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An Interferometric Study of CO and CS in Comet Hale-Bopp (C/1995 O1)

Published online by Cambridge University Press:  19 September 2017

Y.-J. Kuan ,
M.-L. Pen ,
H.-C. Huang ,
J. M. Veal  and
L. M. Woodney
Y.-J. Kuan
Affiliation:
National Taiwan Normal University, Taipei, Taiwan, ROC Academia Sinica Institute of Astronomy & Astrophysics, Taiwan
M.-L. Pen
Affiliation:
National Taiwan Normal University, Taipei, Taiwan, ROC
H.-C. Huang
Affiliation:
National Taiwan Normal University, Taipei, Taiwan, ROC
J. M. Veal
Affiliation:
Southwestern College, CA 91910, USA
L. M. Woodney
Affiliation:
Lowell Observatory, Flagstaff, AZ 86001, USA

Abstract

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We used the BIMA Array to observe CO and CS molecules in Comet Hale-Bopp (C/1995 O1) during the 1997 apparition. A spur-like structure around the cometary nucleus is observed. These molecular spurs may be attributed to gas or dust jets. Using Haser model, we find the theoretically predicted CO scale length agrees well with observations. A large fraction of CO is sublimated directly from the nucleus, with the remaining CO coming from icy dust grains in cometary coma. The [CO/H2O] abundance ratio of Hale-Bopp is consistent with that of icy dust grains in star forming regions. We conclude that Hale-Bopp was likely formed at the stage when there were still ample of icy grains in Solar Nebula; therefore, abundances of parent molecules in a comet may reflect the primordial chemical composition of the Nebula.

Type
Astrochemistry
Information
Symposium - International Astronomical Union , Volume 213: Bioastronomy 2002: Life Among the stars , 2004 , pp. 189 - 192
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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