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Gamma Sagittae

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Gamma Sagittae
Die ligging van Gamma Sagittae (in die rooi sirkel).
Die ligging van Gamma Sagittae (in die rooi sirkel).
Sterrebeeld Pyl
Spektraaltipe M0 III[1][2][3]
Soort Rooireus
Waarnemingsdata (Epog J2000)
Regte klimming 19h 58m 45.42863s[4]
Deklinasie +19° 29′ 31.7281″[4]
Skynmagnitude (m) 3,47[5]
Absolute magnitude (M) -1,11[6]
B-V-kleurindeks  +1,57[5]
U-B-kleurindeks  +1,93[5]
Besonderhede
Massa (M☉) 1,37[7]
Radius (R☉) 55,13±3,29[8]
Ouderdom (jaar) 2,35 miljard[2]
Temperatuur (K) 3 862±40[2]
Afstand (ligjaar) 258
Metaalinhoud [Fe/H] -0,14[8]
Ander name
12 Sagittae, BD+19° 4229 FK5 752, HD 189319, HIP 98337, HR 7635, SAO 105500, GC 27672, PPM 137344
Portaal  Portaalicoon   Sterrekunde

Gamma Sagittae (afgekort as γ Sge) is die helderste ster in die noordelike sterrebeeld Pyl (Sagitta). Dit is ’n enkelster[9] wat teen ’n skynbare magnitude van 3,47[5] met die blote oog sigbaar is. Volgens parallaksmetings is dit sowat 258 ligjare van die Son af. Dit beweeg nader aan ons teen ’n radiale snelheid van -34 km/s.[10]

Dit is ’n geëvolueerde rooireus met ’n sterreklassifikasie van M0 III.[11] Dit is sowat 2,35 miljard jaar oud,[2] en het ’n massa van sowat 1,37 keer dié van die Son[7] en ’n radius van sowat 55 keer die Son s’n.[8] Sy ligsterkte is omtrent 562 keer dié van die Son[8] en sy effektiewe temperatuur is 3 862 K.[2]

Verwysings

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  1. ↑ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  2. ↑ 2,0 2,1 2,2 2,3 2,4 Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". Astronomical Journal. 150 (3). 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88.
  3. ↑ Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/mk. Oorspronklik gepubliseer in: Lowell Observatory (Oktober 2014). 1. Bibcode:2014yCat....1.2023S.
  4. ↑ 4,0 4,1 van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  5. ↑ 5,0 5,1 5,2 5,3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  6. ↑ Setiawan, J. et al. (Julie 2004), "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch", Astronomy and Astrophysics 421: 241–254, doi:10.1051/0004-6361:20041042-1, Bibcode: 2004A&A...421..241S. 
  7. ↑ 7,0 7,1 Reffert, Sabine; Bergmann, Christoph; Quirrenbach, Andreas; Trifonov, Trifon; Künstler, Andreas (2015). "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity". Astronomy & Astrophysics. 574: A116. arXiv:1412.4634. Bibcode:2015A&A...574A.116R. doi:10.1051/0004-6361/201322360. hdl:10722/215277.
  8. ↑ 8,0 8,1 8,2 8,3 Piau, L.; Kervella, P.; Dib, S.; Hauschildt, P. (2011). "Surface convection and red-giant radius measurements". Astronomy and Astrophysics. 526: 12. arXiv:1010.3649. Bibcode:2011A&A...526A.100P. doi:10.1051/0004-6361/201014442. A100.
  9. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  10. ↑ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272.
  11. ↑ Wittkowski, M.; Hummel, C. A.; Aufdenberg, J. P.; Roccatagliata, V. (Desember 2006), "Tests of stellar model atmospheres by optical interferometry. III. NPOI and VINCI interferometry of the M0 giant γ Sagittae covering 0.5-2.2 μm", Astronomy and Astrophysics 460 (3): 843–853, doi:10.1051/0004-6361:20065853, Bibcode: 2006A&A...460..843W. 

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