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Raffaella Margutti edited section_Introduction__.tex
over 8 years ago
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\section{Introduction}
Observations are painting a complex picture of massive stars at the end of their lives. Contrary to expectations, massive stars have been found to experience major eruptions in the years preceding their explosion as supernovae (SNe). This sequence of eruptions was \emph{not predicted} on theoretical grounds and is \emph{not explained} by our current understanding of the physical mechanisms that drive the mass loss in evolved massive stars (Smith 2014).
In this respect, two key observational findings are relevant: (i) The direct detection of luminous precursors in the month before the
major explosion of SN2009ip associated with the ejection of $\sim0.1\,\rm{M_{\odot}}$ of material (Margutti et al., 2014). (ii) Evidence for significant modulations in the radio light-curves of hydrogen-stripped SNe (i.e. SNe Ib/c; Soderberg et al., 2006, Milisavljevic et al., 2013). This latter finding indicates that a complex environment, sculpted and enriched by a significantly \emph{non-steady} mass loss of the progenitor system in the years before the explosion, surrounds some Type Ib/c SNe.
