. . . . . . "\u8239\u5E06\u5EA7KQ\uFF0C\u53C8\u540DCD-41 6220\uFF0CHD 94660\u3001SAO 222422\u3001HR 4263\uFF0C\u662F\u8239\u5E06\u5EA7\u7684\u4E00\u9897\u6052\u661F\uFF0C\u89C6\u661F\u7B49\u4E3A6.11\uFF0C\u4F4D\u4E8E\u9280\u7D93280.98\uFF0C\u9280\u7DEF15.6\uFF0C\u5176B1900.0\u5750\u6807\u4E3A\u8D64\u7D9310h 50m 28.8s\uFF0C\u8D64\u7DEF-41\u00B0 15.6\u2032 5\u2033\u3002"@zh . . "6.112"^^ . . . "KQ Velorum"@en . "HD 94660"@it . "KQ Vel A"@en . . . . . . "1124351715"^^ . . . "HD 94660 \u00E8 una stella ipergigante bianca di magnitudine 6,08 situata nella costellazione delle Vele. Dista 492 anni luce dal sistema solare."@it . . . . . . . "\u221236.021"@en . . . . . . . . . . . "HD94660 \u2014 \u0445\u0456\u043C\u0456\u0447\u043D\u043E \u043F\u0435\u043A\u0443\u043B\u044F\u0440\u043D\u0430 \u0437\u043E\u0440\u044F \u0441\u043F\u0435\u043A\u0442\u0440\u0430\u043B\u044C\u043D\u043E\u0433\u043E \u043A\u043B\u0430\u0441\u0443 A0, \u0449\u043E \u043C\u0430\u0454 \u0432\u0438\u0434\u0438\u043C\u0443 \u0437\u043E\u0440\u044F\u043D\u0443 \u0432\u0435\u043B\u0438\u0447\u0438\u043D\u0443 \u0432 \u0441\u043C\u0443\u0437\u0456 V \u043F\u0440\u0438\u0431\u043B\u0438\u0437\u043D\u043E 6,1.\u0412\u043E\u043D\u0430 \u0440\u043E\u0437\u0442\u0430\u0448\u043E\u0432\u0430\u043D\u0430 \u043D\u0430 \u0432\u0456\u0434\u0441\u0442\u0430\u043D\u0456 \u0431\u043B\u0438\u0437\u044C\u043A\u043E 495,7 \u0441\u0432\u0456\u0442\u043B\u043E\u0432\u0438\u0445 \u0440\u043E\u043A\u0456\u0432 \u0432\u0456\u0434 \u0421\u043E\u043D\u0446\u044F."@uk . "HD94660"@uk . . . . . . . . . . . . . "HD 94660 \u00E8 una stella ipergigante bianca di magnitudine 6,08 situata nella costellazione delle Vele. Dista 492 anni luce dal sistema solare."@it . . . . "Ap"@en . "KQ Velorum"@es . "105"^^ . . . . . . . . . "8.7507"^^ . "A0p EuCrSi"@en . . "KQ Velorum (KQ Vel / HD 94660 / HR 4263)\u200B es una estrella variable en la constelaci\u00F3n de Vela.Tiene magnitud aparente media +6,09 y se encuentra a 496 a\u00F1os luz de distancia del Sistema Solar. De tipo espectral A0p, KQ Velorum es una estrella peculiar con sobreabundancia de ciertos elementos qu\u00EDmicos y con un campo magn\u00E9tico intenso y variable.Su campo magn\u00E9tico efectivo alcanza el valor de 2089 G.\u200BEs tambi\u00E9n una variable Alfa2 Canum Venaticorum \u2014como Alioth (\u03B5 Ursae Majoris) o IM Velorum\u2014, cuya fluctuaci\u00F3n de brillo, de 0,02 magnitudes,\u200B es casi imperceptible."@es . . . . . . . . . . . . "5.157"^^ . "0.24"^^ . . "KQ de la Vela"@ca . . "\u8239\u5E06\u5EA7KQ"@zh . . . . . . "KQ Velorum is a variable star system in the southern constellation of Vela. It has the identifier HD 94660 in the Henry Draper Catalogue; KQ Vel is the variable star designation. This appears as a sixth magnitude star with an apparent visual magnitude of 6.112, and thus is dimly visible to the naked eye under suitable viewing conditions. The system is located at a distance of approximately 373 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of around 23 km/s."@en . "0.1578"^^ . . . . . . . . . "KQ Velorum (KQ Vel / HD 94660 / HR 4263)\u200B es una estrella variable en la constelaci\u00F3n de Vela.Tiene magnitud aparente media +6,09 y se encuentra a 496 a\u00F1os luz de distancia del Sistema Solar. De tipo espectral A0p, KQ Velorum es una estrella peculiar con sobreabundancia de ciertos elementos qu\u00EDmicos y con un campo magn\u00E9tico intenso y variable.Su campo magn\u00E9tico efectivo alcanza el valor de 2089 G.\u200BEs tambi\u00E9n una variable Alfa2 Canum Venaticorum \u2014como Alioth (\u03B5 Ursae Majoris) o IM Velorum\u2014, cuya fluctuaci\u00F3n de brillo, de 0,02 magnitudes,\u200B es casi imperceptible. KQ Velorum tiene una temperatura efectiva de 10.700 K\u200B \u201411.600 K seg\u00FAn otra fuente\u2014\u200B y brilla con una luminosidad 109 veces mayor que la del Sol.Sin embargo, es en longitudes de onda de rayos X donde KQ Velorum exhibe una notable luminosidad, alcanzando 3577 \u00D7 1020 W; en esta parte del espectro es 184 veces m\u00E1s luminosa que Vega (\u03B1 Lyrae) y 127 veces m\u00E1s luminosa que Phecda (\u03B3 Ursae Majoris), tambi\u00E9n estrellas A0V.\u200B Con un radio 3 veces m\u00E1s grande que el radio solar,\u200B la masa de KQ Velorum es de 2,85 masas solares y tiene una edad estimada de 263 millones de a\u00F1os, habiendo transcurrido casi 2/3 de su vida como estrella de la secuencia principal.\u200B"@es . "KQ Velorum is a variable star system in the southern constellation of Vela. It has the identifier HD 94660 in the Henry Draper Catalogue; KQ Vel is the variable star designation. This appears as a sixth magnitude star with an apparent visual magnitude of 6.112, and thus is dimly visible to the naked eye under suitable viewing conditions. The system is located at a distance of approximately 373 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of around 23 km/s. This was first identified as a chemically peculiar star by Carlos and Mercedes Jaschek in 1959, who found spectral peculiarities in the silicon absorption bands. The long-term photometric variability of this star was reported by in 1993, who noted a possibly complicated light curve with an estimated period on the order of 2,700 days. In 1975, and detected a strong magnetic field in excess of 1 kG on the star. Radial velocity measurements by and associates (1997) demonstrated this is a spectroscopic binary system. This single-lined spectroscopic binary has a physical separation of at least 1.25 \u00B1 0.01 AU, an orbital period of 2.32 years, and a high eccentricity (ovalness) of 0.45. The visible component is an Ap star with a stellar classification of Ap(SiCr), although the effective temperature of 11,300 K is a closer match to a spectral type of B8.5p. and associates (1991) gave a spectral type of A0p EuCrSi, indicating the spectrum shows peculiarities in the europium, chromium, and silicon bands. It is classified as an Alpha2 Canum Venaticorum variable with a brightness that varies from 6.10 down to 6.12 in magnitude. KQ Vel is a frequently-studied object that is often used as a magnetic standard star. The magnetic field of this star has a dipole strength of 7.5 kG, while displaying additional quadropole and octopole moments. It is inclined to the rotation axis by 16\u00B0. The mean longitudal field is almost constant, showing a strength of \u22122 kG. The star is less than halfway through its main sequence lifespan, but is rotating very slowly with a period of around 2,800 days. It has three times the mass and 2.5 times the radius of the Sun, while radiating 105 times the Sun's luminosity. The mass function of the system indicates that the secondary must have more than two times the mass of the Sun, yet there is no sign of it in otherwise high-quality spectra. A main sequence stellar companion of this mass would have a spectral type earlier than A5V. This led to the suggestion that this companion must be a compact object, either a black hole, a neutron star, or a pair of white dwarfs. In 2018 the companion was detected in the near infrared using the Pioneer instrument at the VLIT observatory, showing an H-band magnitude difference of 1.8\u00B10.03 at an angular separation of 18.72\u00B10.02 mas. This corresponds to a projected linear separation of a little over 2 AU. X-ray observations with the Chandra X-ray Observatory in 2016 confirmed that the companion is a neutron star; the first known pair of strongly magnetic Ap star and neutron star that have been discovered. The neutron star in this system is the product of a supernova explosion, possibly of the electron capture type that would not significantly disrupt the orbit. The strongly magnetic Ap star is likely the result of a merger, perhaps from an W UMa close binary. The current neutron star may have been the tertiary member of the system, and it gained mass during a Roche lobe overflow of the binary components."@en . "69050204"^^ . . "HD94660 \u2014 \u0445\u0456\u043C\u0456\u0447\u043D\u043E \u043F\u0435\u043A\u0443\u043B\u044F\u0440\u043D\u0430 \u0437\u043E\u0440\u044F \u0441\u043F\u0435\u043A\u0442\u0440\u0430\u043B\u044C\u043D\u043E\u0433\u043E \u043A\u043B\u0430\u0441\u0443 A0, \u0449\u043E \u043C\u0430\u0454 \u0432\u0438\u0434\u0438\u043C\u0443 \u0437\u043E\u0440\u044F\u043D\u0443 \u0432\u0435\u043B\u0438\u0447\u0438\u043D\u0443 \u0432 \u0441\u043C\u0443\u0437\u0456 V \u043F\u0440\u0438\u0431\u043B\u0438\u0437\u043D\u043E 6,1.\u0412\u043E\u043D\u0430 \u0440\u043E\u0437\u0442\u0430\u0448\u043E\u0432\u0430\u043D\u0430 \u043D\u0430 \u0432\u0456\u0434\u0441\u0442\u0430\u043D\u0456 \u0431\u043B\u0438\u0437\u044C\u043A\u043E 495,7 \u0441\u0432\u0456\u0442\u043B\u043E\u0432\u0438\u0445 \u0440\u043E\u043A\u0456\u0432 \u0432\u0456\u0434 \u0421\u043E\u043D\u0446\u044F."@uk . "KQ de la Vela (KQ Velorum) \u00E9s un estel variable en la constel\u00B7laci\u00F3 de Vela.T\u00E9 magnitud aparent mitjana +6,09 i es troba a 496 anys llum de dist\u00E0ncia del Sistema Solar. De tipus espectral A0p, KQ de la Vela \u00E9s un estel peculiar amb sobreabund\u00E0ncia de certs elements qu\u00EDmics i amb un camp magn\u00E8tic intens i variable. El seu camp magn\u00E8tic efectiu, Be aconsegueix el valor de 2089 G. \u00C9s tamb\u00E9 una variable Alfa\u00B2 Canum Venaticorum \u2014com Alioth (\u03B5 Ursae Majoris) o IM Velorum\u2014, de qui la lluentor fluctua 0,02 magnituds, i \u00E9s gaireb\u00E9 imperceptible. KQ de la Vela t\u00E9 una temperatura efectiva de 10.700 K \u201411.600 K segons una altra font\u2014 i brilla amb una lluminositat 109 vegades major que la del Sol. No obstant aix\u00F2, \u00E9s en longituds d'ona de raigs X on KQ Velorum exhibeix una notable lluminositat, aconseguint 3577\u00D71020 W; en aquesta part de l'espectre \u00E9s 184 vegades m\u00E9s lluminosa que Vega (\u03B1 Lyrae) i 127 vegades m\u00E9s lluminosa que Phecda (\u03B3 Ursae Majoris), tamb\u00E9 estels A0V. Amb un radi 3 vegades m\u00E9s gran que el radi solar, la massa de KQ de la Vela \u00E9s de 2,85 masses solars i t\u00E9 una edat estimada de 263 milions d'anys, havent transcorregut gaireb\u00E9 2/3 de la seva vida com a estel de la seq\u00FC\u00E8ncia principal."@ca . . . . . . "J2000.0"@en . . . . . . . . . . . . "\u8239\u5E06\u5EA7KQ\uFF0C\u53C8\u540DCD-41 6220\uFF0CHD 94660\u3001SAO 222422\u3001HR 4263\uFF0C\u662F\u8239\u5E06\u5EA7\u7684\u4E00\u9897\u6052\u661F\uFF0C\u89C6\u661F\u7B49\u4E3A6.11\uFF0C\u4F4D\u4E8E\u9280\u7D93280.98\uFF0C\u9280\u7DEF15.6\uFF0C\u5176B1900.0\u5750\u6807\u4E3A\u8D64\u7D9310h 50m 28.8s\uFF0C\u8D64\u7DEF-41\u00B0 15.6\u2032 5\u2033\u3002"@zh . . . . "13515"^^ . . . . . . . . "KQ de la Vela (KQ Velorum) \u00E9s un estel variable en la constel\u00B7laci\u00F3 de Vela.T\u00E9 magnitud aparent mitjana +6,09 i es troba a 496 anys llum de dist\u00E0ncia del Sistema Solar. De tipus espectral A0p, KQ de la Vela \u00E9s un estel peculiar amb sobreabund\u00E0ncia de certs elements qu\u00EDmics i amb un camp magn\u00E8tic intens i variable. El seu camp magn\u00E8tic efectiu, Be aconsegueix el valor de 2089 G. \u00C9s tamb\u00E9 una variable Alfa\u00B2 Canum Venaticorum \u2014com Alioth (\u03B5 Ursae Majoris) o IM Velorum\u2014, de qui la lluentor fluctua 0,02 magnituds, i \u00E9s gaireb\u00E9 imperceptible."@ca . . . . . .