Variable star in the constellation Vulpecula
T Vulpeculae is a possiblebinary star system in the northernconstellation ofVulpecula , near the starZeta Cygni , close to the pair31 Vulpeculae and32 Vulpeculae .[ 11] apparent visual magnitude that ranges around 5.75.[ 3] light years , as determined from its annualparallax shift ofmas [ 2]
A well-studiedClassical Cepheid variable and one of the brightest known,[ 12] apparent magnitude of T Vulpeculae ranges from 5.41 to 6.09[ 4] [ 3] supergiant of spectral type F5 Ib.[ 5] [ 13] [ 14]
The companion star was detected in 1992;[ 12] A-type main-sequence star with a class of A0.8 V and 2.1 times the Sun's mass.[ 5] [ 15]
^ Kiss, Laszlo L. (July 1998)."A photometric and spectroscopic study of the brightest northern Cepheids - I. Observations" .Monthly Notices of the Royal Astronomical Society .297 (3): 825.Bibcode :1998MNRAS.297..825K .doi :10.1046/j.1365-8711.1998.01559.x ^a b c d e f Brown, A. G. A. ; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties" .Astronomy & Astrophysics 616 . A1.arXiv :1804.09365 Bibcode :2018A&A...616A...1G doi :10.1051/0004-6361/201833051 ^a b c Evans, Nancy Remage; et al. (July 2015). "Binary Properties from Cepheid Radial Velocities (CRaV)".The Astronomical Journal .150 (1): 18.arXiv :1505.05823 Bibcode :2015AJ....150...13E .doi :10.1088/0004-6256/150/1/13 .S2CID 54943097 . 13. ^a b c BSJ (4 January 2010)."T Vulpeculae" .AAVSO Website .American Association of Variable Star Observers . Retrieved24 January 2014 . ^a b c d e f g Evans, Nancy Remage; Bond, Howard E.; Schaefer, Gail H.; Mason, Brian D.; et al. (2013). "Binary Cepheids: Separations and Mass Ratios in 5M ⊙ Binaries".Astronomical Journal .146 (4): 93, 10.arXiv :1307.7123v1 Bibcode :2013AJ....146...93E .doi :10.1088/0004-6256/146/4/93 .S2CID 34133110 . ^a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters ,38 (5): 331,arXiv :1108.4971 Bibcode :2012AstL...38..331A ,doi :10.1134/S1063773712050015 ,S2CID 119257644 . ^ Gallenne, A.; et al. (May 2012). "Mean angular diameters, distances, and pulsation modes of the classical Cepheids FF Aquilae and T Vulpeculae. CHARA/FLUOR near-infrared interferometric observations".Astronomy & Astrophysics .541 : 5.arXiv :1203.6682 Bibcode :2012A&A...541A..87G .doi :10.1051/0004-6361/201219102 .S2CID 2424989 . A87. ^a b Gray, R. O.; et al. (2001)."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.Bibcode :2001AJ....121.2159G .doi :10.1086/319957 ^a b Marsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy".Astronomy Letters .39 (12): 851.Bibcode :2013AstL...39..851M .doi :10.1134/S1063773713120050 .S2CID 119788977 . ^ "HD 198726" .SIMBAD Centre de données astronomiques de Strasbourg . Retrieved18 August 2018 .^ Moore, Patrick (2000),Exploring the Night Sky with Binoculars ISBN 978-0521793902 ^a b Evans, Nancy R. (July 1992). "The luminosity of the classical Cepheid T VUL".Astronomical Journal .104 (1):216– 219.Bibcode :1992AJ....104..216E .doi :10.1086/116232 . ^ Sawyer, E. F. (1886)."On a new variable star in the Constellation Vulpecula" .Astronomische Nachrichten .113 (16): 265.Bibcode :1886AN....113..265S .doi :10.1002/asna.18861131608 . ^ Meyer, Ralf (August 2006). "T Vulpeculae: Maximum Times Covering 120 Years Show a Slight, Continuous Period Decrease".Open European Journal on Variable Stars .46 : 1.Bibcode :2006OEJV...46....1M . ^ Gallenne, A.; et al. (July 2015)."Robust high-contrast companion detection from interferometric observations. The CANDID algorithm and an application to six binary Cepheids" .Astronomy & Astrophysics .579 : 12.arXiv :1505.02715 Bibcode :2015A&A...579A..68G .doi :10.1051/0004-6361/201525917
