Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27523
Campo DC | Valore | Lingua |
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dc.contributor.author | Bose, Subhash | en_US |
dc.contributor.author | Dong, Subo | en_US |
dc.contributor.author | Kochanek, C. S. | en_US |
dc.contributor.author | PASTORELLO, Andrea | en_US |
dc.contributor.author | Katz, Boaz | en_US |
dc.contributor.author | Bersier, David | en_US |
dc.contributor.author | Andrews, Jennifer E. | en_US |
dc.contributor.author | Prieto, J. L. | en_US |
dc.contributor.author | Stanek, K. Z. | en_US |
dc.contributor.author | Shappee, B. J. | en_US |
dc.contributor.author | Smith, Nathan | en_US |
dc.contributor.author | Kollmeier, Juna | en_US |
dc.contributor.author | BENETTI, Stefano | en_US |
dc.contributor.author | CAPPELLARO, Enrico | en_US |
dc.contributor.author | Chen, Ping | en_US |
dc.contributor.author | ELIAS DE LA ROSA, NANCY DEL CARMEN | en_US |
dc.contributor.author | Milne, Peter | en_US |
dc.contributor.author | Morales-Garoffolo, Antonia | en_US |
dc.contributor.author | TARTAGLIA, LEONARDO | en_US |
dc.contributor.author | TOMASELLA, Lina | en_US |
dc.contributor.author | Bilinski, Christopher | en_US |
dc.contributor.author | Brimacombe, Joseph | en_US |
dc.contributor.author | Frank, Stephan | en_US |
dc.contributor.author | Holoien, T. W. -S. | en_US |
dc.contributor.author | Kilpatrick, Charles D. | en_US |
dc.contributor.author | Kiyota, Seiichiro | en_US |
dc.contributor.author | Madore, Barry F. | en_US |
dc.contributor.author | Rich, Jeffrey A. | en_US |
dc.date.accessioned | 2020-09-29T10:54:05Z | - |
dc.date.available | 2020-09-29T10:54:05Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27523 | - |
dc.description.abstract | We report a luminous Type II supernova, ASASSN-15nx, with a peak luminosity of {M}<SUB>V</SUB>=-20 mag that is between those of typical core-collapse supernovae and super-luminous supernovae. The post-peak optical light curves show a long, linear decline with a steep slope of 2.5 mag (100 day)<SUP>-1</SUP> (i.e., an exponential decline in flux) through the end of observations at phase ≈ 260 {day}. In contrast, the light curves of hydrogen-rich supernovae (SNe II-P/L) always show breaks in their light curves at phase ∼100 day, before settling onto <SUP>56</SUP>Co radioactive decay tails with a decline rate of about 1 mag (100 day)<SUP>-1</SUP>. The spectra of ASASSN-15nx do not exhibit the narrow emission-line features characteristic of Type IIn SNe, which can have a wide variety of light-curve shapes usually attributed to strong interactions with a dense circumstellar medium (CSM). ASASSN-15nx has a number of spectroscopic peculiarities, including a relatively weak and triangular-shaped Hα emission profile with no absorption component. The physical origin of these peculiarities is unclear, but the long and linear post-peak light curve without a break suggests a single dominant powering mechanism. Decay of a large amount of {}<SUP>56</SUP>{Ni} (M <SUB>Ni</SUB> = 1.6 ± 0.2 {M}<SUB>☉ </SUB>) can power the light curve of ASASSN-15nx, and the steep light-curve slope requires substantial γ-ray escape from the ejecta, which is possible given a low-mass hydrogen envelope for the progenitor. Another possibility is strong CSM interactions powering the light curve, but the CSM needs to be sculpted to produce the unique light-curve shape and avoid producing SN IIn-like narrow emission lines. | en_US |
dc.language.iso | eng | en_US |
dc.title | ASASSN-15nx: A Luminous Type II Supernova with a “Perfect” Linear Decline | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aacb35 | en_US |
dc.identifier.scopus | 2-s2.0-85051843507 | en_US |
dc.identifier.isi | 000440045800008 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aacb35 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 862 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 107 | en_US |
dc.relation.numberofpages | 19 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 25 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018ApJ...862..107B | 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. Abruzzo | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0002-7259-4624 | - |
crisitem.author.orcid | 0000-0002-3256-0016 | - |
crisitem.author.orcid | 0000-0001-5008-8619 | - |
crisitem.author.orcid | 0000-0002-1381-9125 | - |
crisitem.author.orcid | 0000-0003-3433-1492 | - |
crisitem.author.orcid | 0000-0002-3697-2616 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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