The crossbar is a bright near-equatorial star, β Orion . White and blue supergiant . The name in Arabic means “foot” (meaning the foot of Orion). Has a visual magnitude of 0.12 m . The crossbar is located at a distance of about 860 [2] light years from the Sun. The temperature of its surface is 12 130 K ( spectral class B8I-a) [6] , the diameter is about 103 million km (that is, 74 times the size of the Sun) and the absolute magnitude is −7.84 m ; its luminosity is approximately 130,000 times [5] [9] higher than the sun, which means that it is one of the most powerful stars in the Galaxy (in any case, along with Deneb , one of the two most powerful brightest stars in the sky, since Rigel is the nearest of the stars with such great luminosity).
| Crossbar | |||
|---|---|---|---|
| Star | |||
 The crossbar, as it would be observed from a distance of 1 a. e. | |||
| Observational data ( Age J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 860 ± 80 St. years (260 ± 20 pc ) | ||
| Visible magnitude ( V ) | 0.12 / 8.44 | ||
| Constellation | Orion | ||
| Astrometry | |||
| Radial velocity ( R v ) | 20.7 km / s | ||
| Own movement (μ) | RA: 1.31 mas per year Dec: 0.50 mas per year | ||
| Parallax (π) | 3.78 ± 0.34 [2] mas | ||
| Absolute magnitude (V) | −7.84 ± 0.2 [1] | ||
| Specifications | |||
| Spectral class | B8Iab | ||
| Color Index ( B - V ) | −0.03 | ||
| Color Index ( U - B ) | −0.66 | ||
| Variability | Type α Swan [3] | ||
| physical characteristics | |||
| Weight | 18 [4] M ☉ | ||
| Radius | 74 [5] R ☉ | ||
| Age | 8 ± 1⋅10 6 [1] years | ||
| Temperature | 12 130 [6] K | ||
| Luminosity | 1.26 +0.37 −0.29 × 10 5 [5] L ☉ | ||
| Metallicity | -0.06 ± 0.10 [1] | ||
| Rotation | 40 [7] km / s | ||
| |||
| Database Information | |||
| SIMBAD | data | ||
| Sources: [8] [2] | |||
The ancient Egyptians associated Rigel with Sah , the king of stars and the patron saint of the dead, and later with Osiris .
Content
Physical Parameters
According to spectroscopic measurements, the distance to Rigel is estimated at 700-900 light years ( 210-280 pc ). The Hipparcos catalog data based on the Rigel parallax give a distance of 773 st. years ( 237 pc ), with an error of about 19%. The Rigel star is a blue supergiant , 17 times more massive than the Sun, has a brightness of about 130 thousand solar [5] . Most of these stars concentrate on the line of the Milky Way in the sky. From a distance of 1 a. e. The crossbar has a magnitude of −38 m and is a huge circle with an angular diameter of 35 °. The radiation flux of a star per 1 m² is more than 150 MW (about 15 kW / cm² ), while the solar flux is only 1.4 kW / m² . Any object located at a distance of 1 a. e. from Rigel, evaporates and dissipates by a strong stellar wind.
Being a very bright star, Rigel illuminates the dust clouds in the immediate vicinity. The most visible of these clouds is IC 2118 (Witch Head Nebula) [10] . Also associated with Rigel is the Orion Nebula , which, however, is located almost twice as far from the Earth. The crossbar is sometimes classified as a distant member of the Orion OB1 association , and along with other bright stars in that region of the sky, it is probably a member of the Taurus – Orion OB1 association , which is still being formed [10] .
The crossbar is a variable star with an irregular cycle characteristic of supergiants, and has a magnitude range from 0.03 to 0.3 and a period of about 22-25 days. The Rigel system consists of three stars. The presence of a fourth star in the system is sometimes assumed, but this is usually considered an incorrect interpretation of the variability of the main star, which can be caused by physical surface pulsations [11] .
Space Photometry
Rigel was observed by the Canadian MOST satellite for almost 28 days in 2009. The brightness of this supergiant periodically varied within small limits. Gradual changes in the radiation flux indicate the presence of long-period pulsations of the star [12] .
Spectroscopic observations
The crossbar has a halo of gas around it. Its origin is associated with the formation of a star [10] .
System
The Rigel star has been known as a visual double since 1831, when it was first studied by V. Ya. Struve . Crossbar B is a faint star with an apparent magnitude of + 6.7 m , whose brightness is 500 times lower than that of Crossbar. Due to its proximity to the main star, component B can be confidently observed only with a 7-cm telescope [11] . It is estimated that the distance from component B to the main star is more than 2200 a. e. that excludes the observation of signs of orbital motion [10] [11] .
Crossbar B is a spectrally binary star consisting of two main sequence stars orbiting a common center of mass in 9.8 days. Both stars belong to the spectral class B9V. Crossbar B is a more massive star in this pair - its mass is 2.5 solar masses versus 1.9 for Rigel C [10] [11] .
At the end of the 19th and beginning of the 20th centuries, there were disputes regarding the apparent binary nature of Rigel B. Some observers claimed to have seen it as a binary system, while others disproved it. Many proponents of the Rigel B binary were often unable to repeat their observations. Observations excluded the probability of the presence of a visible satellite for Rigel B [10] [11] .
Cultural Significance
The Maori celebrated Matariki (New Year) on the first sunrise of the Pleiades and Rigel.
Surroundings
The following stars are located within a radius of 20 light years from the star Rigel A [13] .
| Star | Spectral class | Distance, st. years old | Abs. star value | Visible value (from Rigel A) |
| Crossbar B | B9v | 0,03223 | -0.52 | -15.55 |
| Crossbar C | B9v | 0,03223 | -0.52 | -15.55 |
| TYC 4763-516-1 | G0v | 12.65 | 3.99 | 1.93 |
| TYC 5331-1211-1 | F6v | 16.81 | 3.23 | 1.79 |
| TYC 5331-1024-1 | F4v | 17.5 | 2.98 | 1,63 |
| TYC 5330-1720-1 | B4v | 18.28 | -0.45 | -1.71 |
| TYC 5330-1702-1 | G3v | 19.01 | 4.41 | 3.23 |
Notes
- ↑ 1 2 3 Przybilla, N. et al. (January 2006). "Quantitative spectroscopy of BA-type supergiants." Astronomy and Astrophysics 445 (3): 1099–1126. arXiv: astro-ph / 0509669 . Bibcode 2006A & A ... 445.1099P . doi: 10.1051 / 0004-6361: 20053832 .
- ↑ 1 2 3 Accurate distances to nearby massive stars with the new reduction of the Hipparcos raw data. arXiv : 0804.2553 (The page contains only a brief summary (abstract), the article itself is downloaded at the top right in the Download section, for example, in pdf format: http://arxiv.org/pdf/0804.2553v1 )
- ↑ VizieR Detailed Page . - β Orion in the OKPZ catalog. Date of treatment September 21, 2009. Archived August 24, 2011.
- ↑ Moravveji, Ehsan; Moya, Andres; Guinan, Edward F. (April 2012), "Asteroseismology of the nearby SN-II Progenitor: Rigel. Part II. Ε-mechanism Triggering Gravity-mode Pulsations?", The Astrophysical Journal 749 (1): 74–84, Bibcode 2012ApJ ... 749..74M , doi: 10.1088 / 0004-637X / 749/1/74
- ↑ 1 2 3 4 Moravveji, Ehsan; Guinan, Edward F .; Shultz, Matt; Williamson, Michael H .; Moya, Andres (March 2012), "Asteroseismology of the nearby SN-II Progenitor: Rigel. Part I. The MOST High-precision Photometry and Radial Velocity Monitoring", The Astrophysical Journal 747 (1): 108–115, arXiv: 1201.0843 , Bibcode 2012ApJ ... 747..108M , doi: 10.1088 / 0004-637X / 747/2/108
- ↑ 1 2 Zorec, J. et al. (July 2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff", Astronomy and Astrophysics 501 (1): 297–320, Bibcode 2009A & A ... 501. .297Z , doi: 10.1051 / 0004-6361 / 200811147
- ↑ Abt, Helmut A .; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, Bibcode 2002ApJ ... 573..359A , doi: 10.1086 / 340590
- ↑ SIMBAD . - Crossbar in the SIMBAD database . Date of appeal September 15, 2009.
- ↑ Rigel's bolometric magnitude is −7.92 m ± 0.28 m . Knowing the absolute magnitude of the Sun (4.83 m ), it is easy to determine the luminosity of the Rigel: 1.26 +0.37
−0.29 × 10 5 L ☉ - ↑ 1 2 3 4 5 6 Jedicke, Peter; Levy, David H. (1992). "Regal Rigel." The New Cosmos. Waukesha: Kalmbach Books. pp. 48-53
- ↑ 1 2 3 4 5 Burnham, Robert, Jr. (1978). Burnham's Celestial Handbook. New York: Dover Publications. pp. 1300
- ↑ Moravveji, Ehsan; Guinan, Edward F .; Shultz, Matt; Williamson, Michael H .; Moya, Andres. Asteroseismology of the Nearby SN-II Progenitor: Rigel Part I. The MOST High Precision Photometry and Radial Velocity Monitoring (Eng.) // The Astrophysical Journal. - 2012 .-- 4 January ( no. 747 (1) ). - P. 108–115 .
- ↑ Information may be incomplete, since not all stars can be detected from a distance of more than 700 sv. years separating the Rigel system from us