Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30214
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Grefenstette, Brian W. | en_US |
dc.contributor.author | Fryer, Chris L. | en_US |
dc.contributor.author | Harrison, Fiona A. | en_US |
dc.contributor.author | Boggs, Steven E. | en_US |
dc.contributor.author | DeLaney, Tracey | en_US |
dc.contributor.author | Laming, J. Martin | en_US |
dc.contributor.author | Reynolds, Stephen P. | en_US |
dc.contributor.author | Alexander, David M. | en_US |
dc.contributor.author | Barret, Didier | en_US |
dc.contributor.author | Christensen, Finn E. | en_US |
dc.contributor.author | Craig, William W. | en_US |
dc.contributor.author | Forster, Karl | en_US |
dc.contributor.author | Giommi, Paolo | en_US |
dc.contributor.author | Hailey, Charles J. | en_US |
dc.contributor.author | Hornstrup, Alan | en_US |
dc.contributor.author | Kitaguchi, Takao | en_US |
dc.contributor.author | Koglin, J. E. | en_US |
dc.contributor.author | Lopez, Laura | en_US |
dc.contributor.author | Mao, Peter H. | en_US |
dc.contributor.author | Madsen, Kristin K. | en_US |
dc.contributor.author | Miyasaka, Hiromasa | en_US |
dc.contributor.author | Mori, Kaya | en_US |
dc.contributor.author | PERRI, Matteo | en_US |
dc.contributor.author | Pivovaroff, Michael J. | en_US |
dc.contributor.author | Puccetti, Simonetta | en_US |
dc.contributor.author | Rana, Vikram | en_US |
dc.contributor.author | Stern, Daniel | en_US |
dc.contributor.author | Westergaard, Niels J. | en_US |
dc.contributor.author | Wik, Daniel R. | en_US |
dc.contributor.author | Zhang, William W. | en_US |
dc.contributor.author | Zoglauer, Andreas | en_US |
dc.date.accessioned | 2021-02-05T14:21:42Z | - |
dc.date.available | 2021-02-05T14:21:42Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30214 | - |
dc.description.abstract | The distribution of elements produced in the innermost layers of a supernova explosion is a key diagnostic for studying the collapse of massive stars. Here we present the results of a 2.4 Ms NuSTAR observing campaign aimed at studying the supernova remnant Cassiopeia A (Cas A). We perform spatially resolved spectroscopic analyses of the Ti-44 ejecta, which we use to determine the Doppler shift and thus the three-dimensional (3D) velocities of the Ti-44 ejecta. We find an initial Ti-44 mass of (1.54 ± 0.21) × 10^-4 M_☉, which has a present-day average momentum direction of 340° ± 15° projected onto the plane of the sky (measured clockwise from celestial north) and is tilted by 58° ± 20° into the plane of the sky away from the observer, roughly opposite to the inferred direction of motion of the central compact object. We find some Ti-44 ejecta that are clearly interior to the reverse shock and some that are clearly exterior to it. Where we observe Ti-44 ejecta exterior to the reverse shock we also see shock-heated iron; however, there are regions where we see iron but do not observe Ti-44. This suggests that the local conditions of the supernova shock during explosive nucleosynthesis varied enough to suppress the production of Ti-44 by at least a factor of two in some regions, even in regions that are assumed to be the result of processes like α-rich freezeout that should produce both iron and titanium. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Distribution of Radioactive 44Ti in Cassiopeia A | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/834/1/19 | en_US |
dc.identifier.scopus | 2-s2.0-85010204726 | en_US |
dc.identifier.isi | 000391871500007 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/834/1/19 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 834 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 19 | 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 | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...834...19G | 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_10 High energy and particle astronomy – X-rays, cosmic rays, gamma rays, neutrinos | 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. Roma | - |
crisitem.author.orcid | 0000-0003-3613-4409 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Grefenstette_2017_ApJ_834_19.pdf | Pdf editoriale | 2.62 MB | Adobe PDF | View/Open |
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