Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27863
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | BENETTI, Stefano | en_US |
dc.contributor.author | ZAMPIERI, Luca | en_US |
dc.contributor.author | PASTORELLO, Andrea | en_US |
dc.contributor.author | CAPPELLARO, Enrico | en_US |
dc.contributor.author | Pumo, M. L. | en_US |
dc.contributor.author | ELIAS DE LA ROSA, NANCY DEL CARMEN | en_US |
dc.contributor.author | Ochner, P. | en_US |
dc.contributor.author | Terreran, G. | en_US |
dc.contributor.author | TOMASELLA, Lina | en_US |
dc.contributor.author | Taubenberger, S. | en_US |
dc.contributor.author | TURATTO, Massimo | en_US |
dc.contributor.author | Morales-Garoffolo, A. | en_US |
dc.contributor.author | Harutyunyan, A. | en_US |
dc.contributor.author | Tartaglia, L. | en_US |
dc.date.accessioned | 2020-10-16T15:50:01Z | - |
dc.date.available | 2020-10-16T15:50:01Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27863 | - |
dc.description.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. | en_US |
dc.language.iso | eng | en_US |
dc.title | ASASSN-15no: the Supernova that plays hide-and-seek | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty166 | en_US |
dc.identifier.scopus | 2-s2.0-85043509170 | en_US |
dc.identifier.isi | 000429276700021 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/476/1/261/4919569 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 476 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 261 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018MNRAS.476..261B | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0002-3256-0016 | - |
crisitem.author.orcid | 0000-0002-6516-1329 | - |
crisitem.author.orcid | 0000-0002-7259-4624 | - |
crisitem.author.orcid | 0000-0001-5008-8619 | - |
crisitem.author.orcid | 0000-0002-1381-9125 | - |
crisitem.author.orcid | 0000-0002-3697-2616 | - |
crisitem.author.orcid | 0000-0002-9719-3157 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
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