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http://hdl.handle.net/20.500.12386/27863
Title: | ASASSN-15no: the Supernova that plays hide-and-seek | Authors: | BENETTI, Stefano ZAMPIERI, Luca PASTORELLO, Andrea CAPPELLARO, Enrico Pumo, M. L. ELIAS DE LA ROSA, NANCY DEL CARMEN Ochner, P. Terreran, G. TOMASELLA, Lina Taubenberger, S. TURATTO, Massimo Morales-Garoffolo, A. Harutyunyan, A. Tartaglia, L. |
Issue Date: | 2018 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 476 | Issue: | 1 | First Page: | 261 | Abstract: | We report the results of our follow-up campaign of the peculiar supernova ASASSN-15no, based on optical data covering ∼300 d of its evolution. Initially the spectra show a pure blackbody continuum. After few days, the HeI λλ 5876 transition appears with a P-Cygni profile and an expansion velocity of about 8700 km s<SUP>-1</SUP>. Fifty days after maximum, the spectrum shows signs typically seen in interacting supernovae. A broad (FWHM ∼ 8000 km s<SUP>-1</SUP>) Hα becomes more prominent with time until ∼150 d after maximum and quickly declines later on. At these phases Hαstarts to show an intermediate component, which together with the blue pseudo-continuum are clues that the ejecta begin to interact with the circumstellar medium (CSM). The spectra at the latest phases look very similar to the nebular spectra of stripped-envelope SNe. The early part (the first 40 d after maximum) of the bolometric curve, which peaks at a luminosity intermediate between normal and superluminous supernovae, is well reproduced by a model in which the energy budget is essentially coming from ejecta recombination and <SUP>56</SUP>Ni decay. From the model, we infer a mass of the ejecta M<SUB>ej</SUB> = 2.6 M<SUB>☉</SUB>; an initial radius of the photosphere R<SUB>0</SUB> = 2.1 × 10<SUP>14</SUP> cm; and an explosion energy E<SUB>expl</SUB> = 0.8 × 10<SUP>51</SUP> erg. A possible scenario involves a massive and extended H-poor shell lost by the progenitor star a few years before explosion. The shell is hit, heated, and accelerated by the supernova ejecta. The accelerated shell+ejecta rapidly dilutes, unveiling the unperturbed supernova spectrum below. The outer ejecta start to interact with a H-poor external CSM lost by the progenitor system about 9-90 yr before the explosion. | URI: | http://hdl.handle.net/20.500.12386/27863 | URL: | https://academic.oup.com/mnras/article/476/1/261/4919569 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/sty166 | Bibcode ADS: | 2018MNRAS.476..261B | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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ASASSN15no.pdf | PDF editoriale | 1.45 MB | Adobe PDF | View/Open |
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