Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/31598
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Miceli, Marco | en_US |
dc.contributor.author | ORLANDO, Salvatore | en_US |
dc.contributor.author | Burrows, David N. | en_US |
dc.contributor.author | Frank, Kari A. | en_US |
dc.contributor.author | Argiroffi, Costanza | en_US |
dc.contributor.author | Reale, Fabio | en_US |
dc.contributor.author | Peres, Giovanni | en_US |
dc.contributor.author | PETRUK, Oleh | en_US |
dc.contributor.author | BOCCHINO, Fabrizio | en_US |
dc.date.accessioned | 2022-03-15T16:18:41Z | - |
dc.date.available | 2022-03-15T16:18:41Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 2397-3366 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31598 | - |
dc.description.abstract | Astrophysical shocks at all scales, from those in the heliosphere up to cosmological shock waves, are typically `collisionless', because the thickness of their jump region is much shorter than the collisional mean free path. Across these jumps, electrons, protons and ions are expected to be heated at different temperatures. Supernova remnants (SNRs) are ideal targets to study collisionless processes because of their bright post-shock emission and fast shocks, but the actual dependence of the post-shock temperature on the particle mass is still widely debated<SUP>1</SUP>. We tackle this longstanding issue through the analysis of deep multi-epoch and high-resolution observations, made with the Chandra X-ray telescope, of the youngest nearby supernova remnant, SN 1987A. We introduce a data analysis method by studying the observed spectra in close comparison with a dedicated full three-dimensional hydrodynamic simulation that self-consistently reproduces the broadening of the spectral lines of many ions together. We measure the post-shock temperature of protons and ions through comparison of the model with observations. Our results show that the ratio of ion temperature to proton temperature is always significantly higher than one and increases linearly with the ion mass for a wide range of masses and shock parameters. | en_US |
dc.language.iso | eng | en_US |
dc.title | Collisionless shock heating of heavy ions in SN 1987A | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1038/s41550-018-0677-8 | en_US |
dc.identifier.scopus | 2-s2.0-85062678146 | en_US |
dc.identifier.isi | WOS:000460567100015 | en_US |
dc.identifier.url | https://www.nature.com/articles/s41550-018-0677-8 | en_US |
dc.relation.medium | ELETTRONICO | en_US |
dc.relation.volume | 3 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 236 | en_US |
dc.relation.lastpage | 241 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 9 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | UKR | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | NATURE ASTRONOMY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019NatAs...3..236M | 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. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.orcid | 0000-0003-0876-8391 | - |
crisitem.author.orcid | 0000-0003-2836-540X | - |
crisitem.author.orcid | 0000-0003-2073-1348 | - |
crisitem.author.orcid | 0000-0002-1820-4824 | - |
crisitem.author.orcid | 0000-0002-6033-8180 | - |
crisitem.author.orcid | 0000-0002-2321-5616 | - |
crisitem.journal.journalissn | 2397-3366 | - |
crisitem.journal.ance | E240167 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
---|---|---|---|---|
1901.10336.pdf | preprint | 425.49 kB | Adobe PDF | Visualizza/apri |
s41550-018-0677-8.pdf | [Administrators only] | 1.94 MB | Adobe PDF |
Page view(s)
43
controllato il 20-apr-2024
Download(s)
11
controllato il 20-apr-2024
Google ScholarTM
Check
Altmetric
Altmetric
Tutti i documenti in DSpace sono pubblicati ad Accesso Aperto, salvo diversa indicazione per alcuni documenti specifici.