Infrared Observations Of Dust Emission From Comet Hale-Bopp |
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Authors: | Lisse C M Fernández Y R A'hearn M F Kostiuk T Livengood T A Käufl H U Hoffmann W F Dayal A Ressler M E Hanner M S Fazio G G Hora J L Peschke S B Grün E Deutsch L K |
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Institution: | (1) Department of Astronomy, University of Maryland, College Park, MD 20742, USA;(2) NASA/GSFC, Code 693.1, Greenbelt, MD 20771, USA;(3) ESO, KarlSchwarzschildstrasse 2, 85748 Garching, Germany;(4) Steward Observatory, University of Arizona, Tucson, AZ 85721, USA;(5) NASA/JPL, 4800 Oak Grove Drive, Pasadena, CA 91104, USA;(6) Opt.& Infrared Astron. Div., Harvard-SAO, 60 Garden Street, Cambridge, MA 02138, USA;(7) Max-Planck-Institut für Kernphysik, Saupfercheckweg1, Heidelberg, Germany;(8) Astronomy Dept./CAS 519, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA |
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Abstract: | We present infrared imaging and photometry of the bright, giant comet C/1995 O1 (Hale-Bopp). The comet was observed in an
extended infrared and optical observing campaign in 1996–1997. The infrared morphology of the comet was observed to change
from the 6 to 8 jet “porcupine” structure in 1996 to the “pinwheel” structure seen in 1997; this has implications for the
position of the rotational angular momentum vector. Long term light curves taken at 11.3 μm indicate a dust production rate
that varies with heliocentric distance as ∶ r−1.4. Short term light curves taken at perihelion indicate a rotational periodicity of 11.3 hours and a projected dust outflow
speed of ∶ 0.4 km s−1. The spectral energy distribution of the dust on October 31, 1996 is well modeled by a mixture of 70% silicaceous and 30%
carbonaceous non-porous grains, with a small particle dominated size distribution like that seen for comet P/Halley (McDonnell
et al., 1991), an overall dust production rate of 2 × 105 kg s−1, a dust-to-gas ratio of ∶5, and an albedo of 39%.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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Keywords: | Comets infrared radio rotation surfaces origin |
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