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Поисковые слова: п п п п п п п п п п п п п п п п п п п п п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п р п
Minor planet lightcurve parameters

Minor planet lightcurve parameters


  

Notes. An asterisk (*) between the asteroid number and name denotes a new or significantly changed entry (data have been changed over three units of the last decimals or have been added) as compared with the lightcurve parameters table published last year. Also asterisk marks entries where the reliability code has been changed or new symbol A or B or T has been added (or eliminated).  In column “Period” the rotation period expressed in hours is given. The value quoted is the most reliable of the individual values reported, or a subjective “best estimate” based on sometimes discordant results. In column “Variation” the amplitude of variation or range of amplitude observed at all aspects is given (some adjustments have been made to estimate the amplitude which would have been observed at low phase angle at the same aspect). In column “Note” a reliability code is given as follows:

    1. Very tentative result, may be completely wrong.

    2. Reasonably secure result, based on over half coverage of the lightcurve.

    3. Secure result, full lightcurve coverage, no ambiguity of period.

    4. Multiple apparition coverage, pole position reported.

A blank reliability code implies incomplete or inconclusive result.
Following the reliability code is a space for remarks, with the following meanings.

    1. Number of extrema per rotation cycle (e.g., 1, 3). Unless otherwise noted, two per cycle is assumed.

    2. Ambiguous period. The “most likely” period is listed, with other possibilities listed in a footnote ordered by asteroid number, below.

    3. Suspected binary object, based on a second periodicity in the lightcurve data (see footnote).

    4. Rotation period “determined” from published data, but not given by author(s) of original data.

    5. No lightcurve published.
    6. Photographic photometry.
    7. “Tumbling”, that is, non-principal axis rotation motion.
    8. Visual photometry.
    9. Radar observation.

Footnotes and alternative values for ambiguous periods

    1. A  P=13.13 or 6.668 hours
    2. A  P=26.56 hours
    3. B  synchronous, equal diameters
    4. A  P=14.46 hours
    5. A  P=10.9 hours
    6. A  P=42.62 hours
    7. T  P=250 hours
    8. A  P=12 hours
    9. A  P=10.1 hours
    10. A  P=  4.35 or 8.03 hours
    11. A  P=  8.67 hours
    12. A  P=19.35 hours
    13. A  P=16.804 hours
    14. A  P=38.4 hours
    15. A  P=  2.9 hours
    16. A  P=12.0 hours
    17. A  P=  6.78 hours
    18. B  synchronous, 10.6 km and 7.4 km in diameter

    19. B? a modulation of P=7.90 h., ampl.=0.15  mag. was observed near minimum light of the longer period variation. Binzel [1] interprets this as the real rotation period, with the long period being a precession period caused by unseen satellite

    20. B  synchronous, equal diameters
    21. B  2.7 km in diameter, separation = 140 km; adaptive optics
    22. A  P=16.45 hours
    23. A  P=  8.86 hours
    24. A  P=10.3 hours
    25. A  P=  5.5 hours
    26. A  P=  3.862 hours
    27. A  P=  6.65 hours

    28. B  P=27.72 h., ampl. = 0.08 mag. Binary based on apparent eclipse events in the lightcurve with a period (secondary orbital?) of the longer value given [2]

    29. B  P=36.57 h., ampl.=0.3 mag.
    30. T  P1=176 hours, P2=130 hours
    31. B  synchronous, equal diameters
    32. A  P=12 hours

    33. B? P=  6.760 h., ampl. = 0.08 mag. Suspected binary based on apparent eclipse events in the lightcurve with a period (secondary orbital?) of the longer value given [3]

    34. A  P=  2.919 hours
    35. A  P=  3.638 hours
    36. A  P=  7.69 or 11.9 hours
    37. A  P=  3.638 hours
    38. B  2 km in diameter, separation = 230 km; HST

    39. B? P=  7.003 h., ampl. = 0.09 mag. Suspected binary based on a second periodicity in the lightcurve data with a period (secondary orbital?) of the longer value given [3]

    40. A  P=  9.8 hours
    41. B  P=32.69 h., ampl.=0.18 mag. [4]
    42. T  P=52.79 hours
    43. B  P=11.9 h., ampl.=0.08 mag.
    44. B  P=14.53 h., ampl.=0.2 mag.
    45. B  P=17.45 h., ampl.=0.34 mag.
    46. B  synchronous, 0.63 km and 0.57 km in diameter
    47. A  P=10.22 hours
    48. A  P=19.34 hours
    49. B  P=17.72 h., ampl.=0.2 mag., 0.42 km and 0.20 km in diameter
    50. A  P=122.3 hours
    51. B  P=16.40 h., ampl.=0.14 mag.
References:

  1. R. P. Binzel// A photoelectric survey of 130 asteroids. Icarus, 1987. V. 72, P. 135–208

  2. IAUC 6680, 1997

  3. Pravec P. et al.// Two-period lightcurves of 1996 FG3, 1998 PG and (5407) 1992 AX: one probable and two possible binary asteroids. Icarus, 2000. V. 146, P.190–203

  4. Pravec P. et al.// Occultation/eclipse events in binary asteroid 1991 VH. Icarus, 1998. V. 133, P.79–88