The dust tail of Comet Liller 1988 V

Details The dust tail of Comet Liller 1988 V The dust tail of Comet Liller 1988 V

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...253..615f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 253, no. 2, Jan. 1992, p. 615-624.

Astronomy and Astrophysics

Astrophysics

25

Charge Coupled Devices, Comet Tails, Cosmic Dust, Solar System, Isophotes, Radiation Pressure

Scientific paper

The paper discusses the analysis of three CCD frames secured with the 1.06-m Hoher List telescope concerning the dust tail of Comet Liller 1988 V, which were used as input for the inverse numerical approach to the interpretation of comet dust tails (Fulle, 1989). Dust grains are considered of diameters between 15 microns and 10 cm ejected during the time interval t between -200 and +40 (days related to perihelion), and a lower limit of the dust mass production of (4 +/-1) 10 exp 13 g (for an assumed albedo for the phase function Ap(alpha) = 0.06, alpha = 50 deg) and a power index of the time-averaged size distribution of -3.5 +/-0.2 are obtained. The observing geometry leads to the detection of distinct subsets of the total dust distribution: large and slow preperihelion grains and smaller and faster postperihelion grains. The measured lower limit to the total dust mass loss rate reaches a broad maximum of about 5 x 10 exp 6 g/s a week before perihelion, whereas the dust velocity reaches the highest values two weeks after. At least half of the total dust mass was injected into orbits bound in the solar system, supplying a significant source of interplanetary meteoroids of sizes larger than 0.4 mm.

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