TY - JOUR
T1 - Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition
AU - Erikson, A.
AU - Berthier, J.
AU - Denchev, P. V.
AU - Harris, A. W.
AU - Ioannou, Z.
AU - Kryszczynska, A.
AU - Lagerkvist, C. I.
AU - Magnusson, P.
AU - Michalowski, T.
AU - Nathues, A.
AU - Piironen, J.
AU - Pravec, P.
AU - Šarounová, L.
AU - Velichko, F.
N1 - Funding Information:
The work performed by T. Michalowski and A. Kryszczynska was supported by the Polish Grant KBN 2 P03D 024 09. J. Piironen wishes to thank the NorFA foundation, Oslo, Norway, for financial support. The work by P. Pravec and L. Šarounová was supported by the Grant Agency of the Czech Republic, Grant 205-95-1498. F. Velichko acknowledges support from the American Astronomical Society. We would like to thank the two referees, M. A. Barucci and K. Muinonen, for providing constructive reviews.
PY - 1999
Y1 - 1999
N2 - The asteroid 85 Io has been observed using CCD and photoelectric photometry on 18 nights during its 1995-96 and 1997 apparitions. We present the observed lightcurves, determined colour indices and modelling of the asteroid spin vector and shape. The colour indices (U-B = 0.35±0.02, B-V = 0.66±0.02, V-R = 0.34±0.02, R-I = 0.36±0.02) are as expected for a C-type asteroid. The allowed spin vector solutions have the pole co-ordinates λ0 = 285±4°, β0 = -52±9° or λ0 = 108±10°, β0 = -46±10° and λ0 = 290±10°, β0 = -16±10° with a retrograde sense of rotation and a sidereal period Psid = 0d.286463±0d.000001. During the 1995-96 apparition the International Occultation Time Association (IOTA) observed an occultation event by 85 Io. The observations and modelling presented here were analysed together with the occultation data to develop improved constraints on the size of the asteroid. The derived value of 164 km is about 5% larger than the IRAS diameter.
AB - The asteroid 85 Io has been observed using CCD and photoelectric photometry on 18 nights during its 1995-96 and 1997 apparitions. We present the observed lightcurves, determined colour indices and modelling of the asteroid spin vector and shape. The colour indices (U-B = 0.35±0.02, B-V = 0.66±0.02, V-R = 0.34±0.02, R-I = 0.36±0.02) are as expected for a C-type asteroid. The allowed spin vector solutions have the pole co-ordinates λ0 = 285±4°, β0 = -52±9° or λ0 = 108±10°, β0 = -46±10° and λ0 = 290±10°, β0 = -16±10° with a retrograde sense of rotation and a sidereal period Psid = 0d.286463±0d.000001. During the 1995-96 apparition the International Occultation Time Association (IOTA) observed an occultation event by 85 Io. The observations and modelling presented here were analysed together with the occultation data to develop improved constraints on the size of the asteroid. The derived value of 164 km is about 5% larger than the IRAS diameter.
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U2 - 10.1016/S0032-0633(98)00128-7
DO - 10.1016/S0032-0633(98)00128-7
M3 - Article
AN - SCOPUS:0342987172
SN - 0032-0633
VL - 47
SP - 327
EP - 330
JO - Planetary and Space Science
JF - Planetary and Space Science
IS - 3-4
ER -