Spin states of asteroids in the Eos collisional family

Hanuš, Josef; Delbò, M.; Alí-Lagoa, V.; Bolin, Bryce; Jedicke, Robert; Ďurech, Josef; Cibulková, H.; Pravec, Petr; Kušnirák, P.; Behrend, R.; Marchis, Franck; Antonini, P.; Arnold, L.; Audejean, M.; Bachschmidt, M.; Bernasconi, L.; Brunetto, L.; Casulli, Silvano; Dymock, R.; Esseiva, N.; Esteban, M.; Gerteis, O.; Groot, Hugo de; Gully, H.; Hamanowa, Hiroko; Hamanowa, Hiromi; Krafft, P.; Lehký, M.; Manzini, F.; Michelet, J.; Morelle, Etienne; Oey, Julian; Pilcher, Frederick; Reignier, F.; Roy, R.; Salom, P.; Warner, Brian D.

doi:10.1016/j.icarus.2017.07.007

Cited by 31 publications

(20 citation statements)

References 77 publications

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“…We made use of the TPM implementation by Delbó et al (2007a) based on the previous development of Lagerros (1996). In our work, we followed the procedure of Hanuš et al (2015Hanuš et al ( , 2018. The detailed description can be found in the aforementioned papers.…”

Section: Appendixmentioning

confidence: 99%

Asteroid pairs: A complex picture

Pravec

Fatka

Vokrouhlický

et al. 2019

Icarus

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We studied a sample of 93 asteroid pairs, i.e., pairs of genetically related asteroids that are on highly similar heliocentric orbits. We estimated times elapsed since separation of pair members (i.e., pair age) that are between 7 × 10 3 yr and a few 10 6 yr. With photometric observations, we derived the rotation periods P 1 for all the primaries (i.e., the larger members of asteroid pairs) and a sample of secondaries (the smaller pair members). We derived the absolute magnitude differences of the studied asteroid pairs that provide their mass ratios q. For a part of the studied pairs, we refined their WISE geometric albedos and collected or estimated their taxonomic classifications. For 17 asteroid pairs, we also determined their pole positions. In two pairs where we obtained the spin poles for both pair components, we saw the same sense of rotation for both components and constrained the angles between their original spin vectors at the time of their separation. We found that the primaries of 13 asteroid pairs in our sample are actually binary or triple systems, i.e., they have one or two bound, orbiting secondaries (satellites). As a by-product, we found also 3 new young asteroid clusters (each of them consisting of three known asteroids on highly similar heliocentric orbits). We compared the obtained asteroid pair data with theoretical predictions and discussed their implications. We found that 86 of the 93 studied asteroid pairs follow the trend of primary rotation period vs mass ratio that was found by Pravec et al. (2010). Of the 7 outliers, 3 appear insignificant (may be due to our uncertain or incomplete knowledge of the three pairs), but 4 are high mass ratio pairs that were unpredicted by the theory of asteroid pair formation by rotational fission. We discuss a (remotely) possible way that they could be created by rotational fission of flattened parent bodies followed by re-shaping of the formed components. The 13 asteroid pairs with binary primaries are particularly interesting systems that place important constraints on formation and evolution of asteroid pairs. We present two hypotheses for their formation: The asteroid pairs having both bound and unbound secondaries could be "failed asteroid clusters", or they could be formed by a cascade primary spin fission process. Further studies are needed to reveal which of these two hypotheses for formation of the paired binary systems is real.

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Section: Appendixmentioning

confidence: 99%

Asteroid pairs: A complex picture

Pravec

Fatka

Vokrouhlický

et al. 2019

Icarus

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“…423 Diotima Follow-up observations in 1-2.5 µm were performed by Hasegawa et al (2017), and this object was classified as C-type according to the Bus-DeMeo taxonomy. This object is a member of the Eos collisional family (D. Nesvorny 2012 5 , not in D. Nesvorny 2015 4 ), but is likely to be an interloper based on a spin state analysis (Hanuš et al 2018). Jones et al (1990) conducted 3-µm band observations with IRTF and detected no signal associated with hydrated minerals and/or water ice.…”

Section: Eunikementioning

confidence: 99%

AKARI/IRC near-infrared asteroid spectroscopic survey: AcuA-spec

Usui

Hasegawa

Ootsubo

et al. 2018

Publications of the Astronomical Society of Japan

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Knowledge of water in the solar system is important for understanding of a wide range of evolutionary processes and the thermal history of the solar system. To explore the existence of water in the solar system, it is indispensable to investigate hydrated minerals and/or water ice on asteroids. These water-related materials show absorption features in the 3-µm band (wavelengths from 2.7 to 3.1 µm). We conducted a spectroscopic survey of asteroids in the 3-µm band using the Infrared Camera (IRC) on board the Japanese infrared satellite AKARI. In the warm mission period of AKARI, 147 pointed observations were performed for 66 asteroids in the grism mode for wavelengths from 2.5 to 5 µm. According to these observations, most C-complex asteroids have clear absorption features (> 10% with respect to the continuum) related to hydrated minerals at a peak wavelength of approximately 2.75 µm, while S-complex asteroids have no significant feature in this wavelength range. The present data are released to the public as the Asteroid Catalog using AKARI Spectroscopic Observations (AcuA-spec).

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“…It should also be noted that models based on sparse data provide reliable spin parameters, but only low-resolution, coarse shape representations (flag '1' or '2' in the shape quality system proposed by Hanuš et al 2018a), limiting their use in other applications . For example, detailed thermophysical modelling needs rather high-resolution (flag '3') shape models as input, only possible with large datasets of dense lightcurves obtained at various viewing geometries.…”

Section: Introductionmentioning

confidence: 99%

Thermal properties of slowly rotating asteroids: results from a targeted survey

Marciniak

Alí-Lagoa

Müller

et al. 2019

A&A

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Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the sub-surface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 hours, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3 +33 −3 and 45 +60 −30 J m −2 s −1/2 K −1 . Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.

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Spin states of asteroids in the Eos collisional family

Cited by 31 publications

References 77 publications

Asteroid pairs: A complex picture

Asteroid pairs: A complex picture

AKARI/IRC near-infrared asteroid spectroscopic survey: AcuA-spec

Thermal properties of slowly rotating asteroids: results from a targeted survey

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