The Progenitors of Type I SNe

Details The Progenitors of Type I SNe The Progenitors of Type I SNe

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..391..347m&link_type=abstract

Hydrogen-Deficient Stars ASP Conference Series, Vol. 391, proceedings of the conference held 17-21 September, 2007, at Eberhard

Physics

Scientific paper

Supernovae of Type I are deprived of hydrogen and rich in heavy elements, and share the same physics of light curve and spectrum formation: continuum processes are unimportant compared to line-blocking, especially in the UV. An analysis of their spectra and light curves yields insights into the explosion mechanism. SNe Ia, the thermonuclear explosions of white dwarfs accreting mass to reach the Chandrasekhar limit, have homogeneous properties and are used as standardized candles, but the reason for this is only now beginning to emerge. SNe Ib and Ic result from the explosion following the core collapse of massive stars that had lost their outer envelope. SNe Ib are rich in He, while SNe Ic are not, suggesting that they are caused by the collapse of bare CO cores. SNe Ic show a wide range of properties. The most massive and energetic SNe Ic are linked to Gamma Ray Bursts. Additionally, signatures of strong asphericities can be deduced from their late-time spectra and from polarisation. Such asphericities may be common to all core-collapse SNe. The exact nature of the progenitors of these SNe remains unclear.

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