Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30438
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Dalessandro, Emanuele | en_US |
dc.contributor.author | Cadelano, M. | en_US |
dc.contributor.author | Vesperini, E. | en_US |
dc.contributor.author | Salaris, M. | en_US |
dc.contributor.author | Ferraro, F. R. | en_US |
dc.contributor.author | Lanzoni, B. | en_US |
dc.contributor.author | Raso, S. | en_US |
dc.contributor.author | Hong, J. | en_US |
dc.contributor.author | Webb, J. J. | en_US |
dc.contributor.author | Zocchi, A. | en_US |
dc.date.accessioned | 2021-02-17T15:51:05Z | - |
dc.date.available | 2021-02-17T15:51:05Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30438 | - |
dc.description.abstract | We present a detailed analysis of the radial distribution of light-element multiple populations (LE-MPs) in the massive and dense globular cluster M80, based on a combination of UV and optical Hubble Space Telescope data. Surprisingly, we find that first-generation (FG) stars (FG) are significantly more centrally concentrated than extreme second-generation (SG) stars out to ˜2.5r h from the cluster center. To understand the origin of such peculiar behavior, we used a set of N-body simulations following the long-term dynamical evolution of LE-MPs. We find that, given the advanced dynamical state of the cluster, the observed difference does not depend on the primordial relative distributions of FG and SG stars. On the contrary, a difference of ˜0.05-0.10 M ⊙ between the average masses of the two subpopulations is needed to account for the observed radial distributions. We argue that such a mass difference might be the result of the higher He abundance of SG stars (of the order of ΔY ˜ 0.05-0.06) with respect to FG stars. Interestingly, we find that a similar He variation is necessary to reproduce the horizontal branch morphology of M80. These results demonstrate that differences in mass among LE-MPs, due to different He content, should be properly taken into account for a correct interpretation of their radial distribution, at least in dynamically evolved systems. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Peculiar Radial Distribution of Multiple Populations in the Massive Globular Cluster M80 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aabb56 | en_US |
dc.identifier.scopus | 2-s2.0-85047979810 | en_US |
dc.identifier.isi | 000432540700005 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aabb56 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 859 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 15 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 10 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | CAN | en_US |
dc.contributor.country | NLD | 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...859...15D | 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.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 | OAS Bologna | - |
crisitem.author.orcid | 0000-0003-4237-4601 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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