SN 2009ip and SN 2010mc: core-collapse Type IIn supernovae arising from blue supergiants

作者：Smith Nathan^*; Mauerhan Jon C; Prieto Jose L

来源：Monthly Notices of the Royal Astronomical Society, 2014, 438(2): 1191-1207.

DOI：10.1093/mnras/stt2269

• circumstellar matter
• stars: evolution
• supernovae: general
• supernovae: individual: SN 2009ip
• supernovae: individual: SN 2010mc
• stars: winds, outflows

The recent supernova (SN) known as SN 2009ip had dramatic precursor eruptions followed by an even brighter explosion in 2012. Its pre-2012 observations make it the best documented SN progenitor in history, but have fuelled debate about the nature of its 2012 explosion whether it was a true SN or some type of violent non-terminal event. Both could power shock interaction with circumstellar material (CSM), but only a core-collapse SN provides a self-consistent explanation. The persistent broad emission lines in the spectrum require a relatively large ejecta mass, and a corresponding kinetic energy of at least 1051 erg, while the faint 2012a event is consistent with published models of core-collapse SNe from compact (similar to 60 R-circle dot) blue supergiants. The light curves of SN 2009ip and another Type IIn, SN 2010mc, were nearly identical; we demonstrate that their spectra match as well, and that both are standard SNe IIn. Our observations contradict the recent claim that the late-time spectrum of SN 2009ip is returning to its progenitor's luminous blue variable-like state, and we show the that late-time spectra of SN 2009ip closely resemble the spectra of SN 1987A. Moreover, SN 2009ip's changing H alpha equivalent width after explosion matches behaviour typically seen in core-collapse SNe IIn. Several key facts about SN 2009ip and SN 2010mc argue strongly in favour of a core-collapse interpretation, and make a non-terminal 10(50) erg event implausible. The most straightforward and self-consistent interpretation is that SN 2009ip was an initially faint core-collapse explosion of a blue supergiant that produced about half as much Ni-56 as SN 1987A, with most of the peak luminosity from CSM interaction.

• 出版日期2014-2