Other
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424..924m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 424, no. 2, p. 924-932
Other
24
Hydrodynamics, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Stellar Winds, Supernova Remnants, Supernova 1987A, X Ray Spectra, Hubble Space Telescope, Iue, Light Curve, Rosat Mission, Shock Waves, Stellar Envelopes, Stellar Luminosity, Stellar Mass
Scientific paper
The progenitor of the supernova 1987A, Sk -69 deg 202, probably had lost a few solar masses in its stellar wind in the past evolutionary track from the red supergiant through the blue supergiant. A part of the mass is thought to form the ringlike nebula surrounding SN 1987A by the interaction with the faster wind in the later blue supergiant stage, and the other must be left outside the ring. In 10-20 yr after the explosion, the expanding ejecta will catch up and collide with the ring. Shocks due to the collision will propagate into and heat up the ejecta, the ring, and the matter outside. The shocked matter will be a thermal X-ray source of temperature of a few 107 K, and the X-ray luminosity will reach (0.4-1) x 1037 ergs/s for the ring of 0.03-0.08 solar masses. The X-ray emission will last for a few decades with luminosity higher than 1036 ergs/s depending also on the density outside the ring. We predict the X-ray spectrum as well as the light curve with hydrodynamical calculations taking into account the light travel effect and the opacity of the unshocked ejecta. The epoch of the flare-up depends on the mass inside the ring, and earlier X-ray observations can give a constraint. We give the resolutions with nonequipartition in the electron and the ion temperatures. Accordingly, the ROSAT observation in 1991 suggests the collision with the ring in 20 yr after the explosion.
Masai Kuniaki
Nomoto Ken'ichi
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