Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations

Marchis, Franck; Enriquez, J. E.; Emery, Joshua P.; Mueller, Michael; Baek, M.; Pollock, J. T.; Assafin, M.; Martins, R. Vieira; Berthier, J.; Vachier, F.; Cruikshank, D. P.; Lim, L. F.; Reichart, D.; Ivarsen, K.; Haislip, J.; Lacluyzé, A.

doi:10.1016/j.icarus.2012.09.013

Cited by 65 publications

(87 citation statements)

References 95 publications

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“…We apply the mass derived by Fang et al (2011) of 917:5 AE 2:2 Â 10 10 kg and find Alpha's density to be 1:1 AE 0:2 g=cm 3 . Marchis et al (2012) determine that the bulk density for C-complex binary asteroids to range from 0.7 to 1.7 g/cm 3 , supporting the spectral analysis that 2001 SN 263 is a C-complex asteroid. Reddy et al (2008) suggest that the meteorite analog for the asteroid is a CV3.…”

Section: Shape and Size Of 2001 Sn 263 Alphasupporting

confidence: 60%

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Becker

Howell

Nolan

et al. 2015

Icarus

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a b s t r a c tWe report radar observations (2380-MHz, 13-cm) by the Arecibo Observatory and optical light curves observed from eight different observatories and collected at the Ondřejov Observatory of the triple near-Earth asteroid system (153591) 2001 SN 263 . The radar observations were obtained over the course of ten nights spanning February 12-26, 2008 and the light curve observations were made throughout January 12 -March 31, 2008. Both data sets include observations during the object's close approach of 0.06558 AU on February 20th, 2008. The delay-Doppler images revealed the asteroid to be comprised of three components, making it the first known triple near-Earth asteroid. Only one other object, (136617) 1994 CC is a confirmed triple near-Earth asteroid.We present physical models of the three components of the asteroid system. We constrain the primary's pole direction to an ecliptic longitude and latitude of ð309 ; À80 Þ AE 15 . We find that the primary rotates with a period 3:4256 AE 0:0002 h and that the larger satellite has a rotation period of 13:43 AE 0:01 h, considerably shorter than its orbital period of approximately 6 days. We find that the rotation period of the smaller satellite is consistent with a tidally locked state and therefore rotates with a period of 0:686 AE 0:002 days (Fang et al. [2011]. Astron. J. 141, 154-168). The primary, the larger satellite, and the smaller satellite have equivalent diameters of 2:5 AE 0:3 km, 0:77 AE 0:12 km, 0:43 AE 0:14 km and densities of 1:1 AE 0:2 g=cm 3 ; 1:0 AE 0:4 g=cm 3 ; 2:3 AE 1:3 g=cm 3 , respectively.

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Section: Shape and Size Of 2001 Sn 263 Alphasupporting

confidence: 60%

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Becker

Howell

Nolan

et al. 2015

Icarus

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“…The study of these multiple asteroids is an opportunity for planetary astronomers to obtain insights on the asteroids such as their masses and densities and how these quantities possibly relate to their compositions, see e.g. Marchis et al 2012a. Their existence and the understanding of their formation and evolution also provide a direct window to the history of our solar system.…”

Section: Keywordmentioning

confidence: 99%

“…We chose one of these solutions ("sol 4" in Table 2 of Vachier et al (2012) for the schematic in Fig. 8 and the new size estimate of the components based on Spitzer/IRS observations (Marchis et. al 2012a) combined with Polishook et al (2011) photometric survey.…”

Section: Comparison With Other Main-belt Triple Asteroid Systemsmentioning

confidence: 99%

“…Expanding the spectroscopic study to mid-infrared and eventually UV will be useful in characterizing the surface properties of (93) Minerva through comparison with meteorite lab sample spectra. The detection of emission features in the mid-infrared spectra of numerous large and binary asteroids by Marchis et al, (2012a) constrained the nature of asteroid surfaces (e.g. Vernazza et al, 2012).…”

Section: Summary Of Findings and Future Workmentioning

confidence: 99%

“…Table 5: Orbital parameters (a semi-major axis, P period, e eccentricity) and physical characteristics (R p radius of the primary, R s radius of the satellite, R Hill radius of the Hill sphere) of the known triple asteroid systems located in the main-belt. The size of Balam components was derived from Spitzer/IRS observations in Marchis et al (2012a). The processed frame taken at 13:45 UT was recorded using the Kcont filter centered at λ c = 2.2706 µm.…”

Section: Summary Of Findings and Future Workmentioning

confidence: 99%

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Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva

Marchis¹,

Vachier²,

Ďurech³

et al. 2013

Icarus

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Abstract:From a set of adaptive optics (AO) observations collected with the W.M. Keck telescope between August and September 2009, we derived the orbital parameters of the most recently discovered satellites of the large C-type asteroid (93) Minerva. The satellites of Minerva, which are approximately 3 and 4 km in diameter, orbit very close to the primary (~5 & ~8 × R p and ~1% & ~2% × R Hill ) in a circular manner, sharing common characteristics with most of the triple asteroid systems in the main-belt. Combining these AO observations with lightcurve data collected since 1980 and two stellar occultations in 2010 & 2011, we removed the ambiguity of the pole solution of Minerva's primary and showed that it has an almost regular shape with an equivalent diameter D eq = 154 ± 6 km in agreement with IRAS observations. The surprisingly high bulk density of 1.75 ± 0.30 g/cm 3 for this C-type asteroid, suggests that this taxonomic class is composed of asteroids with different compositions, For instance, Minerva could be made of the same material as dry CR, CO, and CV meteorites. We discuss possible scenarios on the origin of the system and conclude that future observations may shine light on the nature and composition of this fifth known triple main-belt asteroid. Keyword:Asteroids -Satellites of asteroids -Adaptive optics -Photometry -Orbit determination -Interior 1 Introduction The serendipitous discovery of Dactyl, a companion of the main-belt asteroid (243) Ida, seen during the Galileo spacecraft voyage to Jupiter (Chapman et al. 1995), gave birth to a new field of study for small solar system bodies. Today, using techniques such as high angular resolution imaging with the Hubble Space Telescope (HST), adaptive optics (AO) on ground-based telescopes, radar observations and photometric studies, about 200 multiple asteroids (asteroids with one or several moons) are known in all populations of small solar system bodies, from the Near-Earth Asteroids to the Kuiper Belt Objects. The study of these multiple asteroids is an opportunity for planetary astronomers to obtain insights on the asteroids such as their masses and densities and how these quantities possibly relate to their compositions, see e.g. Marchis et al. 2012a. Their existence and the understanding of their formation and evolution also provide a direct window to the history of our solar system. In this work, we describe a study of one of these recently discovered triple asteroid systems. (93) Minerva is a large (H v = 7.7, P spin = 5.97909 hours in Tungalag 2002) asteroid discovered by J.C. Watson at Ann Arbor, MI, USA in 1867. Located in the middle of the main-belt (a Minerva = 2.75 AU, e Minerva = 0.14, i Minerva = 9 deg), it was initially classified as a member of an old collisional family (1.2 ± 0.4 Gyrs) named "Gefion" consisting of 973 members based on Nesvorny et al. (2005). Because most of the members of this family are identified as S-type, and (93) Minerva is known to be a C b -type (Lazarro et al. 2004) Ryan & Woodward, 2010). There is a clear ...

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The hierarchical stability of the seven known large size ratio triple asteroids using the empirical stability parameters

Liu

Baoyin

Marchis

2013

Astrophys Space Sci

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In this study, the hierarchical stability of the seven known large size ratio triple asteroids is investigated. The effect of the solar gravity and primary’s J2 are considered. The force function is expanded in terms of mass ratios based on the Hill’s approximation and the large size ratio property. The empirical stability parameters are used to examine the hierarchical stability of the triple asteroids. It is found that the all the known large size ratio triple asteroid systems are hierarchically stable. This study provides useful information for future evolutions of the triple asteroids.

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Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations

Cited by 65 publications

References 95 publications

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva

The hierarchical stability of the seven known large size ratio triple asteroids using the empirical stability parameters

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