Spins and shapes of basaltic asteroids and the missing mantle problem

被引：7

作者：

Oszkiewicz, Dagmara ^{[1
]}

Troianskyi, Volodymyr ^{[1
,2
,3
]}

Galad, Adrian ^{[4
]}

Hanus, Josef ^{[5
]}

Durech, Josef ^{[5
]}

Wilawer, Emil ^{[1
]}

Marciniak, Anna ^{[1
]}

Kwiatkowski, Tomasz ^{[1
]}

Kolenczuk, Pawel ^{[1
]}

Skiff, Brian A. ^{[6
]}

Polakis, Tom ^{[6
]}

Moskovitz, Nicholas A. ^{[6
]}

Geier, Stefan ^{[7
,8
]}

Fohring, Dora ^{[9
]}

Hung, Denise ^{[9
]}

Gajdos, Stefan ^{[4
]}

Vilagi, Jozef ^{[4
]}

Polcic, L'udovit ^{[4
]}

Kashuba, Volodymyr ^{[6
]}

Udovichenko, Sergei ^{[6
]}

Keir, Leonid ^{[2
,3
]}

Benishek, Vladimir ^{[10
]}

Pray, Donald P. ^{[11
]}

Shevchenko, Vasilij ^{[12
]}

Krugly, Yurij ^{[1
,12
]}

Kankiewicz, Pawel ^{[13
]}

Hasegawa, Sunao ^{[14
]}

Behrend, Raoul ^{[15
]}

Bernasconi, Laurent ^{[16
]}

Leroy, Arnaud ^{[17
]}

Roy, Rene ^{[18
]}

Ivanova, Oleksandra ^{[19
,20
,21
]}

Husarik, Marek ^{[19
]}

Simon, Andrii ^{[22
,23
]}

机构：

[1] Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, Sloneczna 36, PL-60286 Poznan, Poland

[2] Odesa II Mechnykov Natl Univ, FMPIT, Dept Phys & Astron, Pastera St 42, UA-65082 Odesa, Ukraine

[3] Mechnykov Natl Univ, Astron Observ Odesa II, Marazlievskaya 1v, UA-65014 Odesa, Ukraine

[4] FMPI UK, Dept Astron Phys Earth & Meteorol, Modra Observ, SK-84248 Bratislava, Slovakia

[5] Charles Univ Prague, Inst Astron, Fac Math & Phys, V Holesovickaach 2, Prague 18000, Czech Republic

[6] Lowell Observ, 14000 Mars Hill Rd, Flagstaff, AZ 86001 USA

[7] Gran Telescopio Canarias GRANTECAN, Cuesta San Jose s n, E-38712 Palma De Mallorca, Spain

[8] Inst Astrofis Canarias, Via Lactea S-N, E-38200 San Cristobal la Laguna, Spain

[9] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[10] Belgrade Astron Observ, Volgina 7 38, Belgrade 11060, Serbia

[11] Sugarloaf Mt Observ, South Deerfield, MA USA

[12] V N Karazin Kharkiv Natl Univ, Dept Astron & Space Informat, 4 Svobody Sq, UA-61022 Kharkiv, Ukraine

[13] Jan Kochanowski Univ, Inst Phys, Uniwersytecka 7, PL-25406 Kielce, Poland

[14] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3 1 1 Yoshinodai Chuo ku, Sagamihara, Kanagawa 2525210, Japan

[15] Geneva Observ, CH-1290 Versoix, Switzerland

[16] Observ Engarouines, F-84570 Mallemort Du Comtat, France

[17] Assoc T60, 14 Ave Edouard Belin, F-31400 Toulouse, France

[18] Observ Blauvac, 294 Ch St Guillaume, F-84570 Blauvac, France

[19] Slovak Acad Sci, Astron Inst 13, Tatranska Lomnica 05960, Slovakia

[20] Natl Acad Sci, Main Astron Observ, 27 Akad Zabolotnoho St, UA-03143 Kiev, Ukraine

[21] Taras Shevchenko Natl Univ Kyiv, Astron Observ, 3 Observatorna St, UA-04053 Kiev, Ukraine

[22] Taras Shevchenko Natl Univ Kyiv, Astron & Space Phys Dept, Glushkova ave 4, UA-03022 Kiev, Ukraine

[23] Natl Ctr Jr Acad Sci Ukraine, 38 44 Dehtiarivska St, UA-04119 Kiev, Ukraine

来源：

ICARUS | 2023年 / 397卷

关键词：

Asteroids; Rotation; Photometry; V-TYPE ASTEROIDS; NEAR-EARTH ASTEROIDS; SPECTRAL CHARACTERIZATION; LIGHTCURVE INVERSION; OPTIMIZATION METHODS; HED METEORITES; VESTA; YARKOVSKY; HOWARDITE; ORIGIN;

D O I：

10.1016/j.icarus.2023.115520

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Basaltic V-type asteroids are common in the inner part of the Main Asteroid Belt and much less abundant in the mid and outer parts. They are of scientific interest because they sample crusts and mantles of theoretically plentiful differentiated planetesimals that existed in the Solar System four billion years ago. Some Solar System theories suggest that those objects formed in the terrestrial planet region and were then implanted in the main asteroid belt. In consequence, we should observe a large number of fragments of multiple differentiated planetesimals in the inner Main Belt. That region of the Asteroid Belt is filled with V-type fragments; however, they are difficult to tell apart from typical Vestoids and Vesta fugitives. In this work, we focus on physical and dynamical characterization of V-types in the inner Main-Belt and aim to reconcile those properties with the planetesimal formation and evolution theories. We conducted an observing campaign over the years 2013-2022 and obtained photometric observations of V-type asteroids located mostly outside the Vesta family at specific locations of the inner Main Belt (the so-called Cells I and II). The total number of partial dense photometric lightcurves obtained in this study was similar to 2910. We were able to model similar to 100 V-types. We further supplement those data with 133 spins of V-types from the DAMIT database and 237 objects derived from Gaia DR3 (Durech & Hanus 2023). We found 78%+/- 11% and 38%+/- 13% retrograde rotators in Cell I and II, respectively. This statistic is remarkably consistent with the numerical simulations of the escape paths of Vesta fugitives that predict 81% retrograde rotators in Cell I and 40% in Cell II after the dynamical integration of 2 Gys. Based on our statistics we conclude that if there are non-Vestoids in the inner main belt, they are likely to be very few. This is consistent with the small fraction of anomalous HED meteorites in meteorite collections, small number of non-Vestoids in the middle and outer Main Belt and points to planetesimal formation location close to the Sun.

引用

页数：12

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