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dc.contributor.authorBarstow, Martin A.pt_BR
dc.contributor.authorWesemael, F.pt_BR
dc.contributor.authorHolberg, J.B.pt_BR
dc.contributor.authorBuckley, David A.H.pt_BR
dc.contributor.authorStobie, Robert S.pt_BR
dc.contributor.authorMittaz, J.P.D.pt_BR
dc.contributor.authorFontaine, Gillespt_BR
dc.contributor.authorRosen, Simon R.pt_BR
dc.contributor.authorDemers, Sergept_BR
dc.contributor.authorLamontagne, R.pt_BR
dc.contributor.authorIrwin, Michael Johnpt_BR
dc.contributor.authorBergeron, Pierrept_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.contributor.authorVennes, S.pt_BR
dc.date.accessioned2014-03-21T01:48:49Zpt_BR
dc.date.issued1994pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/88728pt_BR
dc.description.abstractWe report the discovery of the hot DA white dwarf RE 0457- 281 which has the lowest line-of-sight neutral hydrogen column density yet measured. The star was found independently by the ROSAT EUV, Montreal-Cambridge-Tololo and Edinburgh-Cape surveys. With an effective temperature of 60 700 K and very soft EUV spectrum, this white dwarf resembles the well-studied hot DA white dwarf G 191- B2B. A follow-up observation made using the Voyager 2 UV spectrometer reveals a strong continuum shortward of the 912-Å Lyman limit from which we deduce that the neutral hydrogen column density is 1.3 x 1O 17 atom cm-².en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society. London. Vol. 267, no. 3 (Apr. 1994), p. 647-652pt_BR
dc.rightsOpen Accessen
dc.subjectAstrofisica estelarpt_BR
dc.subjectStars: atmospheresen
dc.subjectStars: individual: RE 0457- 281en
dc.subjectAstrofísicapt_BR
dc.subjectAbundanciapt_BR
dc.subjectWhite dwarfsen
dc.subjectAnãs brancaspt_BR
dc.subjectISM: abundancesen
dc.subjectUltraviolet: starsen
dc.titleA new hot DA white dwarf in a region of exceptionally low HI densitypt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000220166pt_BR
dc.type.originEstrangeiropt_BR


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