V382 Carinae
|
Star V382 Carinae / x Carinae |
|||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
|
|||||||||||||||||
| Image by V382 Carinae | |||||||||||||||||
|
|||||||||||||||||
| AladinLite | |||||||||||||||||
|
Observation dates equinox : J2000.0 , epoch : J2000.0 |
|||||||||||||||||
| Constellation | Keel of the ship | ||||||||||||||||
| Right ascension | 11 h 08 m 35.39 s | ||||||||||||||||
| declination | -58 ° 58 ′ 30.1 ″ | ||||||||||||||||
| Apparent brightness | 3.93 mag | ||||||||||||||||
| Typing | |||||||||||||||||
| B − V color index | +1.23 | ||||||||||||||||
| U − B color index | +0.94 | ||||||||||||||||
| R − I index | +0.58 | ||||||||||||||||
| Spectral class | G0 Ia-0 to G4 Ia-0 | ||||||||||||||||
| Variable star type | classic Cepheid | ||||||||||||||||
| Astrometry | |||||||||||||||||
| Radial velocity | (+6.0 ± 0.5) km / s | ||||||||||||||||
| parallax | (0.5 ± 0.2) mas | ||||||||||||||||
| distance | (6300 ± 2000) ly (1900 ± 600) pc |
||||||||||||||||
| Visual absolute brightness M vis | −7.5 mag | ||||||||||||||||
| Proper movement | |||||||||||||||||
| Rec. Share: | (−4.97 ± 0.17) mas / a | ||||||||||||||||
| Dec. portion: | (+1.67 ± 0.16) mas / a | ||||||||||||||||
| Physical Properties | |||||||||||||||||
| Dimensions | ~ 50 M ☉ | ||||||||||||||||
| radius | ~ 750 R ☉ | ||||||||||||||||
| Luminosity |
approx. 150,000 L ☉ |
||||||||||||||||
| Effective temperature | (5200 ± 200) K. | ||||||||||||||||
|
Other names and catalog entries |
|||||||||||||||||
|
|||||||||||||||||
| annotation | |||||||||||||||||
|
|||||||||||||||||
V382 Carinae , also known as x Carinae , is a supergiant of spectral class G in the constellation Kiel des Schiff . He is one of the greatest known stars .
Surname
The first part of the name "V382" follows the rules for naming variable stars and says that V382 Carinae is the 382nd star in the constellation Kiel of the ship where variability could be determined. The second part of the name "Carinae" corresponds to the genitive of the Latin name of the constellation Schiffskiel (Latin 'Carina').
position
V382 Carinae is part of the ship's keel (lat. Carina), a constellation located in the plane of the Milky Way , which can be observed almost all year round from the southern hemisphere. From Europe , the star never appears in the night sky.
The distance from V382 Carinae is about 6000 light years, so it is very obvious that a large part of its light is attenuated by clouds of dust surrounding it or between it and the sun and that the star therefore appears much darker in the sky than it actually is would have to. So far it has not been possible to clearly determine whether V382 Carinae is part of a star cluster . The center of the Carina Nebula (NGC 3372), the region around the luminous binary systems Eta Carinae and HD 93129 is removed from V382 Carinae from about 2,000 light years. Only one pulsar rotating every 0.253 seconds at a distance of about 20 light years has so far been detected. This could also indicate that V382 Carinae is one of the last remaining active stars in an earlier star cluster.
Physical Properties
The physical values of V382 Carinae are, as is often the case with heavy stars of this class, very uncertain and therefore cannot be clearly determined.
V382 Carinae is a giant star and is due to its luminosity in the Hertzsprung-Russell Diagram in the luminosity class divided Ia-0, its properties are above the level of a typical supergiant its spectral class, but V382 Carinae is not as highly luminous as Rho Cassiopeiae or V509 Cassiopeiae , Hypergiant of the same surface temperature.
The mass of V382 Carinae is estimated to be 50 times that of the Sun, and its diameter is believed to be around a billion kilometers. If V382 Carinae were in the center of our solar system, it would reach as far as the orbit of Jupiter.
V382 Carinae is one of the classic Cepheids, a subclass of the pulsation-variable , named after the star Delta Cephei , the prototype of this class. The surface temperature of such stars changes strictly periodically, consequently their spectral class also varies, in the case of V382 Carinae, from G0 to G4. It is unusually heavy for this type of variable star . For example, the comparable V509 Cassiopeiae is one of the semi-regularly variable stars . According to this, V382 Carinae is not yet at the end of its life and could expand further over time and increase its luminosity.
Individual evidence
- ↑ a b c Hipparcos catalog (ESA 1997)
- ↑ a b c Bright Star Catalog
- ↑ Pulkovo radial velocities for 35493 HIP stars
- ↑ a b c Hipparcos, the New Reduction (van Leeuwen, 2007)
- ^ Richard Nugent: The Garnet Star. (No longer available online.) Weblore.com, archived from the original on September 30, 2011 ; accessed on November 13, 2008 (English). Info: The archive link was inserted automatically and has not yet been checked. Please check the original and archive link according to the instructions and then remove this notice.
