14 Persei

Star in the constellation Perseus 14 Persei Perseus constellation map.svg center right 280 Red circle.svg 10 14 Persei 753 556 Location of 14 Per (circled) J2000 02 44 05.15918340647020322856192 +44 17 49.3488 5.432008PASJ...60..781T 0805.2434 Stellar Parameters and Elemental Abundances of Late-G Giants Publications of the Astronomical Society of Japan 60 4 781 Takeda Yoichi Sato Bun'ei Murata Daisuke 2008 10.1093/pasj/60.4.781 Perseus G0Ib +0.862014AJ....147..137L Parameters and Abundances in Luminous Stars The Astronomical Journal 147 6 137 Luck R. Earle 2014 10.1088/0004-6256/147/6/137 free −1.22 0.15 2.902 −6.682 1.7466 0.0989 −1.57 4.03 57.4 3.7 6.5 372 5,624 1.42 0.00 8.72014PASJ...66...91T 1406.7066 Spectroscopic study on the beryllium abundances of red giant stars Publications of the Astronomical Society of Japan 66 5 91 Takeda Yoichi Tajitsu Akito 2014 10.1093/pasj/psu066 162 14 Per +43°566 1077 16901 12768 800 38289 14 Per 2019-03-31 14+Persei 14 Persei is a single starEggleton P. P. Tokovinin A. A. A catalogue of multiplicity among bright stellar systems Monthly Notices of the Royal Astronomical Society 389 2 869–879 September 2008 10.1111/j.1365-2966.2008.13596.x free 2008MNRAS.389..869E . 0806.2878 14878976 in the northern constellation Perseus, located roughly 1,900 light years away from the Sun. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude is 5.43. The object is slowly moving closer to the Earth with a heliocentric radial velocity of −1.2 km/s. The spectral classification of 14 Persei is as a G0 yellow supergiant, but in other respects it appears to be a giant star. The class has been given as G0Ib-II Ca1 CH-11980ApJS...42..541K Revised MK spectral types for G, K, and M stars Astrophysical Journal Supplement Series 42 541 Keenan P. C. Pitts R. E. 1980 10.1086/190662 free or G0Ib-IIa Ca1,1989ApJS...71..245K The Perkins catalog of revised MK types for the cooler stars Astrophysical Journal Supplement Series 71 245 Keenan Philip C. McNeil Raymond C. 1989 10.1086/191373 where the abundance suffixes indicate stronger Calcium lines than expected for its class, or weaker hydrocarbons. Other analyses of the spectrum give a class of G0Ib.2001AJ....121.2159G The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. II. Basic Parameters of Program Stars and the Role of Microturbulence The Astronomical Journal 121 4 2159 Gray R. O. Graham P. W. Hoyt S. R. 2001 10.1086/319957 free Stellar models of 14 Persei yield an estimated mass four times that of the Sun and an age of 162 million years. It has expanded to 57 times the Sun's radius and has a projected rotational velocity of 8.7 km/s. The star is radiating 372 times as much luminosity compared to the Sun from its enlarged photosphere at an effective temperature of 5,624 K. 14 Persei has been calculated to lie within the Cepheid instability strip although it is not considered to be variable. Uncertainty in the absolute magnitude means that the star may actually lie near the instability strip but not on it. Small periodic radial velocity variations are seen, but an order of magnitude or more smaller than for Cepheid variables and with longer periods than would be expected for pulsations. The cause of the radial velocity changes and the difference between variable and non-variable stars within the instability strip is unknown.1998ApJ...494..342B A Precision Velocity Study of Photometrically Stable Stars in the Cepheid Instability Strip The Astrophysical Journal 494 342–365 Butler R. Paul 1 1998 10.1086/305195 119678211 References Category:Perseus (constellation) Persei, 14 Category:G-type supergiants 0800 016901 012768 BD+43 566