Dust Morphology Of Comet Hale-Bopp (C/1995 O1). II. Introduction Of A Working Model

Details Dust Morphology Of Comet Hale-Bopp (C/1995 O1). II. Introduction Of A Working Model Dust Morphology Of Comet Hale-Bopp (C/1995 O1). II. Introduction Of A Working Model

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997em%26p...78..313s&link_type=abstract

Earth, Moon, and Planets, v. 78, Issue 1/3, p. 313-319 (1997).

Computer Science

9

Comet Hale-Bopp, Nucleus, Active Area, Dust Morphology, Computer Modelling

Scientific paper

A Monte Carlo image simulation code for dust features in comets is applied to comet Hale-Bopp in order to model the object's persistent porcupine-like appearance on high-resolution images taken between May 11 and Nov. 2, 1996. A self-consistent fan model is proposed, with six isolated sources of dust emission assumed at various locations on the surface of the rotating nucleus and with the spin axis undergoing a complex motion in an inertial coordinate system. In the framework of this model, jet pairs represent boundaries of fan-shaped formations described by dust ejected from isolated sources during periods of time when the Sun is above the local horizon. The spin axis is found to have traveled through a field of 10° by 20° during the examined period of nearly six months. Still more successful is a fan model with large diurnal dust-emission fluctuations, which is consistent with an inertially fixed position of the spin axis and requires only three discrete sources. In this scenario, the dust-emission profile is dominated by several brief flare-ups, or “puffs”, in the production of dust from one of the sources. The results are insensitive to the spin rate, but the observed dust coma appearance is more typical of a rapidly rotating comet.

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