G Scorpii

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G Scorpii
Scorpius constellation map.svg
Red circle.svg
Location of G Scorpii (circled)
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
Evolutionary stage horizontal branch [3]
Spectral type K2 III [4]
U−B color index +1.19 [2]
B−V color index +1.17 [2]
Astrometry
Radial velocity (Rv)+24.7 [5]  km/s
Proper motion (μ)RA: 40.59 [1]   mas/yr
Dec.: 27.24 [1]   mas/yr
Parallax (π)25.92 ± 0.15  mas [1]
Distance 125.8 ± 0.7  ly
(38.6 ± 0.2  pc)
Absolute magnitude  (MV)+0.24 [6]
Details [3]
Mass 1.2±0.2  M☉
Radius 20±1  R☉
Luminosity 93±4  L☉
Surface gravity (log g)2.2  cgs
Temperature 4,535±125  K
Metallicity [Fe/H]−0.20 [7]   dex
Rotational velocity (v sin i)<1.0 [8]  km/s
Other designations
Fuyue, G Sco, γ Tel, FK5  669, HD  161892, HIP  87261, HR  6630, SAO  209318
Database references
SIMBAD data

G Scorpii (abbreviated G Sco), also named Fuyue, is a giant star in the constellation of Scorpius. It has an apparent magnitude of +3.19. It is approximately 126 light-years from the Sun.

Contents

Nomenclature

G Scorpii below and right (ie. west) of NGC 6441 NGC 6441 HST 10775 R814B606.png
G Scorpii below and right (ie. west) of NGC 6441

G Scorpii is the star's Bayer designation. It was formerly situated in the constellation of Telescopium where it was designated γ Telescopii, Latinised to Gamma Telescopii. [9] It was resited in Scorpius and redesignated G Scorpii by Benjamin Apthorp Gould. On 30 June 2017 it was included in the List of IAU-approved Star Names. [10]

G Scorpii bore the traditional name Fuyue (simplified Chinese :傅说; traditional Chinese :傅說) in ancient China. Fu Yue was a former slave that became a high-ranking minister to Shang dynasty ruler Wu Ding.

Properties

G Scorpii is an orange K-type giant. The measured angular diameter is 3.94±0.21  mas . [11] At the estimated distance of this system, this yields a physical size of about 16 times the radius of the Sun. [12] Calculations based on its physical properties give a diameter of about 20 R☉. With an effective surface temperature of 4,535  K , it has a bolometric luminosity of 93  L☉. [3]

Evolutionary models show that G Scorpii has probably left the red giant branch and is now fusing helium in its core. This makes it a red clump star, at the cool end of the horizontal branch. [3]

Just 5 arcminutes to the east is the globular cluster NGC 6441. [13] At magnitude 3.2, G Scorpii is around 40 times brighter than the entire globular cluster.

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References

  1. 1 2 3 4 5 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, S2CID   18759600.
  2. 1 2 3 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. 1 2 3 4 Kallinger, T.; Beck, P. G.; Hekker, S.; Huber, D.; Kuschnig, R.; Rockenbauer, M.; Winter, P. M.; Weiss, W. W.; Handler, G.; Moffat, A. F. J.; Pigulski, A.; Popowicz, A.; Wade, G. A.; Zwintz, K. (2019), "Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation", Astronomy and Astrophysics, 624: A35, arXiv: 1902.07531 , Bibcode:2019A&A...624A..35K, doi:10.1051/0004-6361/201834514, S2CID   102486794.
  4. ↑ 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, S2CID   119476992.
  5. ↑ Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
  6. ↑ Cardini, D. (January 2005), "Mg II chromospheric radiative loss rates in cool active and quiet stars", Astronomy and Astrophysics, 430: 303–311, arXiv: astro-ph/0409683 , Bibcode:2005A&A...430..303C, doi:10.1051/0004-6361:20041440, S2CID   12136256.
  7. ↑ Charbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (2020), "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era", Astronomy and Astrophysics, 633: A34, arXiv: 1910.12732 , Bibcode:2020A&A...633A..34C, doi:10.1051/0004-6361/201936360, S2CID   204907220.
  8. ↑ De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (2014), "A catalog of rotational and radial velocities for evolved stars. V. Southern stars", Astronomy and Astrophysics, 561: A126, arXiv: 1312.3474 , Bibcode:2014A&A...561A.126D, doi:10.1051/0004-6361/201220762, S2CID   54046583.
  9. ↑ Ian Ridpath, "Telescopium", Star Tales, retrieved 2020-05-23.
  10. ↑ Naming Stars, IAU.org, retrieved 16 December 2017.
  11. ↑ 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
  12. ↑ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN   3540296921. The radius (R*) is given by:
  13. ↑ O'Meara, Stephen James (2013), Deep-Sky Companions: Southern Gems, Cambridge University Press, pp. 360–363, Bibcode:2013dcsg.book.....O, ISBN   978-1139851541.
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