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dc.rights.licenseCopyright © 2020, Oxford University Press-
dc.contributor.authorBestenlehner, J. M.-
dc.contributor.authorCrowther, P. A.-
dc.contributor.authorCaballero Nieves, S. M.-
dc.contributor.authorSchneider, F. R. N.-
dc.contributor.authorSimón Díaz, S.-
dc.contributor.authorBrands, S. A.-
dc.contributor.authorDe Koter, A.-
dc.contributor.authorGräfener, G.-
dc.contributor.authorHerrero, A.-
dc.contributor.authorLanger, N.-
dc.contributor.authorLennon, D. J.-
dc.contributor.authorMaíz Apellániz, J.-
dc.contributor.authorPuls, J.-
dc.contributor.authorVink, Jorick S.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.contributor.otherCentros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548-
dc.date.accessioned2021-04-13T13:22:40Z-
dc.date.available2021-04-13T13:22:40Z-
dc.date.issued2020-09-14-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 499(2): 1918–1936(2020)es
dc.identifier.issn0035-8711-
dc.identifier.otherhttps://academic.oup.com/mnras/article/499/2/1918/5905414-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/302-
dc.description.abstractWe present an optical analysis of 55 members of R136, the central cluster in the Tarantula Nebula of the Large Magellanic Cloud. Our sample was observed with STIS aboard the Hubble Space Telescope, is complete down to about 40M(circle dot), and includes seven very massive stars with masses over 100M(circle dot). We performed a spectroscopic analysis to derive their physical properties. Using evolutionary models, we find that the initial mass function of massive stars in R136 is suggestive of being top-heavy with a power-law exponent gamma approximate to 2 +/- 0.3, but steeper exponents cannot be excluded. The age of R136 lies between 1 and 2Myr with a median age of around 1.6Myr. Stars more luminous than log L/L-circle dot = 6.3 are helium enriched and their evolution is dominated by mass-loss, but rotational mixing or some other form of mixing could be still required to explain the helium composition at the surface. Stars more massive than 40 M-circle dot have larger spectroscopic than evolutionary masses. The slope of the wind-luminosity relation assuming unclumped stellar winds is 2.41 +/- 0.13 which is steeper than usually obtained (similar to 1.8). The ionizing (log Q(0) [ph/s] = 51.4) and mechanical (logL(SW) [erg/s] = 39.1) output of R136 is dominated by the most massive stars (> 100M(circle dot)). R136 contributes around a quarter of the ionizing flux and around a fifth of the mechanical feedback to the overall budget of the Tarantula Nebula. For a census of massive stars of the Tarantula Nebula region, we combined our results with the VLT-FLAMES Tarantula Survey plus other spectroscopic studies. We observe a lack of evolved Wolf-Rayet stars and luminous blue and red supergiants.es
dc.description.sponsorshipWe thank the referee, Tomer Shenar, for providing helpful comments and suggestions which improved the clarity and content of the manuscript. We thank Chris Evans and Hugues Sana for comments to this manuscript. We would like to thank Nolan Walborn for the spectral classification, which will be published in Paper III. Financial support to Azalee Bostroem from Nolan Walborn's HST grant NAS 5-26555 and thanks to Azalee Bostroem for the work on the data reduction. JMB acknowledges financial support from the University of Sheffield. JMA acknowledges support from the Spanish Government Ministerio de Ciencia e Innovacion through grant PGC-2018-095 049-B-C22. SS-D and AHD acknowledge funding from the Spanish Government Ministerio de Ciencia e Innovacion through grants PGC-2018-091 3741-B-C22, SEV 2015-0548, and CEX2019-000920-S, and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2017010115; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.language.isoenges
dc.publisherOxford Academics: Oxford University Presses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-095049-B-C22-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-0913741-B-C22-
dc.subjectStars: early typees
dc.subjectStars: evolutiones
dc.subjectStars: fundamental parameterses
dc.subjectStars: massivees
dc.subjectGalaxies: clsuters: individual: R136es
dc.subjectMagellanic cloudses
dc.titleThe R136 star cluster dissected with Hubble Space Telescope/STIS – II. Physical properties of the most massive stars in R136es
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidSchneider, F. [0000-0002-5965-1022]-
dc.contributor.orcidBestenlehner, J. [0000-0002-0859-5139]-
dc.contributor.orcidCaballero Nieves, S. [0000-0002-8348-5191]-
dc.contributor.orcidMaíz Apellániz, J. [0000-0003-0825-3443]-
dc.identifier.doi10.1093/mnras/staa2801-
dc.identifier.e-issn1365-2966-
dc.contributor.funderAgencia Canaria de Investigación, Innovación y Sociedad de la Información (ACIISI)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.description.peerreviewedPeer reviewes
dc.identifier.funderhttps://doi.org/10.13039/501100007757-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100011033-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/restrictedAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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