{ "id": "2305.03363", "version": "v1", "published": "2023-05-05T08:31:24.000Z", "updated": "2023-05-05T08:31:24.000Z", "title": "Early excess emission in Type Ia supernovae from the interaction between supernova ejecta and their circumstellar wind", "authors": [ "Takashi J. Moriya", "Paolo A. Mazzali", "Chris Ashall", "Elena Pian" ], "comment": "8 pages, 8 figures, accepted by Monthly Notices of the Royal Astronomical Society", "categories": [ "astro-ph.HE", "astro-ph.SR" ], "abstract": "The effects of the interaction between Type Ia supernova ejecta and their circumstellar wind on the photometric properties of Type Ia supernovae are investigated. We assume that a hydrogen-rich, dense, and extended circumstellar matter (CSM) is formed by the steady mass loss of their progenitor systems. The CSM density is assumed to be proportional to r^{-2}. When the mass-loss rate is above 1e-4 Msun/yr with a wind velocity of 100 km/s, CSM interaction results in an early flux excess in optical light-curves within 4 days of explosion. In these cases, the optical colour quickly evolves to the blue. The ultraviolet flux below 3000 A is found to have a persistent flux excess compared to Type Ia supernovae as long as CSM interaction continues. Type Ia supernovae with progenitor mass-loss rates between 1e-4 and 1e-3 Msun/yr may not have a CSM that is dense enough to affect spectra to make them Type Ia-CSM, but they may still result in Type Ia supernovae with an early optical flux excess. Because they have a persistent ultraviolet flux excess, ultraviolet light curves around the luminosity peak would be significantly different from those with a low-density CSM.", "revisions": [ { "version": "v1", "updated": "2023-05-05T08:31:24.000Z" } ], "analyses": { "keywords": [ "early excess emission", "circumstellar wind", "type ia supernova ejecta", "persistent ultraviolet flux excess", "mass-loss rate" ], "note": { "typesetting": "TeX", "pages": 8, "language": "en", "license": "arXiv", "status": "editable" } } }