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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Affiliation: | (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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