Eclipsing binary asteroid 90 Antiope

Michałowski, Tadeusz; Bartczak, P.; Velichko, F. P.; Kryszczyńska, A.; Kwiatkowski, T.; Breiter, S.; Colas, François; Fauvaud, S.; Marciniak, A.; Michałowski, J.; Hirsch, R.; Behrend, R.; Bernasconi, L.; Rinner, C.; Charbonnel, S.

doi:10.1051/0004-6361:20040449

Cited by 22 publications

(18 citation statements)

References 9 publications

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“…We consider the lightest one, (854) Frostia, with a mean bulk density of 0.9. This is comparable with the C Type asteroid (90) Antiope with a bulk density of 1.3 (Michalowski et al 2004). If it is a C type asteroid, the bulk density of its matter could be 1.65 like the CI Orgueil meteorite.…”

Section: Size Orbit and Densitiessupporting

confidence: 51%

“…Amongst the 4.5×10 2 observed asteroids in our database, about 10 of them were observed knowing that they were binary (for example (69230) Hermes, Margot et al 2003; (90) Antiope, Michalowski et al 2004), whilst others were observed without detecting that they are in fact a minor planet plus one satellite (for example (130) Elektra, (45) Eugenia, (22) Kalliope). About 40 other minor planets cannot be included in the binarity detection because they were not observed for long enough to cover at least 2/3 of the phased light curve (at least, half the light curve is required to unambiguously detect an eclipse event in a synchronised system).…”

Section: Description Of the Samplementioning

confidence: 94%

“…Based on binary system light curves anlysis, we present a method to derive the bulk density independently of size and mass determinations. From single opposition measurements the accuracy of the bulk density determination is about 30 percent, but this can be easily improved as in the case of (90) Antiope (Michalowski et al 2004) by additional data from several oppositions. This paper is devoted to the discovery of four binary systems from their light curves.…”

Section: Introductionmentioning

confidence: 99%

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Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy

Behrend¹,

Bernasconi²,

Roy³

et al. 2006

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Aims. We present evidence that four minor planets of the main belt are binary systems. Methods. These discoveries are based on CCD photometric measurements made by many observers coordinated in a network of observatories. Results. Orbital and physical properties are derived from a total of 134 partial light curves involving 26 stations. (854) Frostia, (1089) Tama, (1313) Berna, and (4492) Debussy show mutual eclipses features on their light curves. In all cases, rotation and revolution are synchronous. Synodic periods are 37. 728, 16.444, 25.464 and 26.606 h respectively. From a simple model, we have derived their bulk densities as follows: 0.89 ± 0.14, 2.52 ± 0.30, 1.22 ± 0.15 and 0.91 ± 0.10 g cm −3 respectively. Uncertainties in the bulk densities, arising from scattering and shadow effects are not taken into account. These could increase the density estimates by a factor up to 1.6. Our method of determining bulk density is completely independent of their mass and their diameter estimates. The low rotational periods and the low bulk densities clearly imply a collisional process to explain this kind of binary asteroid. Based on our database of a few thousand light curves of minor planets, the population of similar-sized objects in the main belt is estimated to 6 ± 3 percent in the 10-50 km diameter class.Key words. planets and satellites: formation -minor planets, asteroids -techniques: photometric IntroductionThe first confirmed satellite of a minor planet was Dactyl around (243) Ida, discovered in 1993 on Galileo spacecraft images (Belton & Carlson 1993). Ten years later, about fifty asteroids are suspected or confirmed to be multiple bodies. These asteroids are very useful in determining the physical and dynamical properties of small bodies, in particular the bulk density, which is important in understanding the collisional evolution of this kind of object.Various techniques are used to detect satellites for minor planets: occultation of stars, light curves, direct imaging by spacecraft, radars or adaptive optic (see review by Merline et al. 2002). Binary studies allows the derivation of dimensions, shape, bulk densities, rotation and orbital properties of the bodies. Asteroid densities are known for only a few of them Based on observations performed with the T1 M and T60 cm at the Pic du Midi, TAROT at the Calern observatory, Faulkes-North at Hawaii, T50 cm at Brorfelde, and by many amateur observatories coordinated by Geneva Observatory.(see the review by Britt et al. 2002). We distinguish two types of multiple systems. Those consisting of comparable size bodies are designated as binary. The others are designated as primaries with satellites. When the orbital plane of a binary system is seen edge-on, mutual eclipses can be detected from light curves. That allows to discover binary systems that cannot be found by other methods. Based on binary system light curves anlysis, we present a method to derive the bulk density independently of size and mass determinations. From single opposition measurement...

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Section: Size Orbit and Densitiessupporting

confidence: 51%

Section: Description Of the Samplementioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

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Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy

Behrend¹,

Bernasconi²,

Roy³

et al. 2006

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“…in [27], [28] and [21]). Recently a new algorithm capable to generate model solutions for binary asteroids has been developed using a nonconvex shape representation of the components [1].…”

Section: Models Of Binary Asteroidsmentioning

confidence: 99%

Shape Models and Physical Properties of Asteroids

Santana-Ros¹,

Dudziński²,

Bartczak³

2016

Astrophysics and Space Science Proceedings

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Despite the large amount of high quality data generated in recent space encounters with asteroids, the majority of our knowledge about these objects comes from ground based observations. Asteroids travelling in orbits that are potentially hazardous for the Earth form an especially interesting group to be studied. In order to predict their orbital evolution, it is necessary to investigate their physical properties. This paper briefly describes the data requirements and different techniques used to solve the lightcurve inversion problem. Although photometry is the most abundant type of observational data, models of asteroids can be obtained using various data types and techniques. We describe the potential of radar imaging and stellar occultation timings to be combined with disk-integrated photometry in order to reveal information about physical properties of asteroids.

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“…Thanks to the Keck Adaptive Optics observations (Merline et al 2000) and extensive photometric data covering 5 oppositions (first 4 collected in Michałowski et al 2004), the asteroid 90 Antiope is known to be an interesting example of a binary system with two comparable components. According to the recent results of Michałowski et al (2004), Antiope is most likely an almost synchronous system with the rotation period of the primary T e = 16. h 5047 ± 0.0002 and the orbital period of the satellite T s = 16. h 5051 ± 0.0002.…”

Section: Binary System Of 90 Antiopementioning

confidence: 99%

Synchronous motion in the Kinoshita problem

Breiter¹,

Melendo²,

Bartczak³

et al. 2005

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Abstract.A Lie-Poisson integrator with Wisdom-Holman type splitting is constructed for the problem of a rigid body and a sphere (the Kinoshita problem). The algorithm propagates not only the position, momentum and angular momentum vector of the system, but also the tangent vector of "infinitesimal displacements". The latter allow to evaluate the maximum Lyapunov exponent or the MEGNO indicator of Cincotta and Simó. Three exemplary cases are studied: the motion of Hyperion, a fictitious binary asteroid with Hyperion as one of the components, and the binary asteroid 90 Antiope. In all cases the attitude instability of the rotation state with spin vector normal to an equatorial orbit influences stability of the system at lower rotation rates. The MEGNO maps with variations restricted to the orbital plane for position and momentum, and to the orbit normal direction for the angular momentum resemble usual Poincaré sections. But if no restriction is imposed on the variations, some stable zones turn into highly chaotic regions, often retaining the shape of their boundaries.

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Eclipsing binary asteroid 90 Antiope

Cited by 22 publications

References 9 publications

Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy

Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy

Shape Models and Physical Properties of Asteroids

Synchronous motion in the Kinoshita problem

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