The dust coma of Comet P/Giacobini-Zinner in the infrared

Details The dust coma of Comet P/Giacobini-Zinner in the infrared The dust coma of Comet P/Giacobini-Zinner in the infrared

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....104..386h&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 104, no. 1, July 1992, p. 386-393.

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21

Astronomical Photometry, Cometary Atmospheres, Giacobini-Zinner Comet, Infrared Telescopes, Scattering Cross Sections, Spectral Emission, Astronomical Observatories, Cosmic Dust, Halley'S Comet, Silicates, Thermal Emission

Scientific paper

The paper presents 1-20-micron photometry of P/Giacobini-Zinner obtained at the NASA Infrared Telescope Facility, during 1985 June-September (r = 1.57-1.03 AU). A broad, weak 10-micron silicate emission feature was detected on August 26.6; a similar weak emission feature could have been hidden in the broadband photometry on other dates. The total scattering and emitting cross section of dust in the inner coma was similar to that in other short-period comets, but a factor of 10 (r = 1.56 AU) to 100 (r = 1.03 AU) lower than the amount of dust in Comet Halley. The thermal emission continuum can be fit with models weighted toward either small or large absorbing grains. The dust production rate near perihelion was about 100,000 g/s (small-grain model) to about 1,000,000 g/s (large-grain model). The corresponding dust/gas mass ratio on August 26 was about 0.1-1. A silicate-rich heterogeneous grain model with an excess of large particles is compatible with the observed spectrum of Giacobini-Zinner on August 26. Thus, weak or absent silicate emission does not necessarily imply an absence of silicates in the dust, although the abundance of silicate particles not greater than 1 micron radius must have been lower than in Comet Halley.

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