41 Arae
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Observation data Equinox J2000 |
|
---|---|
Constellation | Ara |
Right ascension | 17h 19m 03.8337s |
Declination | -46° 38′ 10.444″ |
Apparent magnitude (V) | 5.55 |
Characteristics | |
Spectral type | G8 V/K7 Vp |
U-B color index | 0.37/0.91 |
B-V color index | 0.78/1.41 |
Variable type | None/Suspected |
Astrometry | |
Radial velocity (Rv) | +25.3 km/s |
Proper motion (μ) | RA: 1,035.20 mas/yr Dec.: 109.26 mas/yr |
Parallax (π) | 113.81 ± 1.36 mas |
Distance | 28.7 ± 0.3 ly (8.8 ± 0.1 pc) |
Absolute magnitude (MV) | 5.83 |
Details | |
Mass | 0.74/? M☉ |
Radius | 0.58/? R☉ |
Luminosity | 0.42/? L☉ |
Temperature | 5305/? K |
Metallicity | 45% |
Rotation | ? |
Age | ? years |
Other designations | |
Database references | |
SIMBAD | data |
ARICNS | data |
41 Arae is a binary star system in the constellation Ara. The two stars share a highly elliptical orbit that takes several centuries to complete. The estimates of the period range from 693 to 2,200 years,[1] and the average separation of the two stars is about 210 AUs (or 210 times the average distance between the Earth and the Sun.)
This system has a relatively high proper motion, moving over a second of arc across the sky each year. The fainter member of the pair has a peculiar spectrum that shows a deficiency in metals, which, for astronomical purposes, are the elements heavier than Helium.
The stars in this system show low chromospheric activity, and have a net space velocity of 52 km/s relative to the Sun. This, in combination with their low metallicity, shows that the pair below to the old disk population.[2]
[edit] References
- ^ G. F. Porto de Mello, E. F. del Peloso, L. Ghezzi (2006). "Astrobiologically interesting stars within 10 parsecs of the Sun". Astrobiology 6 (2): 308-331.
- ^ M.-N. Perrin, G. Cayrel de Strobel, M. Dennefeld (1988). "High S/N detailed spectral analysis of four G and K dwarfs within 10 PC of the sun". Astronomy and Astrophysics 191 (2): 237-247.
[edit] External links
- 41 Arae 2 SolStation entry.