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- Q603657 subject Q7009295.
- Q603657 subject Q8284795.
- Q603657 subject Q8398144.
- Q603657 subject Q8589650.
- Q603657 subject Q8691170.
- Q603657 abstract "VV Cephei, also known as HD 208816, is an eclipsing binary star system located in the constellation Cepheus, approximately 5,000 light years from Earth. A red supergiant fills the system's Roche lobe when closest to its companion blue star, the latter appearing to be on the main sequence. Matter flows from the red supergiant onto the blue companion for at least part of the orbit and the hot star is obscured by a large disk of material. The red supergiant primary, known as VV Cephei A, is currently recognised as one of the largest stars in the galaxy, with an estimated solar radius of 1,050. Although VV Cephei is an extremely large star showing high mass loss and having some emissions lines, the spectral luminosity class and absolute magnitude do not qualify it as a hypergiant.It should be possible to calculate the masses of eclipsing binary stars with some accuracy, but in this case mass loss, changes in the orbital parameters, a disk obscuring the hot secondary, and doubt about the distance of the system have led to wildly varying estimates. Calculations before the most recent primary and secondary eclipses had started to settle on masses of around 20 for both stars, but more recent papers have suggested that even this is too high. Evolutionary models show that the initial mass of a star reaching the red supergiant stage as a star like VV Cephei would be no more than 25 times the Sun, and obviously considerably lower now. Like Betelgeuse, VV Cephei A is plagued by phenomena intrinsic to large diffuse stars that make them difficult to measure with precision. VV Cephei is not entirely spherical, being surrounded by opaque shells of a highly extended atmosphere, which, coupled with limb darkening, unstable luminosity, and other factors, make it difficult to determine its true size. Some researchers still hold that VV Cephei is a normal AGB star about 500 times the radius of the Sun, and not a hypergiant, including results from the most recent eclipse.".
- Q603657 thumbnail VV_Cephei.png?width=300.
- Q603657 wikiPageExternalLink alapre.pl?-c=21+56+39.144+%2B63+37+32.01&button=N%26B.
- Q603657 wikiPageExternalLink vv-cephei.shtml.
- Q603657 wikiPageExternalLink VVCephei.html.
- Q603657 wikiPageExternalLink aas_largest_stars_050110.html.
- Q603657 wikiPageExternalLink three_largest_stars.html.
- Q603657 wikiPageWikiLink Q10468.
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- Q603657 wikiPageWikiLink Q555846.
- Q603657 wikiPageWikiLink Q5898.
- Q603657 wikiPageWikiLink Q7009295.
- Q603657 wikiPageWikiLink Q772102.
- Q603657 wikiPageWikiLink Q8284795.
- Q603657 wikiPageWikiLink Q8398144.
- Q603657 wikiPageWikiLink Q848485.
- Q603657 wikiPageWikiLink Q854050.
- Q603657 wikiPageWikiLink Q8589650.
- Q603657 wikiPageWikiLink Q8691170.
- Q603657 wikiPageWikiLink Q8928.
- Q603657 type Place.
- Q603657 type CelestialBody.
- Q603657 type Location.
- Q603657 type Place.
- Q603657 type Star.
- Q603657 type Thing.
- Q603657 comment "VV Cephei, also known as HD 208816, is an eclipsing binary star system located in the constellation Cepheus, approximately 5,000 light years from Earth. A red supergiant fills the system's Roche lobe when closest to its companion blue star, the latter appearing to be on the main sequence. Matter flows from the red supergiant onto the blue companion for at least part of the orbit and the hot star is obscured by a large disk of material.".
- Q603657 label "VV Cephei".
- Q603657 depiction VV_Cephei.png.
- Q603657 name "VV Cephei".