The Interaction of C/1995 O1 Hale-Bopp with the Solar Wind as recorded in CoCam Images: A Progress Report

Details The Interaction of C/1995 O1 Hale-Bopp with the Solar Wind as recorded in CoCam Images: A Progress Report The Interaction of C/1995 O1 Hale-Bopp with the Solar Wind as recorded in CoCam Images: A Progress Report

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997em%26p...77..281j&link_type=abstract

Earth, Moon, and Planets, v. 77, Issue 3, p. 281-281 (1997).

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The Isaac Newton Group's CoCam instrument obtained wide-field (10 degx 20 deg) CCD images of the H_2O^+ tail of Hale-Bopp on March 12-15, 19, 20, 25, 28, 29, 31, April 1, 7, 9-13, 21, 23-29 and May 4, 1997. A 6185Å filter recorded the distribution of H_2O^+; 6250Å-centered continuum images were also obtained. Initial analysis has revealed the CoCam dataset to be an invaluable record of the large-scale structure of the comet's ion tail. Several images show evidence of upstream parabolic envelopes of ions reminiscent of those reported in C/1908 R1 Morehouse (Eddington A. S., Mon. Not. Roy. Astron. Soc. 70, 442-458, 1910). Studies of these features may help towards a better understanding of the tail ray phenomenon. During most of March and early April, the tail had a largely consistent quiescent appearance, with numerous rays exhibited, but no major disturbances; most probably as a result of being in the stream of fast polar solar wind. A significant kink propagated down the tail around April 9/10. Towards the end of April, as the comet entered more variable solar wind at near-equatorial heliographic latitudes, the tail's morphology became significantly more structured. Striking tail disturbances were recorded in late April and early May, when the comet was in the vicinity of the heliospheric current sheet. Analysis of the dataset continues.

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