Tachibana, E Palmer, R Gaskell, L Le Corre, R Jaumann, K Otto, N Schmitz, P A Abell, M A Barucci, M E Zolensky, F Vilas, F Thuillet, C Sugimoto, N Takaki, Y Suzuki, H Kamiyoshihara, M Okada, K Nagata, M Fujimoto, M Yoshikawa, Y Yamamoto, K Shirai, R Noguchi, N Ogawa, F Terui, S Kikuchi, T Yamaguchi, Y Oki, Y Takao, H Takeuchi, G Ono, Y Mimasu, K Yoshikawa, T Takahashi, Y Takei, A Fujii, C Hirose, S Nakazawa, S Hosoda, O Mori, T Shimada, S Soldini, T Iwata, M Abe, H Yano, R Tsukizaki, M Ozaki, K Nishiyama, T Saiki, S Watanabe, Y Tsuda

325 citations


Cites background from "In search of the source of asteroid..."

  • ...considered for different scales of surface ages because Ryugu is estimated to have migrated from the main belt to the near-Erth orbit most likely through ν6, the inner most resonance zone of the main belt (9, 15)....

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  • ...Their populations in the inner main belt, from which the largest fraction of near-Earth asteroids is derived (2), contain many large families, such as the Eulalia and Polana families, with these spectral characteristics (23)....

    [...]

  • ...The collisional lifetime of Ryugu [(3 to 5) × 108 years] is similar to or less than the breakup time of these families [830þ370 150 million years and 1400 ± 150million years for Eulalia and Polana, respectively (15)]....

    [...]

  • ...The collisional lifetime of Ryugu (3 – 5 × 10(8) yr) is similar to or less than the breakup time of these families (830!!"# !!"# My and 1400 ± 150 Myr for Eulalia and Polana, respectively (15))....

    [...]

  • ...Orbital dynamics calculations have shown that the most likely origin of Ryugu is either Eulalia or Polana (15)....

    [...]

Journal ArticleDOI
TL;DR: The Hayabusa2 mission as mentioned in this paper was the first mission to explore a C-type near-Earth asteroid (162173) Ryugu (1999 JU3) to observe and explore the 900 m-sized object, and return samples collected from the surface layer.
Abstract: The Hayabusa2 mission journeys to C-type near-Earth asteroid (162173) Ryugu (1999 JU3) to observe and explore the 900 m-sized object, as well as return samples collected from the surface layer. The Haybusa2 spacecraft developed by Japan Aerospace Exploration Agency (JAXA) was successfully launched on December 3, 2014 by an H-IIA launch vehicle and performed an Earth swing-by on December 3, 2015 to set it on a course toward its target Ryugu. Hayabusa2 aims at increasing our knowledge of the early history and transfer processes of the solar system through deciphering memories recorded on Ryugu, especially about the origin of water and organic materials transferred to the Earth’s region. Hayabusa2 carries four remote-sensing instruments, a telescopic optical camera with seven colors (ONC-T), a laser altimeter (LIDAR), a near-infrared spectrometer covering the 3-μm absorption band (NIRS3), and a thermal infrared imager (TIR). It also has three small rovers of MINERVA-II and a small lander MASCOT (Mobile Asteroid Surface Scout) developed by German Aerospace Center (DLR) in cooperation with French space agency CNES. MASCOT has a wide angle imager (MasCam), a 6-band thermal radiator (MARA), a 3-axis magnetometer (MasMag), and a hyperspectral infrared microscope (MicrOmega). Further, Hayabusa2 has a sampling device (SMP), and impact experiment devices which consist of a small carry-on impactor (SCI) and a deployable camera (DCAM3). The interdisciplinary research using the data from these onboard and lander’s instruments and the analyses of returned samples are the key to success of the mission.

210 citations

Journal ArticleDOI
15 Sep 2018-Icarus
TL;DR: In this article, the authors presented a new four-dimensional model of the near-Earth objects population that describes debiased steady-state distributions of semimajor axis, eccentricity, inclination, and absolute magnitude H in the range 17.962 − 56 + 52 + 52 ( 802 − 42 + 48 × 10 3 ) NEOs with H.

171 citations

Journal ArticleDOI
01 Sep 2015-Icarus
TL;DR: In this paper, a catalog of proper elements with ∼384,000 numbered asteroids and on new methods is available, including a least squares fit of the two sides of a V-shape plot in the proper semimajor axis, inverse diameter plane to determine the corresponding slopes, an advanced error model for the uncertainties of asteroid diameters, an iterative outlier rejection scheme and quality control.

145 citations


Additional excerpts

  • ..., 2006b) give an age of 280± 112 My, which is higher but consistent; (Bottke et al., 2015) by a different method give an age 170 −30, which is lower but consistent with the IN side....

    [...]

  • ...(Vokrouhlický et al., 2006b) give an age of 280± 112 My, which is higher but consistent; (Bottke et al., 2015) by a different method give an age 170+25 −30, which is lower but consistent with the IN side....

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References
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Journal ArticleDOI
30 Aug 2007-Nature
TL;DR: It is reported that boulders can undergo efficient gravitational collapse in locally overdense regions in the midplane of the disk, and it is found that gravitationally bound clusters form with masses comparable to dwarf planets and containing a distribution of boulder sizes.
Abstract: During the initial stages of planet formation in circumstellar gas disks, dust grains collide and build up larger and larger bodies. How this process continues from metre-sized boulders to kilometre-scale planetesimals is a major unsolved problem: boulders are expected to stick together poorly, and to spiral into the protostar in a few hundred orbits owing to a 'headwind' from the slower rotating gas. Gravitational collapse of the solid component has been suggested to overcome this barrier. But even low levels of turbulence will inhibit sedimentation of solids to a sufficiently dense midplane layer, and turbulence must be present to explain observed gas accretion in protostellar disks. Here we report that boulders can undergo efficient gravitational collapse in locally overdense regions in the midplane of the disk. The boulders concentrate initially in transient high pressure regions in the turbulent gas, and these concentrations are augmented a further order of magnitude by a streaming instability driven by the relative flow of gas and solids. We find that gravitationally bound clusters form with masses comparable to dwarf planets and containing a distribution of boulder sizes. Gravitational collapse happens much faster than radial drift, offering a possible path to planetesimal formation in accreting circumstellar disks.

1,238 citations

Journal ArticleDOI
14 Jul 2011-Nature
TL;DR: Simulation of the early Solar System shows how the inward migration of Jupiter to 1.5 au, and its subsequent outward migration, lead to a planetesimal disk truncated at 1’au; the terrestrial planets then form from this disk over the next 30–50 million years, with an Earth/Mars mass ratio consistent with observations.
Abstract: Jupiter and Saturn formed in a few million years from a gas-dominated protoplanetary disk, and were susceptible to gas-driven migration of their orbits on timescales of only approximately 100,000 years. Hydrodynamic simulations show that these giant planets can undergo a two-stage, inward-then-outward, migration. The terrestrial planets finished accreting much later and their characteristics, including Mars' small mass, are best reproduced by starting from a planetesimal disk with an outer edge at about one astronomical unit from the Sun (1 AU is the Earth-Sun distance). Here we report simulations of the early Solar System that show how the inward migration of Jupiter to 1.5 AU, and its subsequent outward migration, lead to a planetesimal disk truncated at 1 AU; the terrestrial planets then form from this disk over the next 30-50 million years, with an Earth/Mars mass ratio consistent with observations. Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspect missing from previous models of terrestrial planet formation is the substantial radial migration of the giant planets, which suggests that their behaviour is more similar to that inferred for extrasolar planets than previously thought.

1,174 citations


"In search of the source of asteroid..." refers background in this paper

  • ...For example, it is likely that Bennu’s parent body spent most of its life in the main asteroid belt, but we cannot yet say whether it was indigenous to the main belt region (e.g., Bottke et al., 2006b; Bottke and Asphaug, 2013; Levison et al., 2009; Walsh et al., 2011)....

    [...]

  • ...The formation location could have been the main asteroid belt, but it may also have been another region altogether (e.g., the outer Solar System beyond Jupiter; Levison et al., 2009; Walsh et al., 2011; Bottke et al., 2006b; Bottke and Asphaug, 2013)....

    [...]

Journal ArticleDOI
01 Mar 1994-Icarus
TL;DR: In this paper, the authors developed and tested a new computer code to follow the long-term dynamical evolution of a swarm of test particles in the solar system and found that the Tisserand parameter, T, does not vary substantially for most comets.

851 citations


"In search of the source of asteroid..." refers methods in this paper

  • ...Using these test bodies, we employed the symplectic N-body code SWIFT-RMVS3 (e.g., Levison and Duncan, 1994), modified to accommodate Yarkovsky thermal forces (e.g., Vokrouhlický and Nesvorný, 2008), to track the evolution of test asteroids either entering into the m6 and J3:1 resonances or…...

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Journal ArticleDOI
01 Apr 2002-Icarus
TL;DR: In this article, a best-fit model of the near-Earth objects (NEOs) population is presented, which is fit to known NEs discovered or accidentally rediscovered by Spacewatch.

717 citations

30 Jun 1993
TL;DR: In this article, it is shown that the anomalous concentration of the argument of perihelion of the Jupiter-family comets near 0 and 180 deg is a direct result of their aphelion distance being close to 5.2AU and the comet being recently perturbed onto a Jupiter- family orbit.
Abstract: The orbits of the known short-period comets under the influence of the Sun and all the planets except Mercury and Pluto are numerically integrated. The calculation was undertaken in order to determine the dynamical lifetimes for these objects as well as explaining the current orbital element distribution. It is found that a comet can move between Jupiter-family and Halley-family comets several times in its dynamical lifetime. The median lifetime of the known short-period comets from the time they are first injected into a short-period comet orbit to ultimate ejection is approximately 50,000 years. The very flat inclination distribution of Jupiter-family comets is observed to become more distended as it ages. The only possible explanation for the observed flat distribution is that the comets become extinct before their inclination distribution can change significantly. It is shown that the anomalous concentration of the argument of perihelion of Jupiter-family comets near 0 and 180 deg is a direct result of their aphelion distance being close to 5.2AU and the comet being recently perturbed onto a Jupiter-family orbit. Also the concentration of their aphelion near Jupiter's orbit is a result of the conservation of the Tisserand invariant during the capture process.

677 citations