The Rings of SN87A: Rotation and a Binary Companion

Details The Rings of SN87A: Rotation and a Binary Companion The Rings of SN87A: Rotation and a Binary Companion

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.4015c&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #40.15; Bulletin of the American Astronomical Society, Vol. 29, p.1269

Astronomy and Astrophysics

Astronomy

Scientific paper

In this poster we address the origin of the bipolar nebula surrounding Supernova 1987A and the possibility of a binary companion for the progenitor. Our model for the formation of the bipolar bubble is the popular interacting stellar winds scenario. This model assumes that a fast, spherically symmetric wind emanating from the central blue giant star interacted with a toroidal shaped wind expelled during the red giant phase. The new addition in our model is the use of the Wind Compressed Disk model of Bjorkman & Cassinelli 1994 where rotation of the Red Giant forces streamlines towards the equator forming a dense "excretion" disk. The fast blue star wind expands into this disk producing the central ring and bipolar lobes. Using a self-similar analytic model we determine the stellar rotation rate needed to produce a bipolar bubble with properties similar to that observed around Supernova 1987A. Inferences about the presence of a binary companion may be possible from these results.

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