Beta Capricorni
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| Observation data Epoch J2000.0 |
|
|---|---|
| Constellation | Capricornus |
| Right ascension | 20h21m00.7s |
| Declination | −14°46′53″ |
| Apparent magnitude (V) | +3.05/+6.09 |
| Spectral Characteristics | |
| Spectral type | K0II+B8V/A0III |
| U-B color index | 0.28/−0.11 |
| B-V color index | 0.79/−0.02 |
| Variable type | none |
| Astrometry | |
| Radial velocity (Rv) | −19/−18 km/s |
| Proper motion (μ) | RA: 48.42/42.64 mas/yr Dec.: 14.00/0.37 mas/yr |
| Parallax (π) | 9.94 ± 1.00 mas |
| Distance | 328 ly (101 pc) |
| Absolute magnitude (MV) | −1.96/+1.08 |
| Other designations | |
Beta Capricorni (β Cap / β Capricorni) is a star system in the constellation Capricornus. It also has the traditional name Dabih, which comes from the Arabic, meaning "butchers". The β Capricorni system is located 328 light years from Earth. Because it is near the ecliptic, β Capricorni can be occulted by the Moon, and also (rarely) by planets.
Contents |
[edit] Visual double
With binoculars or a small telescope, β Capricorni can be resolved into a double star. The brighter of these two components, β¹ Capricorni or Dabih Major, has an apparent magnitude of +3.05, while the dimmer one, β² Capricorni or Dabih Minor, has an apparent magnitude of +6.09. The two components are separated by 3.5 arcminutes on the sky, putting them at leat 21,000 AU (0.34 light years) apart. They take approximately 700,000 years to complete one orbit. Both of these components are themselves made up of multiple stars.
Due to the complexity of this system, several different schemes have arisen to denote the subcomponents. This article follows the naming used in the Multiple Star Catalogue[1].
[edit] β¹ Capricorni
The brighter component, β¹ Capricorni, is the more complex of the pair. It has at least three components, and it's spectrum is difficult to interpret. It is dominated by a pair of stars, the orange K-type bright giant β Capricorni Aa, with an apparent magnitude of +3.08, and the blue-white B-Type main sequence dwarf, β Capricorni Ab with an apparent magnitude of +7.20. These two components are separated by 0.05 arcseconds (5 AU) and have an orbital period of 3.77 years.
The Aa component has a surface temperature of 4900 kelvins, a diameter of 35 times that of the Sun, and a luminosity 600 times that of the Sun. The Ab component has another, unseen companion, β Capricorni Ac, which orbits Ab with an orbital period of 8.7 days. It is thought that the Aa component is itself multiple.
[edit] β² Capricorni
The dimmer of the visual double star, β¹ Capricorni, is simpler and more studied. It is a binary star, whose brighter component, β Capricorni B, has a magnitude of 6.1. It is a A0-giant with 40 times the luminosity of the Sun. The companion, β Capricorni C, is approximately 3 arcseconds from B. β Capricorni B is unusual for having large amounts of mercury and manganese in its atmosphere.
[edit] Other components
Two other nearby stars were discovered by John Herschel. These lie 112 arcseconds away from β¹ Capricorni, and it is unclear whether they are simply optical doubles or part of the β Capricorni system. They are sometimes referred to as β Capricorni D and E.
[edit] References
- ^ Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". A&AS 124: 75-84.
