Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/32912
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | PASQUATO, MARIO | en_US |
dc.contributor.author | RAIMONDO, Gabriella | en_US |
dc.contributor.author | BROCATO, Enzo | en_US |
dc.contributor.author | Chung, C. | en_US |
dc.contributor.author | Moraghan, A. | en_US |
dc.contributor.author | Lee, Y. -W. | en_US |
dc.date.accessioned | 2023-01-18T10:39:09Z | - |
dc.date.available | 2023-01-18T10:39:09Z | - |
dc.date.issued | 2013 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32912 | - |
dc.description.abstract | Context. Stellar collision rates in globular clusters (GCs) do not appear to correlate with horizontal branch (HB) morphology, suggesting that dynamics does not play a role in the second-parameter problem. However, core densities and collision rates derived from surface-brightness may be significantly underestimated as the surface-brightness profile of GCs is not necessarily a good indicator of the dynamical state of GC cores. Core-collapse may go unnoticed if high central densities of dark remnants are present. <BR /> Aims: We test whether GC HB morphology data supports a dynamical contribution to the so-called second-parameter effect. <BR /> Methods: To remove first-parameter dependence we fitted the maximum effective temperature along the HB as a function of metallicity in a sample of 54 Milky Way GCs. We plotted the residuals to the fit as a function of second-parameter candidates, namely dynamical age and total luminosity. We considered dynamical age (i.e. the ratio between age and half-light relaxation time) among possible second-parameters. We used a set of direct N-body simulations, including ones with dark remnants to illustrate how core density peaks, due to core collapse, in a dynamical-age range similar to that in which blue HBs are overabundant with respect to the metallicity expectation, especially for low-concentration initial conditions. <BR /> Results: GC total luminosity shows nonlinear behavior compatible with the self-enrichment picture. However, the data are amenable to a different interpretation based on a dynamical origin of the second-parameter effect. Enhanced mass-stripping in the late red-giant-branch phase due to stellar interactions in collapsing cores is a viable candidate mechanism. In this picture, GCs with HBs bluer than expected based on metallicity are those undergoing core-collapse. | en_US |
dc.language.iso | eng | en_US |
dc.title | Core collapse and horizontal-branch morphology in Galactic globular clusters | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201321361 | en_US |
dc.identifier.scopus | 2-s2.0-84879121384 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2013/06/aa21361-13/aa21361-13.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 554 | en_US |
dc.relation.firstpage | A129 | 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 | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2013A&A...554A.129P | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | 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.grantfulltext | open | - |
item.cerifentitytype | Publications | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Abruzzo | - |
crisitem.author.dept | O.A. Abruzzo | - |
crisitem.author.orcid | 0000-0003-3784-5245 | - |
crisitem.author.orcid | 0000-0002-5577-7023 | - |
crisitem.author.orcid | 0000-0001-7988-8177 | - |
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