CCD photometry, spin and shape models of five asteroids: 225,
 360, 416, 516, and 1223

Michałowski, Tadeusz; Pych, W.; Berthier, J.; Kryszczyńska, A.; Kwiatkowski, T.; Boussuge, J.; Fauvaud, S.; Denchev, P.; Baranowski, R.

doi:10.1051/aas:2000282

Cited by 16 publications

(9 citation statements)

References 8 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Observations of other asteroids performed in Borowiec have been already published, together with the new models in, for example, Michałowski et al (2000Michałowski et al ( , 2001, Kryszczyńska et al (2003), Ďurech et al (2007), and in the three previous papers of the present series - Michałowski et al (2004Michałowski et al ( , 2005Michałowski et al ( , 2006.…”

Section: Observations Of Three Main Belt Asteroidsmentioning

confidence: 78%

Photometry and models of selected main belt asteroids

Marciniak¹,

Michałowski²,

Kaasalainen

et al. 2007

A&A

Self Cite

View full text Add to dashboard Cite

Section: Observations Of Three Main Belt Asteroidsmentioning

confidence: 78%

Photometry and models of selected main belt asteroids

Marciniak¹,

Michałowski²,

Kaasalainen

et al. 2007

A&A

Self Cite

View full text Add to dashboard Cite

“…We carried out optical photometric observations of 1998 SF36 during its 2001 apparition, using the 105-cm Kiso Schmidt telescope with the SITe 2KCCD, the 50-cm NAOMitaka telescope with the Astromed CCD (Dermawan et al, 2002) and the 105-cm Pic du Midi telescope with the Thomson CCD (Michałowski et al, 2000). The observational conditions are summarized in Table 1.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Pole orientation and triaxial ellipsoid shape of (25143) 1998 SF36, a target asteroid of the MUSES-C* mission

et al. 2014

View full text Add to dashboard Cite

The near-earth asteroid (25143) 1998 SF36 is a target body for the Japanese sample-return MUSES-C mission. We present here its pole orientation and triaxial ellipsoid shape, using light curve data obtained with three telescopes at Kiso, Mitaka, and Pic du Midi. The solution obtained for the pole orientation has ecliptic latitude λ = 320 ± 30• and ecliptic longitude β = −75 ± 12• . The estimated triaxial ellipsoid shape is a/b = 2.1 and b/c = 1.7 assuming m = 0.03, which is the coefficient of the empirical relation between the light curve amplitude and the phase angle for S-type asteroids (Zappalà et al., 1990). We also found m to be related to asteroid surface roughness, using a light curve simulator.

show abstract

“…The published data come from Harris & Young (1983), Di Martino et al (1987), Dotto et al (1995), and Michalowski et al (2000). The time stamps of all involved observations were corrected by the light time and then converted into JD in the TDB time system.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Until now, no other direct evidence confirms the binarity of (171) Ophelia except the V-shape minima of the light curves and, in addition, no pole orientation and shape information have been derived for it. Several groups studied the spin parameters and shape of (360) Carlova (Harris & Young 1983;Di Martino et al 1987;Michalowski et al 2000;Ďurech et al 2009;Wang & Zhang 2006), and reported inconsistent spin parameters because different data sets or different analysis methods were used. The last analysis for Carlova was made byĎurech et al (2009) with the convex inversion technique using six published light curves at two apparitions, from which a pair of poles slightly different from those previously published were given.…”

Section: Introductionmentioning

confidence: 99%

Photometric analysis for the spin and shape parameters of the C-type main-belt asteroids (171) Ophelia and (360) Carlova

Wang

Muinonen

Wang

et al. 2015

A&A

View full text Add to dashboard Cite

Aims. Two C-type main-belt asteroids (171) Ophelia and (360) Carlova are studied for their spin parameters and shapes in the present paper. Although it was suspected that Ophelia was a binary system owing to the eclipse features in the light curve obtained in 1977, no direct evidence has been obtained to confirm the binarity. To verify the previous findings, the spin parameters and shape of Ophelia are derived by analyzing the photometric data. To understand the dispersion in the previous determination of Carlova's spin parameters, new observational data and existing photometric data are reanalyzed to find a homogenous solution for its spin parameters and shape. Methods. The spin parameters and shapes of two asteroids were determined from photometric data using the convex inversion technique. The simplified virtual-observation Markov chain Monte Carlo method was applied to estimate the uncertainties of the spin parameters and to understand the divergence of derived shapes. Results. A pair of possible poles for Ophelia are derived, the spin periods corresponding to the two poles are nearly the same. The convex shape of Ophelia shows binary characteristics. For Carlova, a unique pole solution and its convex shape are ascertained together with the occultation observations. The convex shape of Carlova shows that it is a rough ellipsoid.

show abstract

CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

Cited by 16 publications

References 8 publications

Photometry and models of selected main belt asteroids

Photometry and models of selected main belt asteroids

Pole orientation and triaxial ellipsoid shape of (25143) 1998 SF36, a target asteroid of the MUSES-C* mission

Photometric analysis for the spin and shape parameters of the C-type main-belt asteroids (171) Ophelia and (360) Carlova

Contact Info

Product

Resources

About