41 G. Arae

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41 G. Arae A
Observation data
Epoch J2000      Equinox J2000
Constellation Ara
Right ascension 17h 19m 03.83574s[1]
Declination −46° 38′ 10.4467″[1]
Apparent magnitude (V) 5.469
Characteristics
Spectral type G8V[2]
U−B color index 0.38
B−V color index 0.80[2]
R−I color index 0.41[2]
Astrometry
Radial velocity (Rv) 25.3 ± 0.1[3] km/s
Proper motion (μ) RA: 1037.56[1] mas/yr
Dec.: 108.99[1] mas/yr
Parallax (π) 113.61 ± 0.69[1] mas
Distance 28.7 ± 0.2 ly
(8.80 ± 0.05 pc)
Absolute magnitude (MV) 6.28
Orbit
Companion 41 G. Arae B
Period (P) 2204.982 yr
Semi-major axis (a) 23.9"
Eccentricity (e) 0.901
Inclination (i) 44.88°
Longitude of the node (Ω) 137.02°
Periastron epoch (T) 1907.765
Details
Mass 0.810[4] M
Radius 0.79[4] R
Luminosity 0.42 L
Surface gravity (log g) 4.5[2] cgs
Temperature 5,305[2] K
Metallicity [Fe/H] −0.35[2] dex
Rotational velocity (v sin i) 4.5[5] km/s
Age (5.5–6.3) × 109[6] years
Other designations
41 G. Arae, 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 G. Arae or GJ 666 A is a binary star system in the constellation Ara. Although often called just 41 Arae, it is more accurate to call it 41 G. Arae, as the number 41 is the Gould designation (Flamsteed only covered the northern hemisphere).

The primary star in this system is a G-type main sequence star with a stellar classification of G8V. It has about 81% of the mass of the Sun, and 79% of the Sun's radius.[4] 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.[citation needed] No planetary companions have been detected in orbit around these stars.[7]

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,[8] 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 space velocity components of this system are [U, V, W] = [+38, +30, −19] km/s.[2] 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 belongs to the old disk population.[2]

References[edit]

  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 
  2. ^ a b c d e f g h Perrin, M.-N.; Cayrel de Strobel, G.; Dennefeld, M. (February 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, Bibcode:1988A&A...191..237P 
  3. ^ Nordström, B. et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959 
  4. ^ a b c Takeda, G. et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~ 1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series 168 (2): 297−318, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763 
  5. ^ Schröder, C.; Reiners, A.; Schmitt, J. H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics 493 (3): 1099−1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377 
  6. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785 
  7. ^ Santos, N. C. et al. (July 2005), "Spectroscopic metallicities for planet-host stars: Extending the samples", Astronomy and Astrophysics 437 (3): 1127−1133, arXiv:astro-ph/0504154, Bibcode:2005A&A...437.1127S, doi:10.1051/0004-6361:20052895 
  8. ^ de Mello, G. F. Porto; del Peloso, E. F.; Ghezzi, L. (2006), "Astrobiologically interesting stars within 10 parsecs of the Sun", Astrobiology 6 (2): 308–331, arXiv:astro-ph/0511180, Bibcode:2006AsBio...6..308P, doi:10.1089/ast.2006.6.308, PMID 16689649 

External links[edit]