An Analysis of the Peculiar Type IIn Supernova 1995N

Details An Analysis of the Peculiar Type IIn Supernova 1995N An Analysis of the Peculiar Type IIn Supernova 1995N

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.4704b&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #47.04; Bulletin of the American Astronomical Society, Vol. 30, p.1323

Astronomy and Astrophysics

Astronomy

3

Scientific paper

SN 1995N is a peculiar type IIn supernova. Spectroscopic and photometric data for this analysis were gathered between May 10, 1995 (two days after discovery) and July 18, 1998. A total of twenty two photometric images and eight spectra were obtained at the FLWO and MMTO. The photometric data show a broad maximum at R=17.0 occurred in late October, 1995, followed by a very slow decline at a rate of 2.39 millimag-day(-1) for R and 1.37 millimag-day(-1) for V. The R decay rate corresponds to a half life of 315 days, which is much longer than that of (56) Co. The spectra show broad hydrogen (1500 km/s FWHM) and oxygen (10000 km/s FWZI) emission features along with many unresolved emission lines. Some of the more interesting narrow lines identified correspond to high ionization states for iron such as Fe VII and Fe X which indicate temperatures as high as 10(6) degrees K. These high ionization states, the X-ray detection by Lewin et al. (1996, IAUC 6445) and the slow photometric decay suggest that SN 1995N is powered by a shock propagating through a dense circumstellar environment. From the earliest observations the energy output appears dominated by the interaction and not by radioactivity, implying that the progenitor exploded well before the discovery of SN 1995N. The situation may be similar to SN 1987A, where the rise in emission from a circumstellar interaction is only now beginning and is expected to peak some 15 years after the supernova explosion.

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