G Scorpii

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G Scorpii
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 17h 49m 51.48081s[1]
Declination −37° 02′ 35.8975″[1]
Apparent magnitude (V) 3.21[2]
Characteristics
Spectral type K2 III[3]
U−B color index +1.19[2]
B−V color index +1.17[2]
Astrometry
Radial velocity (Rv) +24.7[4] km/s
Proper motion (μ) RA: 40.59[1] mas/yr
Dec.: 27.24[1] mas/yr
Parallax (π) 25.92 ± 0.15[1] mas
Distance 125.8 ± 0.7 ly
(38.6 ± 0.2 pc)
Details
Mass 1.44 ± 0.21[5] M
Radius 16[6] R
Luminosity 95 ± 6[5] L
Temperature 4,538[5] K
Other designations
G Sco, CD–37 11907, FK5 669, HD 161892, HIP 87261, HR 6630, SAO 209318.

G Scorpii (G Sco) is a star in the constellation Scorpius. It is an orange K-type giant with an apparent magnitude of +3.19. It is approximately 126 light years from Earth.[1] The measured angular diameter of the primary star is 3.94 ± 0.21 mas.[7] At the estimated distance of this system, this yields a physical size of about 16 times the radius of the Sun.[6]

Just 8.5 arcminutes to the east is the globular cluster NGC 6441.

It was formerly known as "Gamma Telescopii" (γ Tel) and "Fuyue" (傅說) in ancient China.

See also[edit]

References[edit]

  1. ^ a b c d e f 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 Johnson, H. L. et al. (1966), UBVRIJKL photometry of the bright stars, Communications of the Lunar and Planetary Laboratory 4 (99), Bibcode:1966CoLPL...4...99J. 
  3. ^ Gray, R. O. et al. (July 2006), Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample, The Astronomical Journal 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637. 
  4. ^ Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:1953QB901.W495..... 
  5. ^ a b c Stello, D. et al. (2008), Oscillating K Giants with the WIRE Satellite: Determination of Their Asteroseismic Masses, The Astrophysical Journal Letters 674 (1): L53–L56, arXiv:0801.2155, Bibcode:2008ApJ...674L..53S, doi:10.1086/528936. 
  6. ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3 ed.), Birkhäuser, ISBN 3540296921 . The radius (R*) is given by:
    \begin{align} 2\cdot R_*
 & = \frac{(38.6\cdot 3.94\cdot 10^{-3})\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\
 & \approx 32.7\cdot R_{\bigodot}
\end{align}
  7. ^ Richichi; Percheron, I.; Khristoforova, M. (February 2005), CHARM2: An updated Catalog of High Angular Resolution Measurements, Astronomy and Astrophysics 431: 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039