2006/08/21 by Н. Н. Чугай, N. N. Chugai · 37 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Asymmetry #Ejecta #Gamma-ray bursts and supernovae #Optics #Physics #Polarization (electrochemistry) #Radiation #Supernova #astro-ph
paper · pdf · doi:10.1134/s1063773706110041
published in Astronomy Letters 32(11), 739-746 (Pleiades Publishing) · 9 pages, 7 figures, to appear in Astronomy Letters
arxiv created 2006/08/21 · openalex publication_date 2006/10/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
I study the question of whether the asymmetry of 56 Ni ejecta that results in the asymmetry of the H α emission line at the nebular epoch of the type-IIP supernova SN 2004dj can account for the recently detected polarization of the supernova radiation. I have developed a model of the H α profile and luminosity with nonthermal ionization and excitation in a spherically symmetric envelope for an asymmetric bipolar 56 Ni distribution. I have calculated the polarized radiation transfer against the background of the recovered electron density distribution. The observed polarization is shown to be reproduced at the nebular epoch around day 140 for the same parameters of the envelope, and the 56 Ni distribution for which the evolution of the H α luminosity and profile is explained. Yet the model polarization decreases with time more slowly than is observed. The origin of the additional component responsible for the early polarization on day 107 is discussed.