Evidence for Dust Related X-ray Emission from Comet C/1995 O1 (Hale-Bopp)

Details Evidence for Dust Related X-ray Emission from Comet C/1995 O1 (Hale-Bopp) Evidence for Dust Related X-ray Emission from Comet C/1995 O1 (Hale-Bopp)

1997-10-31

arxiv.org/abs/astro-ph/9710363v1

Astronomy and Astrophysics

Astrophysics

17 pages. 4 postscript figs (2 in color). Accepted for publication in ApJ (Letters)

Scientific paper

10.1086/311119

We report the discovery of X-ray emission from comet C/1995 O1 (Hale-Bopp) by the LECS instrument on-board BeppoSAX on 1996 September 10--11. The 0.1--2.0 keV luminosity decayed by a factor of 2 on a timescale of ~10 hr with a mean value of 5.10E16 erg s-1. The spectrum is well fit by a thermal bremsstrahlung model with a temperature of 0.29 +/- 0.06 keV, or a power-law with a photon index of 3.1 +{0.6} -{0.2}. The lack of detected C and O line emission places severe constraints on many models for cometary X-ray emission, especially those which involve X-ray production in cometary gas. The luminosity is a factor of at least 3.4 greater than measured by Extreme Ultraviolet Explorer (EUVE) 4 days later. This difference may be related to the emergence from the nucleus on 1996 September 9 of a dust-rich cloud. Over the next few days the cloud continued to expand becoming increasingly tenuous, until it had reached an extent of ~3.10E5 km (or ~2 arcmin) by the start of EUVE observation. We speculate that the observed reduction in X-ray intensity is evidence for dust fragmentation. These results support the view that cometary X-ray emission arises from the interaction between solar X-rays and cometary dust.

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