Star in the constellation Andromeda
15 Andromedae Location of 15 Andromedae (circled)
Observation dataEpoch J2000.0 Equinox J2000.0 Constellation Andromeda Right ascension 23h 34m 37.53652s [ 1] Declination +40° 14′ 11.1795″[ 1] Apparent magnitude (V)5.55[ 2] Characteristics Spectral type A1 III,[ 3] [ 4] [ 5] B−Vcolor index ± 0.005[ 2] Variable type δ Sct [ 6] Astrometry Radial velocity (Rv )± 0.6[ 2] km/s Proper motion (μ)RA: -18.165mas /yr Dec.: −46.183[ 1] mas /yr Parallax (π)12.9406± 0.0973 mas [ 1] Distance 252 ± 2 ly pc ) Absolute magnitude (MV )± 0.16[ 7] Details[ 3] Mass 2.7 M ☉ Luminosity 27 L ☉ Surface gravity (log g )± 0.03[ 7] cgs Temperature 9,225 K Rotational velocity (v sin i )105[ 7] Age 130 Myr Other designations 15 And ,V340 And ,BD +39°5114FK5 1616HD 221756HIP 116354HR 8947SAO 73346PPM 64401[ 8] Database references SIMBAD data
Alight curve for V340 Andromedae, plotted fromTESS [ 9] 15 Andromedae , abbreviated15 And , is a single,[ 10] variable star [ 6] constellation ofAndromeda .15 Andromedae is theFlamsteed designation , while itsvariable star designation is V340 And.[ 8] apparent visual magnitude is 5.55,[ 2] light years , and it is moving further away with a heliocentricradial velocity of 13 km/s.[ 2]
Rufener and Bartholdi (1982) included the star (under the name HD 221756) in their list of 333 variable, microvariable and suspected variable stars, based on multicolorphotometry performed at several observatories in the 1960s and 1970s. However they were unable to conclusively demonstrate that the star's brightness varied.[ 11] [ 12] [ 13]
Depending on the source, this star has been classified as agiant star with astellar classification of A1 III,[ 3] A-type main-sequence star with a class of A1 Va,[ 4] Lambda Boötis star with a class of kA1hA3mA0.5 Va+.[ 5] Delta Scuti variable that changes in brightness by 0.03 magnitude.[ 6] [ 14] [ 3] projected rotational velocity of 105 km/s.[ 7] mass of the Sun and is radiating 27 times theSun's luminosity from itsphotosphere at aneffective temperature of 9,225 K.[ 3]
This system has anexcess emission of infrared radiation that suggests the presence of an orbiting disk of dust at a distance of around 50 AU from the host star.[ 3]
^a b c d 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 d e 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 . ^a b c d e f Wyatt, M. C.; et al. (July 2007), "Steady State Evolution of Debris Disks around A Stars",The Astrophysical Journal ,663 (1):365– 382,arXiv :astro-ph/0703608 Bibcode :2007ApJ...663..365W ,doi :10.1086/518404 ,S2CID 18883195 ^a b Paunzen, E.; et al. (July 2001), "A spectroscopic survey for λ Bootis stars. II. The observational data",Astronomy and Astrophysics ,373 (2):625– 632,Bibcode :2001A&A...373..625P ,doi :10.1051/0004-6361:20010630 ^a b Murphy, Simon J.; et al. (2015), "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue",Publications of the Astronomical Society of Australia ,32 : e036,arXiv :1508.03633 Bibcode :2015PASA...32...36M ,doi :10.1017/pasa.2015.34 ,ISSN 1323-3580 ,S2CID 59405545 . ^a b c Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General catalogue of variable stars: Version GCVS 5.1",Astronomy Reports ,61 (1): 80,Bibcode :2017ARep...61...80S ,doi :10.1134/S1063772917010085 ,S2CID 125853869 . ^a b c d Paunzen, E.; et al. (November 2002), "The status of Galactic field λ Bootis stars in the post-Hipparcos era",Monthly Notices of the Royal Astronomical Society ,336 (3):1030– 1042,arXiv :astro-ph/0207488 Bibcode :2002MNRAS.336.1030P ,doi :10.1046/j.1365-8711.2002.05865.x S2CID 2389489 . ^a b "15 And" .SIMBAD Centre de données astronomiques de Strasbourg . RetrievedSeptember 20, 2018 .^ "MAST: Barbara A. Mikulski Archive for Space Telescopes" . Space Telescope Science Institute. Retrieved8 December 2021 .^ 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,arXiv :0806.2878 Bibcode :2008MNRAS.389..869E ,doi :10.1111/j.1365-2966.2008.13596.x S2CID 14878976 . ^ Rufener, F.; Bartholdi, P. (June 1982)."List of 333 variable microvariable or suspected variable stars detected in the Geneva photometry" .Astronomy and Astrophysics, Supplement Series .48 :503– 511.Bibcode :1982A&AS...48..503R . Retrieved5 November 2024 . ^ Paunzen, E.; Handler, G. (March 1996)."Pulsation of HD 83041 and HD 221756" .Information Bulletin on Variable Stars .4301 : 1.Bibcode :1996IBVS.4301....1P . Retrieved5 November 2024 . ^ Kazarovets, E. V.; Samus, N. N. (April 1997)."The 73rd Name-List of Variable Stars" (PDF) .Information Bulletin on Variable Stars .4471 :1– 45.Bibcode :1997IBVS.4471....1K . Retrieved5 November 2024 . ^ Dorokhova, T. N.; et al. (March 2008), "The pulsating λ Bootis star 15 Andromedae: results from a three-site photometry campaign.",Astronomy and Astrophysics ,480 (1):187– 191,Bibcode :2008A&A...480..187D ,doi :10.1051/0004-6361:20078750
