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dc.creatorWalborn, Nolan R.-
dc.creatorHowarth, Ian D.-
dc.creatorEvans, Christopher J.-
dc.creatorCrowther, Paul A.-
dc.creatorMoffat, Anthony F. J.-
dc.creatorSt Louis, Nicole-
dc.creatorFariña, Cecilia-
dc.creatorBosch, Guillermo Luis-
dc.creatorMorrell, Nidia Irene-
dc.creatorBarba, Rodolfo Hector-
dc.creatorvan Loon, Jacco Th.-
dc.date2016-12-16T14:07:36Z-
dc.date2016-12-16T14:07:36Z-
dc.date2010-03-
dc.date2016-12-14T15:26:14Z-
dc.date.accessioned2019-04-29T15:46:36Z-
dc.date.available2019-04-29T15:46:36Z-
dc.date.issued2010-03-
dc.identifierWalborn, Nolan R.; Howarth, Ian D.; Evans, Christopher J.; Crowther, Paul A.; Moffat, Anthony F. J.; et al.; The Onfp class in the Magellanic Clouds; Iop Publishing; Astronomical Journal; 139; 3-2010; 1283-1294-
dc.identifier0004-6256-
dc.identifierhttp://hdl.handle.net/11336/9568-
dc.identifier.urihttp://rodna.bn.gov.ar:8080/jspui/handle/bnmm/301709-
dc.descriptionThe Onfp class of rotationally broadened, hot spectra was defined some time ago in the Galaxy, where its membership to date numbers only eight. The principal defining characteristic is a broad, centrally reversed He ii λ 4686 emission profile; other emission and absorption lines are also rotationally broadened. Recent surveys in the Magellanic Clouds (MCs) have brought the class membership there, including some related spectra, to 28. We present a survey of the spectral morphology and rotational velocities, as a first step toward elucidating the nature of this class. Evolved, rapidly rotating hot stars are not expected theoretically, because the stellar winds should brake the rotation. Luminosity classification of these spectra is not possible, because the principal criterion (He ii λ4686) is peculiar; however, the MCs provide reliable absolute magnitudes, which show that they span the entire range from dwarfs to supergiants. The Onfp line-broadening distribution is distinct and shifted toward larger values from those of normal O dwarfs and supergiants with >99.99% confidence. All cases with multiple observations show line-profile variations, which even remove some objects from the class temporarily. Some of them are spectroscopic binaries; it is possible that the peculiar profiles may have multiple causes among different objects. The origin and future of these stars are intriguing; for instance, they could be stellar mergers and/or gamma-ray-burst progenitors.-
dc.descriptionFil: Walborn, Nolan R.. Space Telescope Science Institute; Estados Unidos-
dc.descriptionFil: Howarth, Ian D.. University College London; Estados Unidos-
dc.descriptionFil: Evans, Christopher J.. Royal Observatory Edinburgh. Astronomy Technology Centre; Reino Unido-
dc.descriptionFil: Crowther, Paul A.. University of Sheffield. Department of Physics and Astronomy; Reino Unido-
dc.descriptionFil: Moffat, Anthony F. J.. University Of Montreal; Canadá-
dc.descriptionFil: St Louis, Nicole. University Of Montreal; Canadá-
dc.descriptionFil: Fariña, Cecilia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina-
dc.descriptionFil: Bosch, Guillermo Luis. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina-
dc.descriptionFil: Morrell, Nidia Irene. Observatorio Las Campanas; Chile-
dc.descriptionFil: Barba, Rodolfo Hector. Universidad de la Serena. Facultad de Ciencias; Chile. Consejo Nacional de Investigaciones Cienti­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina-
dc.descriptionFil: van Loon, Jacco Th.. Keele University. School of Physical & Geographical Sciences; Reino Unido-
dc.formatapplication/pdf-
dc.formatapplication/pdf-
dc.formatapplication/pdf-
dc.languageeng-
dc.publisherIop Publishing-
dc.relationinfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2010AJ....139.1283W-
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1001.4032-
dc.relationinfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-6256/139/3/1283/meta-
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://www.dx.doi.org/10.1088/0004-6256/139/3/1283-
dc.rightsinfo:eu-repo/semantics/openAccess-
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/-
dc.sourcereponame:CONICET Digital (CONICET)-
dc.sourceinstname:Consejo Nacional de Investigaciones Científicas y Técnicas-
dc.sourceinstacron:CONICET-
dc.subjectMagellanic Clouds, stars: early-type-
dc.subjectStars emission-line-
dc.subjectStars fundamental parameters-
dc.subjectStars rotation-
dc.subjectStars: variables-
dc.subjectBe-
dc.subjectOtras Ciencias Naturales y Exactas-
dc.subjectOtras Ciencias Naturales y Exactas-
dc.subjectCIENCIAS NATURALES Y EXACTAS-
dc.subjectAstronomía-
dc.subjectCiencias Físicas-
dc.subjectCIENCIAS NATURALES Y EXACTAS-
dc.titleThe Onfp class in the Magellanic Clouds-
dc.typeinfo:eu-repo/semantics/article-
dc.typeinfo:eu-repo/semantics/publishedVersion-
dc.typeinfo:ar-repo/semantics/articulo-
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