Host Galaxy Effects in the Susy Model for Supernovae Ia

TL;DR

This paper explores how host galaxy effects can inform the susy phase transition model for Type Ia supernovae, challenging traditional binary star models and offering new insights into supernova mechanisms and cosmological relations.

Contribution

It introduces a susy phase transition model for SN Ia, linking host galaxy effects to the explosion mechanism and providing predictions that differ from binary star models.

Findings

Host galaxy effects can be explained by the susy phase transition model.

The model predicts specific host galaxy correlations for SN Ia.

Discussion of a susy perspective on the Phillips relation.

Abstract

For more than forty years virtually all work on the theory of type Ia Supernovae (SN Ia) has assumed that these explosions were due to the transfer of mass to a degenerate star from a partner in a binary system. In these binary models, when the mass of one partner closely approaches the Chandrasekhar maximum for a stable degenerate system, fusion can be initiated and the star explodes. However, there are now a number of indications that fusion could instead be triggered by a phase transition in a sub-Chandrasekhar white dwarf star. Although these indications provide no clue as to what specific phase transition initiates the explosion, it is possible that remarkable and well established host galaxy effects as considered in the present work could point to a specific source of the energy deposition. These host galaxy correlations are, at first glance, surprising since the typical distance scale of white dwarf stars is the earth radius while the typical distance between stars is at the light year scale. Performing a least $\chi^2$ fit to the delay time distribution to fix parameters, we give predictions from the susy phase transition model for the host galaxy effects. In addition we discuss a susy insight into the Phillips relation which is basic to the cosmological importance of the type Ia supernovae.