Interplanetary Dust Particles as Samples of Icy Asteroids

Vernazza, Pierre; Marsset, Michaël; Beck, Pierre; Binzel, Richard P.; Birlan, Mirel; Brunetto, R.; DeMeo, Francesca E.; Djouadi, Z.; Dumas, Christophe; Merouane, S.; Mousis, O.; Zanda, B.

doi:10.1088/0004-637x/806/2/204

Cited by 102 publications

(168 citation statements)

References 60 publications

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“…The B/C-complex groupThis group includes four asteroids classified as B-types, four as C-, six as Cg-, one as Cgh-, and one low albedo Xc-type. They show spectral similarities with carbonaceous chondrite meteorites (e.g.Cloutis et al 2011a,b;de León et al 2012) and with interplanetary dust particles(Vernazza et al 2015;Marsset et al 2016).The albedos are available for five of these objects, and their low values (p V ≤ 0.1) are compatible with their taxonomic classification. The diameters of the NEAs belonging to this sample range from 0.4 to 5.5 km.…”

mentioning

confidence: 67%

Near-Earth asteroids spectroscopic survey atIsaac NewtonTelescope

Popescu

Văduvescu

León

et al. 2019

A&A

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Context. The population of near-Earth asteroids (NEAs) shows a large variety of objects in terms of physical and dynamical properties. They are subject to planetary encounters and to strong solar wind and radiation effects. Their study is also motivated by practical reasons regarding space exploration and long-term probability of impact with the Earth. Aims. We aim to spectrally characterize a significant sample of NEAs with sizes in the range of ∼0.25 -5.5 km (categorized as large), and search for connections between their spectral types and the orbital parameters. Methods. Optical spectra of NEAs were obtained using the Isaac Newton Telescope (INT) equipped with the IDS spectrograph. These observations are analyzed using taxonomic classification and by comparison with laboratory spectra of meteorites. Results. A total number of 76 NEAs were observed. We spectrally classified 44 of them as Q/S-complex, 16 as B/C-complex, eight as V-types, and another eight belong to the remaining taxonomic classes. Our sample contains 27 asteroids categorized as potentially hazardous and 31 possible targets for space missions including (459872) 2014 EK24, (436724) 2011 UW158, and (67367) 2000 LY27. The spectral data corresponding to (276049) 2002 CE26 and (385186) 1994 AW1 shows the 0.7 µm feature which indicates the presence of hydrated minerals on their surface. We report that Q-types have the lowest perihelia (a median value and absolute deviation of 0.797 ± 0.244 AU) and are systematically larger than the S-type asteroids observed in our sample. We explain these observational evidences by thermal fatigue fragmentation as the main process for the rejuvenation of NEA surfaces. Conclusions. In general terms, the taxonomic distribution of our sample is similar to the previous studies and matches the broad groups of the inner main belt asteroids. Nevertheless, we found a wide diversity of spectra compared to the standard taxonomic types.

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mentioning

confidence: 67%

Near-Earth asteroids spectroscopic survey atIsaac NewtonTelescope

Popescu

Văduvescu

León

et al. 2019

A&A

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“…It was classified in the B-spectral class following the Bus taxonomy based on visible data alone, whereas it is labeled a C-type in the Bus-DeMeo taxonomy (Clark et al 2010). In the visible and near-infrared spectral range, it thus appears similar to objects such as (1) Ceres, (10) Hygiea, (24) Themis, and (52) Europa, which have been connected to interplanetary dust particles (IDPs) rather than to carbonaceous chondrites (Vernazza et al 2015(Vernazza et al , 2017Marsset et al 2016). Interamnia is also of great interest to the present study, being the largest asteroid for which a detailed shape model (convex or with local topography) and consistent spin-state solutions do not yet exist.…”

Section: Introductionmentioning

confidence: 86%

(704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

Hanuš

Vernazza

Viikinkoski

et al. 2020

A&A

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Context. With an estimated diameter in the 320 to 350 km range, (704) Interamnia is the fifth largest main belt asteroid and one of the few bodies that fills the gap in size between the four largest bodies with D > 400 km (Ceres, Vesta, Pallas and Hygiea) and the numerous smaller bodies with diameter ≤200 km. However, despite its large size, little is known about the shape and spin state of Interamnia and, therefore, about its bulk composition and past collisional evolution. Aims. We aimed to test at what size and mass the shape of a small body departs from a nearly ellipsoidal equilibrium shape (as observed in the case of the four largest asteroids) to an irregular shape as routinely observed in the case of smaller (D ≤200 km) bodies. Methods. We observed Interamnia as part of our ESO VLT/SPHERE large program (ID: 199.C-0074) at thirteen different epochs. In addition, several new optical lightcurves were recorded. These data, along with stellar occultation data from the literature, were fed to the All-Data Asteroid Modeling (ADAM) algorithm to reconstruct the 3D-shape model of Interamnia and to determine its spin state. Results. Interamnia's volume-equivalent diameter of 332 ± 6 km implies a bulk density of ρ=1.98 ± 0.68 g · cm −3 , which suggests that Interamnia -like Ceres and Hygiea -contains a high fraction of water ice, consistent with the paucity of apparent craters. Our observations reveal a shape that can be well approximated by an ellipsoid, and that is compatible with a fluid hydrostatic equilibrium at the 2 σ level. Conclusions. The rather regular shape of Interamnia implies that the size/mass limit, under which the shapes of minor bodies with a high amount of water ice in the subsurface become irregular, has to be searched among smaller (D ≤300km) less massive (m ≤3x10 19 kg) bodies.

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“…The major reason why interpretation of these asteroids is difficult is that there are few spectral counterparts of meteorites found to X-or D-complex asteroids (c.f., Kanno et al 2003;Hiroi & Hasegawa 2003). Nevertheless, it can be considered that low-albedo Xcomplex (i.e., P-type) and D-complex asteroids may possess properties similar to C-complex in the sense of primitive objects (e.g., Vernazza et al 2015). Thus it is natural that some of these asteroids have signatures of hydration as seen in some stages of C-complex asteroids as the 2.7-µm band feature in this study (e.g., 56 Melete, 476 Hedwig, and 308 Polyxo).…”

Section: From Dry To Wet: Characteristics Of Hydrated Asteroidsmentioning

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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Interplanetary Dust Particles as Samples of Icy Asteroids

Cited by 102 publications

References 60 publications

Near-Earth asteroids spectroscopic survey atIsaac NewtonTelescope

Near-Earth asteroids spectroscopic survey atIsaac NewtonTelescope

(704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

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

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