CCD observations of 11 faint asteroids

Sárneczky, K.; Szabó, Gy. M.; Kiss, L. L.

doi:10.1051/aas:1999251

Cited by 8 publications

(8 citation statements)

References 4 publications

(4 reference statements)

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“…In combination with the data by Sarneczky et al (1999) we derived a more precise value of the asteroid's rotation period of P = 6.364 ± 0.001 h. …”

Section: Fm5mentioning

confidence: 78%

See 1 more Smart Citation

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Krugly

Belskaya²,

Shevchenko³

et al. 2002

Icarus

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“…In combination with the data by Sarneczky et al (1999) we derived a more precise value of the asteroid's rotation period of P = 6.364 ± 0.001 h. …”

Section: Fm5mentioning

confidence: 78%

“…This Amor-type asteroid was first observed by Sarneczky et al (1999) for less than 3 h shortly after its discovery. With these observations they could only put constraints on the lightcurve amplitude (≥0.61 mag).…”

Section: Fm5mentioning

confidence: 94%

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Krugly

Belskaya²,

Shevchenko³

et al. 2002

Icarus

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“…The first photometry including 41 data points was discussed in Harris & Young (1989); later, Wisniewski et al (1997) presented the second lightcurve of this asteroid. We presented the lightcurve in the 1998 opposition in Sárneczky et al (1999). In this paper both the lightcurves of the opposition in 1999 (Fig.…”

Section: Cerberusmentioning

confidence: 99%

Photometric observations of 9 Near-Earth Objects

Szabó

Csák

Sárneczky

et al. 2001

A&A

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Abstract. We present new CCD observations of nine Near-Earth Asteroids carried out between February, 1999 and July, 2000. The bulk of the data was acquired through an RC filter, while the minor planet 11405 was observed without filter. We could determine synodic periods and amplitudes for 5 asteroids, 699: 3. (5) for this object with retrograde rotation. The remaining 3 objects have only partial coverage, thus no firm conclusion on their synodic period is possible.

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“…Such phenomenon are expected to greatly constrain the orbital model. (1089) Tama was observed on 1998-04-04 by Sárneczky, Szabó & Kiss (1999). Their light curve, covering about a quarter of the period, including the minimum of brightness, did not show any sign of eclipse in the 0.03 mag variation.…”

Section: Size Orbit and Densitiesmentioning

confidence: 93%

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

Behrend¹,

Bernasconi²,

Roy³

et al. 2006

A&A

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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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CCD observations of 11 faint asteroids

Abstract: Abstract. We present new CCD observations of 11 poorly studied, faint and moderately faint asteroids. Six of them

Cited by 8 publications

References 4 publications

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Photometric observations of 9 Near-Earth Objects

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

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