C/1991 L3 (Levy)

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C/1991 L3 (Levy)
Discovery [1]
Discovered by David H. Levy
Discovery date14 June 1991
Designations
1991q, 1991 XI
Orbital characteristics [2]
Epoch 29 December 1991 (JD 2448619.5)
Observation arc 587 days
Number of
observations		136
Aphelion 26.643 AU
Perihelion 0.9827 AU
Semi-major axis 13.813 AU
Eccentricity 0.9289
Orbital period 51.34 years
Inclination 19.190°
329.432°
Argument of
periapsis 		41.479°
Last perihelion8 July 1991
Next perihelion30 October 2042 [3]
TJupiter 1.517
Earth MOID 0.075 AU
Jupiter MOID 0.050 AU
Physical characteristics [4]
Dimensions < 16.4 km
11.6 ± 0.2 km
8.34 hours
0.04 (assumed)
Comet total
magnitude (M1)		8.9
7.5 (1991 apparition)

C/1991 L3 (Levy) is a periodic comet discovered by David H. Levy on 14 June 1991. The comet has an orbital period of 51 years and thus fits the definition of Halley-type comets, which have orbital periods between 20 and 200 years.

Contents

Observational history

The comet was discovered by David H. Levy from his observatory in Tucson, Arizona, on 14 June 1991. He discovered the comet in the constellation of Pisces, near the galaxy Messier 74, using a 41-cm f/5 reflector telescope. He estimated it had an apparent magnitude of 8 and its coma was three arcminutes across, while no tail was visible. [1] The comet at that point was at a solar elongation of 54° and was located 1.27 AU from Earth. [5]

The presence of the comet was confirmed by M. Koishikawa from Sendai Observatory using a 300mm telephoto lens and the estimated magnitude was 7.5. The next day Alan Hale estimated the comet's magnitude to be 9.6 while C. S. Morris estimated it to be mag 8.5 using binoculars. [6] The closest approach to Earth took place on 17 June, at a distance of 1.27 AU. [5] On that day, David Levy reported the comet was 7.6 mag. and had a sunwards tail about 3 arcminutes long. An image of the comet from 18 June obtained with the Catalina 1.5-m reflector revealed ion streamers, a dust fan, and one or perhaps two dust envelopes. [7] For the rest of the month the comet's magnitude was reported to be between 8.4 and 8.7. [8] During July its magnitude remained constant. The comet passed perihelion on 8 July. C. S. Morris reported the comet on 15 July had a tail 50 arcminutes long with two components. [5]

The comet faded in August as it moved both away from Earth and the Sun and by the end of the month its magnitude was reported to be around 10. The comet continued to fade slowly and was reported to be mag. 13. It's coma was reported to be 1 arcminute across on 17 October. The comet was last observed on 21 January 1993 from Spacewatch, with an estimated magnitude of about 22. [5]

Orbit

The comet has an orbital period of 51.34 years and approaches close to Earth when perihelion is in September. In 1991, both S. Nakano and D. Green suggested that a comet observed in 1499 was a previous apparition of C/1991 L3 (Levy). [9]

During the 2042 apparition the comet is expected to approach Earth at a distance of 0.47 ± 0.07 AU in the second half of November (21 ± 8 November) and at the 2094 apparition it will approach Earth at a distance of 0.44 ± 0.09 AU on 3 August ± 5 days. [2]

Scientific results

The spectrum of the comet obtained on 18 June 1991 from Catalina Station showed the presence of CN, C2, C3, H2O+, and possibly NH2. [7] The comet was observed on 2 February 1992 displaying very minimal coma and a faint anti-tail whose morphology the comet had stopped outgassing. The light curve of the nucleus indicated a rotational period of 8.34 hours. [4] The light curve amplitudes indicated the nucleus was elongated, with a dimensions ratio of 1:1.3 or larger. The effective radius of the nucleus was estimated to be less than 8.2 kilometres (5.1 mi), being 5.8 ± 0.1 kilometers if an albedo of 0.04, the albedo of most cometary nuclei, is assumed. [4]

Meteors

The comet has a minimum orbit intersection distance with Earth of 0.075 AU leading to the assumption that it could create a meteor shower with a theoretical radius near Gamma Pavonis and peaking on 31 August/1 September. The presence of the shower has not been officially confirmed. [5] David Levy mentions that in 2006 meteors that could be attributed to the shower were observed by John Drummond, director of the Royal Astronomical Society of New Zealand. He mentioned the shower produced ten slow moving meteors within the span of 6 nights. [10]

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References

  1. 1 2 Green, Daniel (14 June 1991). "1991q; 1991 JW". International Astronomical Union Circular (5291).
  2. 1 2 "C/1991 L3 (Levy) – JPL Small-Body Database Lookup". ssd.jpl.nasa.gov. Jet Propulsion Laboratory . Retrieved 28 December 2024.
  3. ↑ Yoshida, Seiichi. "C/1991 L3 ( Levy )". www.aerith.net. Retrieved 28 December 2024.
  4. 1 2 3 Fitzsimmons, A.; Williams, I. P. (1994). "The nucleus of comet P/Levy 1991XI". Astronomy and Astrophysics. 289 (1): 304–310. Bibcode:1994A&A...289..304F. ISSN   0004-6361.
  5. 1 2 3 4 5 Kronk, Gary W.; Meyer, Maik; Seargent, David A. J. (2017). Cometography: a catalog of comets. Cambridge: Cambridge university press. pp. 596–600. ISBN   9780521872164.
  6. ↑ Green, Daniel (15 June 1991). "1991r; 1991q; 1991af; 1991d". International Astronomical Union Circular (5292).
  7. 1 2 Green, Daniel (18 June 1991). "COMET LEVY (1991q)". International Astronomical Union Circular (5293).
  8. ↑ Green, Daniel (2 July 1991). "COMET LEVY (1991q)". International Astronomical Union Circular (5296).
  9. ↑ Green, Daniel (13 July 1991). "COMET LEVY (1991q)". International Astronomical Union Circular (5306).
  10. ↑ Levy, David H. (2008). David Levy's guide to observing meteor showers. Cambridge: Cambridge University Press. p. 79. ISBN   9780511735196.
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