Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition

A. Erikson, J. Berthier, P. V. Denchev, A. W. Harris, Z. Ioannou, A. Kryszczynska, C. I. Lagerkvist, P. Magnusson, T. Michalowski, A. Nathues, J. Piironen, P. Pravec, L. Šarounová, F. Velichko

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Abstract

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.

Original languageEnglish
Pages (from-to)327-330
Number of pages4
JournalPlanetary and Space Science
Volume47
Issue number3-4
Publication statusPublished - 1999

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Io
occultation
asteroids
asteroid
modeling
color
Infrared Astronomy Satellite
night
photometry
charge coupled devices
poles
index

ASJC Scopus subject areas

  • Geophysics
  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Erikson, A., Berthier, J., Denchev, P. V., Harris, A. W., Ioannou, Z., Kryszczynska, A., ... Velichko, F. (1999). Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition. Planetary and Space Science, 47(3-4), 327-330.

Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition. / Erikson, A.; Berthier, J.; Denchev, P. V.; Harris, A. W.; Ioannou, Z.; Kryszczynska, A.; Lagerkvist, C. I.; Magnusson, P.; Michalowski, T.; Nathues, A.; Piironen, J.; Pravec, P.; Šarounová, L.; Velichko, F.

In: Planetary and Space Science, Vol. 47, No. 3-4, 1999, p. 327-330.

Research output: Contribution to journalArticle

Erikson, A, Berthier, J, Denchev, PV, Harris, AW, Ioannou, Z, Kryszczynska, A, Lagerkvist, CI, Magnusson, P, Michalowski, T, Nathues, A, Piironen, J, Pravec, P, Šarounová, L & Velichko, F 1999, 'Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition', Planetary and Space Science, vol. 47, no. 3-4, pp. 327-330.
Erikson, A. ; Berthier, J. ; Denchev, P. V. ; Harris, A. W. ; Ioannou, Z. ; Kryszczynska, A. ; Lagerkvist, C. I. ; Magnusson, P. ; Michalowski, T. ; Nathues, A. ; Piironen, J. ; Pravec, P. ; Šarounová, L. ; Velichko, F. / Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995-96 apparition. In: Planetary and Space Science. 1999 ; Vol. 47, No. 3-4. pp. 327-330.
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abstract = "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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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.

PY - 1999

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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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