VV Orionis (original) (raw)
VV Orionis è una stella bianco-azzurra nella sequenza principale di magnitudine 5,38 situata nella costellazione di Orione. Dista 1853 anni luce dal sistema solare, e si tratta di una binaria spettroscopica, formata da 2 stelle di classe B molto vicine tra loro (0.063 UA), e da una terza componente, di classe A, più lontana, a circa 1 UA
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| dbo:abstract | VV Orionis (VV Ori / HD 36695 / HR 1868) es un sistema estelar situado debajo del Cinturón de Orión, en la constelación del mismo nombre. De acuerdo a su paralaje se halla a 1850 años luz del Sistema Solar. La estrella principal del sistema es una binaria espectroscópica con un período orbital de 1,485378 días (1 día, 11 horas y 39 minutos).La solución orbital otorga una separación entre las componentes de sólo 0,063 UA —un 15% de la distancia entre Mercurio y el Sol.La más luminosa del par es una estrella azul de tipo espectral B1V con una incierta temperatura comprendida entre 21.000 y 25.000 K. Es también la componente más masiva con una masa aproximada de 10,8 masas solares y una luminosidad 9400 veces mayor que la luminosidad solar. Su radio es 2,5 veces más grande que el del Sol.La otra componente es una estrella blanco-azulada de tipo B7V y 15.500 K de temperatura. 330 veces más luminosa que el Sol, tiene una masa de 4,5 masas solares. El diámetro de esta última es la mitad que el de su compañera. Estas cifras, sin embargo, no concuerdan con las obtenidas directamente a partir de luminosidad y temperatura; la discrepancia probablemente tenga su origen en que la distancia determinada por la paralaje es excesiva —una distancia de 1200 años luz puede aproximarse más a la realidad. Dado que el plano orbital es casi paralelo a la línea de visión, VV Orionis es una binaria eclipsante que exhibe dos eclipses desiguales.El eclipse principal tiene lugar cuando la estrella B7, menos luminosa, pasa por delante de su compañera, lo que conlleva una caída en el brillo de magnitud +5,3 a +5,7, siendo su duración de 2,5 horas. Cuando la estrella más luminosa pasa por delante de su compañera tiene lugar el eclipse secundario, produciéndose una caída en el brillo de 0,2 magnitudes. Una tercera estrella, con una separación de 1 UA, orbita el par interior cada 119 días. Es una estrella blanca de tipo A. (es) VV Orionis is an eclipsing binary located in the belt region of the constellation Orion. It is a faint naked eye star. The brightness of VV Orionis dips regularly every 18 hours. The peak visual magnitude is 5.3, which varies slowly in between the dips. The minimum brightness of the dips alternates between magnitude 5.55 and 5.66. The deep minima have a somewhat rounded bottom, while the less deep minima have flat bottoms with a constant magnitude for several hours. However, there are also additional cycles in the lightcurve that suggest that at least one of the stars is pulsating. The VV Orionis system contains two stars which are very close but are not touching. Their orbit is aligned almost perpendicularly to us and there are both primary and secondary eclipses. During secondary eclipse, the primary transits against the secondary, which produces the flat bottom to the secondary minimum. The orbital alignment allows very precise calculation of the orbit and the properties of the stars, but results from different studies have been unusually inconsistent. The lack of a single consistent solution to the orbit has led to suggestions that there is a third star in the system, but this is unproven. A circular orbit with the stars only 13.5 R☉ apart can account for the observed brightness and radial velocity changes, while a third body may explain the decreasing orbital inclination. The two stars are both on the main sequence. The primary, a β Cephei pulsator, has a spectral type of B1 and temperature of about 26,000 K, while the secondary (possibly a slowly pulsating B-type star) has a spectral type of B7 and a temperature of about 16,000 K. The secondary has a mass of 3.8 M☉, radius of 2.4 R☉, and bolometric luminosity of 340 L☉. The primary is over twice the mass, twice the radius, and thirty times the luminosity of its companion. (en) VV Orionis è una stella bianco-azzurra nella sequenza principale di magnitudine 5,38 situata nella costellazione di Orione. Dista 1853 anni luce dal sistema solare, e si tratta di una binaria spettroscopica, formata da 2 stelle di classe B molto vicine tra loro (0.063 UA), e da una terza componente, di classe A, più lontana, a circa 1 UA (it) 獵戶座VV，又名BD-01 943，HD 36695、SAO 132255、HR 1868，是獵戶座的一颗恒星，视星等为5.34，位于銀經204.84，銀緯-17.81，其B1900.0坐标为赤經5h 28m 26.8s，赤緯-1° -17.81′ 35″。 (zh) |
| dbo:thumbnail | wiki-commons:Special:FilePath/Orion_Belt_2009-01-29.jpg?width=300 |
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| dbp:absmagBol | −5.36 + −1.65 (en) |
| dbp:appmagV | 5.310000 (xsd:double) |
| dbp:bV | −0.18 (en) |
| dbp:caption | Location of VV Orionis in the Orion's Belt region (en) |
| dbp:component | VV Ori A (en) VV Ori B (en) |
| dbp:constell | dbr:Orion_(constellation) |
| dbp:credit | Martin Mutti (en) |
| dbp:distLy | 1210 (xsd:integer) |
| dbp:distPc | 371 (xsd:integer) |
| dbp:eccentricity | 0 (xsd:integer) |
| dbp:epoch | J2000 (en) |
| dbp:gravity | 4.026000 (xsd:double) 4.272000 (xsd:double) |
| dbp:inclination | 78.280000 (xsd:double) |
| dbp:luminosity | 339 (xsd:integer) 10400 (xsd:integer) |
| dbp:mass | 3.800000 (xsd:double) 9.520000 (xsd:double) |
| dbp:pError | 0.113800 (xsd:double) |
| dbp:parallax | 2.265400 (xsd:double) |
| dbp:periodUnitless | 128336.69376000001 |
| dbp:propMoDec | −1.183 (en) |
| dbp:propMoRa | −1.088 (en) |
| dbp:radialV | 22.200000 (xsd:double) |
| dbp:radius | 2.360000 (xsd:double) 4.958000 (xsd:double) |
| dbp:temperature | 16100 (xsd:integer) 26200 (xsd:integer) |
| dbp:type | B1V + B7V (en) |
| dbp:uB | −0.09 (en) |
| dbp:variable | dbr:Beta_Cephei_variable dbr:Eclipsing_binary |
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| rdf:type | owl:Thing dbo:Place dbo:Location schema:Place dbo:CelestialBody dbo:Star |
| rdfs:comment | VV Orionis è una stella bianco-azzurra nella sequenza principale di magnitudine 5,38 situata nella costellazione di Orione. Dista 1853 anni luce dal sistema solare, e si tratta di una binaria spettroscopica, formata da 2 stelle di classe B molto vicine tra loro (0.063 UA), e da una terza componente, di classe A, più lontana, a circa 1 UA (it) 獵戶座VV，又名BD-01 943，HD 36695、SAO 132255、HR 1868，是獵戶座的一颗恒星，视星等为5.34，位于銀經204.84，銀緯-17.81，其B1900.0坐标为赤經5h 28m 26.8s，赤緯-1° -17.81′ 35″。 (zh) VV Orionis (VV Ori / HD 36695 / HR 1868) es un sistema estelar situado debajo del Cinturón de Orión, en la constelación del mismo nombre. De acuerdo a su paralaje se halla a 1850 años luz del Sistema Solar. Una tercera estrella, con una separación de 1 UA, orbita el par interior cada 119 días. Es una estrella blanca de tipo A. (es) VV Orionis is an eclipsing binary located in the belt region of the constellation Orion. It is a faint naked eye star. The brightness of VV Orionis dips regularly every 18 hours. The peak visual magnitude is 5.3, which varies slowly in between the dips. The minimum brightness of the dips alternates between magnitude 5.55 and 5.66. The deep minima have a somewhat rounded bottom, while the less deep minima have flat bottoms with a constant magnitude for several hours. However, there are also additional cycles in the lightcurve that suggest that at least one of the stars is pulsating. (en) |
| rdfs:label | VV Orionis (es) VV Orionis (it) VV Orionis (en) 獵戶座VV (zh) |
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| foaf:name | VV Orionis (en) |
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