Grain Properties of the Dust in Comet C/1995 O1 Hale-Bopp

Details Grain Properties of the Dust in Comet C/1995 O1 Hale-Bopp Grain Properties of the Dust in Comet C/1995 O1 Hale-Bopp

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.6526h&link_type=abstract

American Astronomical Society, DPS Meeting #32, #65.26; Bulletin of the American Astronomical Society, Vol. 32, p.1644

Astronomy and Astrophysics

Astronomy

Scientific paper

Comets are a collection of dust and ices formed early during protosolar disk evolution. Probing the mineralogy and properties of dust grains in comets can yield insight into conditions and processes which existed in the protoplanetary disk. Because of its brightness, comet Hale-Bopp afforded us a unique opportunity to examine its dust properties through a range of heliocentric distances, pre and post perihelion. In building on the dust mineralogy of Hale-Bopp as presented by Wooden et al. (1999, ApJ, 517, 1034) and Wooden et al. (2000, Icarus, 143, 126), we present model fits to the spectral energy distribution (SED) of Hale-Bopp during four temporal epochs pre and post perihelion: 1996 October UT (rh = 2.8 AU), 1997 February UT (rh = 1.21 AU), and 1997 June UT (rh = 1.7 AU). Each epoch includes data from the HIFOGS mid-infrared spectrometer, covering the 10 μ m window in which identifying silicate resonances are detected. Using Mie scattering theory to calculate radiative equilibrium temperatures and laboratory optical extinctions of crystalline silicates, we have modeled the 1 - 45μ m SED of Hale-Bopp at each epoch. Presented are the constraints determined for the dust grain parameters. Findings include the requirement of the use of fractal porous amorphous grains at each epoch, and the constraint that the crystalline grains are solid and sub-micron (<= 1 μ m) in size. We acknowledge funding from NAG 5-7906, NSF, NRC and NASA.

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