Photometric evidences for the binary asteroids 87 sylvia and 423 diotima

Прокофьева, В. В.; Demchik, M. L.; Karachkina, L. G.

doi:10.1080/10556799508226945

Cited by 7 publications

(4 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The minor planet (87) Sylvia is a main belt asteroid discovered in 1866 by Pogson (1866). In the 1990s, frequency analysis of photometric observations hinted that this asteroid could be binary Demchik 1992, 1994;Prokof'eva et al 1995). Its first satellite (S/2001 (87) 1, known as Romulus) was discovered in February 2001 by Brown et al (2001) using the Keck II telescope atop Hawaii's Mauna Kea.…”

Section: Introductionmentioning

confidence: 99%

Physical and dynamical properties of the main belt triple Asteroid (87) Sylvia

Berthier

Vachier

Marchis

et al. 2014

Icarus

View full text Add to dashboard Cite

We present the analysis of high angular resolution observations of the triple asteroid (87) Sylvia collected with three 8-10 m class telescopes (Keck, VLT, Gemini North) and the Hubble Space Telescope. The moons' mutual orbits were derived individually using a purely Keplerian model. We computed the position of Romulus, the outer moon of the system, at the epoch of a recent stellar occultation which was successfully observed at less than 15 km from our predicted position, within the uncertainty of our model. The occultation data revealed that the moon, with a surface-area equivalent diameter D S = 23.1 ± 0.7 km, is strongly elongated (axes ratio of 2.7 ± 0.3), significantly more than single asteroids of similar size in the main-belt. We concluded that its shape is probably affected by the tides from the primary. A new shape model of the primary was calculated combining adaptive-optics observations with this occultation and 40 archived light-curves recorded since 1978. The difference between the J 2 = 0.024 +0.016 −0.009 derived from the 3-D shape model assuming an homogeneous distribution of mass for the volume equivalent diameter D V = ✩ Based on observations collected at the European Southern Observatory,

show abstract

Section: Introductionmentioning

confidence: 99%

Physical and dynamical properties of the main belt triple Asteroid (87) Sylvia

Berthier

Vachier

Marchis

et al. 2014

Icarus

View full text Add to dashboard Cite

show abstract

“…Its diameter is about 20 kilometers. Previous observations were made in 1986 (Wisniewski & McMillan 1987) and in 1988(Prokof'eva et al 1992. Precise lightcurves were presented, so we could model this moderately faint asteroid (13.9 mag during our observing run).…”

Section: Mettementioning

confidence: 77%

CCD observations of 11 faint asteroids

Sárneczky

Szabó

Kiss

1999

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

show abstract

“…Previous CCD photometric observations were reported by Wisniewski & McMillan (1987), Prokof'eva et al (1992), and Sarneczky et al (1999), who derived unreliable synodic rotational periods of 2.637 ± 0.004 h and 3.22 ± 0.22 h, on the basis of poor-sampled and incomplete lightcurves.…”

Section: Mettementioning

confidence: 97%

“…The asteroid 1727 Mette is a relatively small object (D ≈ 7 km; Wisniewski & McMillan, 1987), belonging to the Hungaria zone, as defined by Zellner et al (1985). Previous CCD photometric observations were reported by Wisniewski & McMillan (1987), Prokof'eva et al (1992, and Sarneczky et al (1999), who derived unreliable synodic rotational periods of 2.637 ± 0.004 h and 3.22 ± 0.22 h, on the basis of poor-sampled and incomplete lightcurves. In order to confirm our result, further V and R photometric observations were carried out during five nights in April 2003, at the same observing site using the CCD ITANET camera.…”

Section: Mettementioning

confidence: 99%