Die ligging van Gamma Sagittae (in die rooi sirkel).
Spektraaltipe M0 III
Regte klimming 19h 58m 45.42863s
Deklinasie +19° 29′ 31.7281″
Skynmagnitude (m) 3,47
Absolute magnitude (M) -1,11
Massa (M☉) 1,37
Radius (R☉) 55,13±3,29
Ouderdom (jaar) 2,35 miljard
Temperatuur (K) 3 862±40
Afstand (ligjaar) 258
Metaalinhoud [Fe/H] -0,14
12 Sagittae, BD+19° 4229 FK5 752, HD 189319, HIP 98337, HR 7635, SAO 105500, GC 27672, PPM 137344
Gamma Sagittae (afgekort as γ Sge) is die helderste ster in die noordelike sterrebeeld Pyl (Sagitta). Dit is ’n enkelster wat teen ’n skynbare magnitude van 3,47 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.
Dit is ’n geëvolueerde rooireus met ’n sterreklassifikasie van M0 III. Dit is sowat 2,35 miljard jaar oud, en het ’n massa van sowat 1,37 keer dié van die Son en ’n radius van sowat 55 keer die Son s’n. Sy ligsterkte is omtrent 562 keer dié van die Son en sy effektiewe temperatuur is 3 862 K.
↑ 2,0 2,1 2,2 2,3 2,4 (2015) “Abundances in the Local Region. I. G and K Giants”. Astronomical Journal 150 (3). doi:10.1088/0004-6256/150/3/88.
↑ (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.
↑ 4,0 4,1 van Leeuwen, F. (2007). “Validation of the New Hipparcos Reduction”. Astronomy and Astrophysics 474 (2): 653–64. doi:10.1051/0004-6361:20078357.
↑ 5,0 5,1 5,2 5,3 (2002) “VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system”. CDS/ADC Collection of Electronic Catalogues 2237.
↑ 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.
↑ 7,0 7,1 (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. doi:10.1051/0004-6361/201322360.
↑ 8,0 8,1 8,2 8,3 (2011) “Surface convection and red-giant radius measurements”. Astronomy and Astrophysics 526: 12. doi:10.1051/0004-6361/201014442. A100.
↑ (2005) “Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters”. Astronomy and Astrophysics 430: 165. doi:10.1051/0004-6361:20041272.
↑ 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.
Kaler, James B. "GAMMA SGE (Gamma Sagittae)". STARS. University of Illinois. Besoek op 2017-11-30.
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Die bladsy is laas op 13 Julie 2019 om 11:28 bygewerk.