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41 Arae - Wikipedia, the free encyclopedia

41 Arae

From Wikipedia, the free encyclopedia

41 Arae A
Observation data
Epoch J2000
Constellation
(pronunciation)
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
41 Ara, GJ 666, HR 6416, CD -46°11370, HD 156274, LHS 444, LTT 6886, GCTP 3919.00, SAO 227816, NSV 21372, CP(D)-46 8513, BSO 13, LPM 636, LFT 1334, HIP 84720.
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

  1. ^ 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. doi:10.1089/ast.2006.6.308. 
  2. ^ 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


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