Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27863
DC Field | Value | Language |
---|---|---|
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 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
ASASSN15no.pdf | PDF editoriale | 1.45 MB | Adobe PDF | View/Open |
Page view(s)
68
checked on Apr 23, 2024
Download(s)
26
checked on Apr 23, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.