Quark nova imprint in the extreme supernova explosion SN 2006gy

Abstract

The extremely luminous supernova 2006gy (SN 2006gy) is among the most energetic ever observed. The peak brightness was 100 times that of a typical supernova and it spent an unheard of 250 days at magnitude -19 or brighter. Efforts to describe SN 2006gy have pushed the boundaries of current supernova theory. In this work we aspire to simultaneously reproduce the photometric and spectroscopic observations of SN 2006gy using a quark nova model. This analysis considers the supernova explosion of a massive star followed days later by the quark nova detonation of a neutron star. We lay out a detailed model of the interaction between the supernova envelope and the quark nova ejecta paying special attention to a mixing region which forms at the inner edge of the supernova envelope. This model is then fit to photometric and spectroscopic observations of SN 2006gy. This QN model naturally describes several features of SN 2006gy including the late stage light curve plateau, the broad H{\alpha} line and the peculiar blue H{\alpha} absorption. We find that a progenitor mass between 20Msun and 40Msun provides ample energy to power SN 2006gy in the context of a QN.Comment: 15 pages, 9 figure

Spallation Model for the Titanium-Rich Supernova Remnant Cassiopeia A

“…If the QN occurs less than a few weeks after the SN, the QN energy release reheats the preceding SN ejecta, and results in an event we call a dual-shock quark nova (dsQN). In previous papers, we introduced the dsQN as a model for superluminous SNe [15] and discussed their photometric and spectroscopic [16] signatures. Here, for the first time, we explore the nuclear processing of the innermost SN ejecta by the QN relativistic ejecta (neutrons and heavy nuclei).…”

Properties of Magnetars Mimicking 56Ni-Powered Light Curves in Type IC Superluminous Supernovae

“…However, subsequent theoretical and observational studies suggest that the short LC rise times and little line blanketing of slowly-declining Type Ic SLSNe like SN 2007bi are inconsistent with 56 Ni-powered PISNe and prefer the magnetar-powered model (e.g., Dessart et al 2012;Inserra et al 2013;Nicholl et al 2013Nicholl et al , 2015bNicholl et al , 2016aMcCrum et al 2014;Chen et al 2015;Jerkstrand et al 2016a,b;Mazzali et al 2016) or other power sources (e.g., Chevalier & Irwin 2011;Ginzburg & Balberg 2012;Moriya & Maeda 2012;Ouyed et al 2012;Chatzopoulos et al 2013b;Dexter & Kasen 2013;Baklanov et al 2015;Sorokina et al 2016;Nicholl et al 2015a;Wang et al 2016). In addition, there also exist many Type Ic SLSNe with fast LC declines that cannot be explained by the 56 Ni power (e.g., Pastorello et al 2010;Chomiuk et al 2011;Inserra et al 2013;Howell et al 2013;Nicholl et al 2015b).…”

r-Java: anr-process code and graphical user interface for heavy-element nucleosynthesis

“…Since the half-life of tritium is relatively short (12.32 years), a large amount of its daughter element, He-3, would be formed and dispelled into the surrounding space. In the case of a dual-shock Quark-Nova (Leahy & Ouyed 2008;Ouyed et al 2010), this can have important consequences, through spallation on supernova ejecta, for cosmic rays and anomalous abundance ratios in some supernovae (e.g., Cas A).…”