ACCELERATING VERY FAST GAS IN THE SUPERNOVA IMPOSTOR SN 2009ip WITH JETS FROM A STELLAR COMPANION

Abstract

Using hydrodynamic numerical simulations we show that high-velocity ejecta with v ∼ 10 4 km s −1 in the outbursts of the supernova impostor SN 2009ip and similar luminous blue variable (LBV) stars can be explained by the interaction of fast jets, having v jet ∼ 2000-3000 km s −1 , with a circumbinary shell (extended envelope). The density profile in the shell is very steep such that the shock wave, that is excited by the jets' interaction with the shell, accelerates to high velocities as it propagates outward. The amount of very fast ejecta is small, but sufficient to account for some absorption lines. Such an extended envelope can be formed from the binary interaction and/or the unstable phase of the LBV primary star. The jets themselves are launched by the more compact secondary star near periastron passages.

Spectropolarimetry of the 2012 outburst of SN 2009ip: a bi-polar explosion in a dense, disc-like CSM

“…The polarimetry is indicative of a bipolar explosion for the 2012 outbursts, consistent with the predictions of the non-terminal binary interaction models of , Kashi et al (2013) and Tsebrenko & Soker (2013). The predicted geometry of SN 2009ip also fits in quite well with the bipolar structure commonly observed in LBV nebulae (Weis 2003).…”

“…A somewhat natural explanation for asymmetry in pre-existing CSM would be interaction with a binary companion. , Kashi et al (2013) and Tsebrenko & Soker (2013) have discussed the outbursts of SN 2009ip in the context of binary interaction between an LBV and a more compact companion which is proposed to launch jets upon accretion from the more massive object. Such interactions in the pre-explosion system could lead to a bipolar arrangement for the CSM (Mcley & Soker 2014).…”

Supernovae 2016bdu and 2005gl, and their link with SN 2009ip-like transients: another piece of the puzzle

“…This scenario has also been suggested by and Soker & Kashi (2016) for SNe 2009ip, 2010mc, and 2015bh (see also Sana et al 2012;de Mink et al 2014;Justham, Podsiadlowski & Vink 2014;Portegies Zwart & van den Heuvel 2016, for a discussion of massive stellar mergers including LBVs). In these massive binary systems, formed by an LBV and a more compact companion, the high-velocity gas outflow seen in the spectra of both SN 2009ip and SN 2015bh during the impostor phase (hence months to years before Event A) would be powered by jets from the secondary star (Tsebrenko & Soker 2013). Goranskij et al (2016) proposed a hybrid explanation for SN 2015bh, with the core collapse of an evolved massive star while merging with a massive binary companion.…”

Recovery From Giant Eruptions in Very Massive Stars

“…An example with a more complex history is SN2009ip. In 2009 it experienced a giant eruption initially labeled a SN event; but then a series of later outbursts arose in 2011-2012, leaving researchers uncertain about whether the terminal event had finally occurred or not (Drake et al 2012;Fraser et al 2013; Kashi et al 2013;Mauerhan et al 2013Mauerhan et al , 2014Pastorello et al 2013;Prieto et al 2013;Tsebrenko & Soker 2013;Graham et al 2014;Margutti et al 2014).…”