Volume 635, March 2020
|Number of page(s)||7|
|Published online||31 March 2020|
White dwarf deflagrations for Type Iax supernovae: polarisation signatures from the explosion and companion interaction
Nordita, KTH Royal Institute of Technology and Stockholm University,
106 91 Stockholm,
2 Yunnan Observatories, Chinese Academy of Sciences (CAS), Kunming 650216, PR China
3 Key Laboratory for thea Structure and Evolution of Celestial Objects, CAS, Kunming 650216, PR China
4 Center for Astronomical Mega-Science, CAS, Beijing 100012, PR China
5 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Philosophenweg 12, 69120 Heidelberg, Germany
6 Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany
7 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, BT7 1NN, UK
8 Institut für Theoretische Physik und Astrophysik, Universität Würzburg, Emil-Fischer-Straße 31, 97074 Würzburg, Germany
9 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
10 School of Science, University of New South Wales, Australian Defence Force Academy, Northcott Drive, Canberra, ACT 2600, Australia
Accepted: 25 February 2020
Growing evidence suggests that Type Iax supernovae might be the result of thermonuclear deflagrations of Chandrasekhar-mass white dwarfs in binary systems. We carry out Monte Carlo radiative transfer simulations and predict spectropolarimetric features originating from the supernova explosion and subsequent ejecta interaction with the companion star. Specifically, we calculate viewing-angle dependent flux and polarisation spectra for a 3D model simulating the deflagration of a Chandrasekhar-mass white dwarf and, for a second model, simulating the ejecta interaction with a main-sequence star. We find that the intrinsic signal is weakly polarised and only mildly viewing-angle dependent, owing to the overall spherical symmetry of the explosion and the depolarising contribution of iron-group elements dominating the ejecta composition. The interaction with the companion star carves out a cavity in the ejecta and produces a detectable, but modest signal that is significant only at relatively blue wavelengths (≲5000 Å). In particular, increasingly fainter and redder spectra are predicted for observer orientations further from the cavity, while a modest polarisation signal P ~ 0.2 per cent is found at blue wavelengths for orientations 30° and 45° away from the cavity. We find a reasonable agreement between the interaction model viewed from these orientations and spectropolarimetric data of SN 2005hk and interpret the maximum-light polarisation signal seen at blue wavelengths for this event as a possible signature of the ejecta–companion interaction. We encourage further polarimetric observations of SNe Iax to test whether our results can be extended and generalised to the whole SN Iax class.
Key words: hydrodynamics / radiative transfer / polarization / methods: numerical / supernovae: general / supernovae: individual: SN 2005hk
© ESO 2020
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