"-0.22"^^ . "BV Centauri"@en . . . . . . "40000"^^ . "BV Centauri"@pt . "2.81"^^ . "1.05"^^ . . . "0.77"^^ . "10062"^^ . . . . ""@en . "1.18"^^ . "0.38"^^ . . . "13.05"^^ . . . . . . "-25.8"^^ . . . . . "3.5"^^ . "500"^^ . . . . . . . . . "-1.4"^^ . . . . "+3.0 - +5.8"@en . "Primary"@en . . . "1.41"^^ . . . . . . "55740699"^^ . "BV Centauri"@en . . . . . "1076214332"^^ . "-22.3"^^ . . "BV Centauri \u00E9 uma estrela bin\u00E1ria vari\u00E1vel catacl\u00EDsmica na constela\u00E7\u00E3o de Centaurus. \u00C9 uma , apresentando aumentos r\u00E1pidos de luminosidade que s\u00E3o recorrentes com um per\u00EDodo m\u00E9dio de 150 dias, que parece ter aumentado nas \u00FAltimas d\u00E9cadas. Durante o estado quieto, sua magnitude aparente visual \u00E9 de aproximadamente 13, com varia\u00E7\u00F5es de alguns d\u00E9cimos ao longo de uma \u00F3rbita devido a diferen\u00E7as na \u00E1rea vis\u00EDvel das estrelas, aumentando at\u00E9 um m\u00E1ximo de 10,7 nas erup\u00E7\u00F5es. Medi\u00E7\u00F5es de paralaxe pelo sat\u00E9lite astrom\u00E9trico Gaia determinaram que o sistema est\u00E1 a uma dist\u00E2ncia de aproximadamente 361 parsecs (1 178 anos-luz) da Terra, um valor menor que a estimativa indireta anterior de 500 parsecs, baseada na sua luminosidade."@pt . . . . . . . . . . . . "G5-G8IV-V"@en . . . . "J2000"@en . ","@en . . "5250"^^ . ""@en . . "BV Centauri is a cataclysmic variable binary star in the constellation Centaurus. It is a dwarf nova, and undergoes rapid increases in brightness that are recurrent with a mean period of 150 days. This period seems to have increased in the last few decades. During quiescence, its visual apparent magnitude is about 13, with variations of a few tenths of magnitude over an orbit due to differences in the star's visible surface area (ellipsoidal variability), brightening to a maximum magnitude of 10.7 during outbursts. From its luminosity, it is estimated that the system is about 500 parsecs (1,600 ly) away from Earth. A Gaia parallax of 2.81 mas has been measured, corresponding to about 360 pc."@en . . "8.300000000000001"^^ . . "BV Centauri \u00E9 uma estrela bin\u00E1ria vari\u00E1vel catacl\u00EDsmica na constela\u00E7\u00E3o de Centaurus. \u00C9 uma , apresentando aumentos r\u00E1pidos de luminosidade que s\u00E3o recorrentes com um per\u00EDodo m\u00E9dio de 150 dias, que parece ter aumentado nas \u00FAltimas d\u00E9cadas. Durante o estado quieto, sua magnitude aparente visual \u00E9 de aproximadamente 13, com varia\u00E7\u00F5es de alguns d\u00E9cimos ao longo de uma \u00F3rbita devido a diferen\u00E7as na \u00E1rea vis\u00EDvel das estrelas, aumentando at\u00E9 um m\u00E1ximo de 10,7 nas erup\u00E7\u00F5es. Medi\u00E7\u00F5es de paralaxe pelo sat\u00E9lite astrom\u00E9trico Gaia determinaram que o sistema est\u00E1 a uma dist\u00E2ncia de aproximadamente 361 parsecs (1 178 anos-luz) da Terra, um valor menor que a estimativa indireta anterior de 500 parsecs, baseada na sua luminosidade. Vari\u00E1veis catacl\u00EDsmicas s\u00E3o sistemas bin\u00E1rios de curto per\u00EDodo em que uma estrela secund\u00E1ria transfere mat\u00E9ria para uma an\u00E3 branca prim\u00E1ria. Em BV Centauri, a an\u00E3 branca e sua companheira t\u00EAm massas estimadas em 1,18 e 1,05 vezes a massa solar e cada uma contribui para aproximadamente metade da luz vis\u00EDvel do sistema. A estrela secund\u00E1ria parece ser uma estrela evolu\u00EDda com um tipo espectral de G5-G8IV-V, o que \u00E9 evidenciado por seu raio estendido de 1,4 raios solares. A reconstru\u00E7\u00E3o de sua superf\u00EDcie revelou que esta \u00E9 uma estrela com alta atividade magn\u00E9tica, apresentando cerca de 25% de sua superf\u00EDcie coberta por manchas estelares, que s\u00E3o mais abundantes no hemisf\u00E9rio da estrela virado para a an\u00E3 branca. Al\u00E9m disso, uma proemin\u00EAncia foi detectada acima da superf\u00EDcie da estrela secund\u00E1ria, tamb\u00E9m no lado virado para a an\u00E3 branca. A \u00F3rbita do sistema tem um per\u00EDodo de 0,611179 dias (16,7 horas), um dos maiores per\u00EDodos conhecidos para uma nova an\u00E3, e est\u00E1 inclinada em 53 \u00B1 4\u00B0 em rela\u00E7\u00E3o ao plano do c\u00E9u. A curva de luz de BV Centauri durante as erup\u00E7\u00F5es apresenta comportamento anormal para uma nova an\u00E3, com um longo intervalo de cerca de 15 dias antes de atingir luminosidade m\u00E1xima, tendo sido comparada \u00E0 nova cl\u00E1ssica . Com base nisso, j\u00E1 foi proposto que BV Centauri pode ter gerado uma nova no s\u00E9culo XIX, n\u00E3o registrada pelos observadores da \u00E9poca."@pt . . . . . . . . . "Secondary"@en . . "days"@en . . . . . "BV Centauri is a cataclysmic variable binary star in the constellation Centaurus. It is a dwarf nova, and undergoes rapid increases in brightness that are recurrent with a mean period of 150 days. This period seems to have increased in the last few decades. During quiescence, its visual apparent magnitude is about 13, with variations of a few tenths of magnitude over an orbit due to differences in the star's visible surface area (ellipsoidal variability), brightening to a maximum magnitude of 10.7 during outbursts. From its luminosity, it is estimated that the system is about 500 parsecs (1,600 ly) away from Earth. A Gaia parallax of 2.81 mas has been measured, corresponding to about 360 pc. Cataclysmic variables are short-period binary systems in which a white dwarf primary accretes matter from a secondary star. For BV Centauri, the white dwarf and its companion have estimated masses of 1.18 and 1.05 times the mass of the Sun respectively, although alternate, conflicting mass measurements were reported too. The secondary is a conventional star with a spectral type of G5-G8IV-V and it is assumed to contribute to half of the visual luminosity of the system. It is thought to have a radius of 1.4 R\u2609 and so to be significantly evolved away from the zero age main sequence. The reconstruction of its surface by Doppler imaging revealed it to be a highly magnetically active star, with about 25% of its surface covered in starspots which are much more abundant on the hemisphere facing the white dwarf. Furthermore, a prominence was detected above the secondary star's surface, also in the side facing the white dwarf. The white dwarf primary can be observed clearly at ultraviolet wavelengths where it is the strongest source. Any accretion disk in the system appears relatively faint. The system has a period of 0.611179 days (16.7 hours), one of the longest periods for a dwarf nova, and is inclined by 53 \u00B1 4\u00B0 in relation to the plane of the sky. It has been noted that BV Centauri's light curve during outbursts has anomalous behavior for a dwarf nova, with a long interval of up to 15 days before reaching peak brightness and no plateau at maximum brightness, and it has been compared to the classic nova GK Persei. Based on this, it has been proposed that BV Centauri could have generated an unobserved nova outburst in the 19th century, which was missed by the observers at the time."@en .