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| parallax_footnote = <ref name=aaa474_2_653/> | parallax_footnote = <ref name=aaa474_2_653/>
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<ref name=aaa474_2_653>{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | postscript=. |arxiv = 0708.1752 }}</ref> <ref name=aaa474_2_653>{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | postscript=. |arxiv = 0708.1752 }}</ref>

<ref name=Cardini2005>{{citation
| title=Mg II chromospheric radiative loss rates in cool active and quiet stars
| last1=Cardini | first1=D. | postscript=.
| journal=Astronomy and Astrophysics
| volume=430 | pages=303-311 | date=January 2005
| doi=10.1051/0004-6361:20041440 | bibcode=2005A&A...430..303C }}</ref>


<ref name=apjl674_1_L53>{{citation | display-authors=1 | last1=Stello | first1=D. | last2=Bruntt | first2=H. | last3=Preston | first3=H. | last4=Buzasi | first4=D. | title=Oscillating K Giants with the WIRE Satellite: Determination of Their Asteroseismic Masses | journal=The ] Letters | volume=674 | issue=1 | date=2008 | pages=L53–L56 | doi=10.1086/528936 | bibcode=2008ApJ...674L..53S | postscript=. |arxiv = 0801.2155 }}</ref> <ref name=apjl674_1_L53>{{citation | display-authors=1 | last1=Stello | first1=D. | last2=Bruntt | first2=H. | last3=Preston | first3=H. | last4=Buzasi | first4=D. | title=Oscillating K Giants with the WIRE Satellite: Determination of Their Asteroseismic Masses | journal=The ] Letters | volume=674 | issue=1 | date=2008 | pages=L53–L56 | doi=10.1086/528936 | bibcode=2008ApJ...674L..53S | postscript=. |arxiv = 0801.2155 }}</ref>

Revision as of 22:29, 20 July 2017

G Scorpii
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 17 49 51.48081
Declination −37° 02′ 35.8975″
Apparent magnitude (V) 3.21
Characteristics
Spectral type K2 III
U−B color index +1.19
B−V color index +1.17
Astrometry
Radial velocity (Rv)+24.7 km/s
Proper motion (μ) RA: 40.59 mas/yr
Dec.: 27.24 mas/yr
Parallax (π)25.92 ± 0.15 mas
Distance125.8 ± 0.7 ly
(38.6 ± 0.2 pc)
Absolute magnitude (MV)+0.24
Details
Mass1.44 ± 0.21 M☉
Radius16 R☉
Luminosity95 ± 6 L☉
Temperature4,538 K
Other designations
G Sco, CD–37 11907, FK5 669, HD 161892, HIP 87261, HR 6630, SAO 209318.
Database references
SIMBADdata

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. The measured angular diameter of the primary star is 3.94 ± 0.21 mas. At the estimated distance of this system, this yields a physical size of about 16 times the radius of the Sun.

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

References

  1. ^ 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. ^ Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 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:1953GCRV..C......0W.{{cite book}}: CS1 maint: postscript (link)
  5. Cardini, D. (January 2005), "Mg II chromospheric radiative loss rates in cool active and quiet stars", Astronomy and Astrophysics, 430: 303–311, Bibcode:2005A&A...430..303C, doi:10.1051/0004-6361:20041440.
  6. ^ 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.
  7. ^ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN 3540296921. The radius (R*) is given by:
    2 ⋅ R ∗ = ( 38.6 ⋅ 3.94 ⋅ 10 − 3 )   AU 0.0046491   AU / R ⨀ ≈ 32.7 ⋅ R ⨀ {\displaystyle {\begin{aligned}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{aligned}}}
  8. Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039
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