Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/32309
Campo DC | Valore | Lingua |
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dc.contributor.author | Draine, B. T. | en_US |
dc.contributor.author | Li, Aigen | en_US |
dc.contributor.author | Hensley, Brandon S. | en_US |
dc.contributor.author | HUNT, Leslie Kipp | en_US |
dc.contributor.author | Sandstrom, K. | en_US |
dc.contributor.author | Smith, J. D.T. | en_US |
dc.date.accessioned | 2022-06-14T14:28:25Z | - |
dc.date.available | 2022-06-14T14:28:25Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32309 | - |
dc.description.abstract | Using physical models, we study the sensitivity of polycyclic aromatic hydrocarbon (PAH) emission spectra to the character of the illuminating starlight, to the PAH size distribution, and to the PAH charge distribution. The starlight models considered range from the emission from a 3 Myr old starburst, rich in far-ultraviolet (FUV) radiation, to the FUV-poor spectrum of the very old population of the M31 bulge. A wide range of starlight intensities is considered. The effects of reddening in dusty clouds are investigated for different starlight spectra. For a fixed PAH abundance parameter q PAH (the fraction of the total dust mass in PAHs with <103 C atoms), the fraction of the infrared power appearing in the PAH emission features can vary by a factor of two as the starlight spectrum varies from FUV-poor (M31 bulge) to FUV-rich (young starburst). We show how q PAH can be measured from the strength of the 7.7 μm emission. The fractional power in the 17 μm feature can be suppressed by high starlight intensities. | en_US |
dc.language.iso | eng | en_US |
dc.title | Excitation of Polycyclic Aromatic Hydrocarbon Emission: Dependence on Size Distribution, Ionization, and Starlight Spectrum and Intensity | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/abff51 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/abff51 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 917 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 3 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 6 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | USA | 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 | 2021ApJ...917....3D | 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 | 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.cerifentitytype | Publications | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0001-9162-2371 | - |
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