Variable star in Taurus
SZ Tauri Observation dataEpoch J2000 Equinox J2000 Constellation Taurus [ 2] Right ascension 04h 37m 14.778s [ 3] Declination +18° 32′ 34.93″[ 3] Apparent magnitude (V)6.39 to 6.69 [ 4] Characteristics Evolutionary stage Supergiant Spectral type F5Ib-F9.5Ib[ 5] B−Vcolor index 0.810± 0.025[ 2] Variable type δ Cep [ 6] Astrometry Radial velocity (Rv )−1.2± 0.2[ 7] km/s Proper motion (μ)RA: −4.403mas /yr [ 3] Dec.: −5.232mas /yr [ 3] Parallax (π)1.5741± 0.028 mas [ 3] Distance 2,070 ± 40 ly pc ) Details Mass 6.1± 0.8[ 8] M ☉ Radius 42.2± 3.0[ 9] R ☉ Luminosity 1,905[ 10] L ☉ Surface gravity (log g )2.0–2.2[ 11] cgs Temperature 6,015–6,420[ 10] K Metallicity [Fe/H] 0.08[ 11] dex Age 69–80[ 12] Myr Other designations SZ Tau ,BD +18 661GC 5621HD 29260HIP 21517SAO 94036PPM 120081[ 13] Database references SIMBAD data
SZ Tauri is avariable star in theequatorial constellation ofTaurus . The brightness of this star varies from anapparent visual magnitude of 6.39 down to 6.69 with a period of 3.149 days,[ 4] naked eye . The distance to this star is approximately 2,070 light years based onparallax measurements.[ 3] binary system , but the evidence is inconclusive.[ 14]
The variability of this star was announced byK. Schwarzschild in 1911 and was given a preliminary designation of 41.1910 with a period of[ 15] [ 16] H. S. Leavitt extended the study up to 1914, producing alight curve with a period of[ 17] spectral study byH. Shapley showed that theclass of thispulsating Cepheid variable changed along thelight curve , ranging from F7 at minimum up to A9 at peak luminosity.[ 18] Y. N. Efremov suggested in 1964 that this star may be a halo member of theNGC 1647 open cluster ,[ 19] proper motion match.[ 20] classical Cepheid byW. P. Gieren in 1985.[ 21]
In theGeneral Catalogue of Variable Stars , SZ Tau is classified as a Delta Cepheid of type DCEPS, which shows a nearly symmetric light curve with a small amplitude.[ 6] overtone [ 19] evolutionary terms is undergoing its second crossing of the Cepheidinstability strip .[ 12] [ 22] [ 12] [ 12] [ 8] [ 9] effective temperature , radius, and spectral type of the star vary across each pulsation cycle.[ 10]
^ "MAST: Barbara A. Mikulski Archive for Space Telescopes" . Space Telescope Science Institute. Retrieved8 December 2021 .^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 . ^a b c d e Brown, A. G. A. ; et al. (Gaia collaboration) (2021)."Gaia Early Data Release 3: Summary of the contents and survey properties" .Astronomy & Astrophysics 649 : A1.arXiv :2012.01533 Bibcode :2021A&A...649A...1G .doi :10.1051/0004-6361/202039657 S2CID 227254300 . (Erratum: doi :10.1051/0004-6361/202039657e ) . Gaia EDR3 record for this source atVizieR .^a b Klagyivik, P.; Szabados, L. (September 2009), "Observational studies of Cepheid amplitudes. I. Period-amplitude relationships for Galactic Cepheids and interrelation of amplitudes",Astronomy and Astrophysics ,504 (3):959– 972,arXiv :0908.3561 Bibcode :2009A&A...504..959K ,doi :10.1051/0004-6361/200811464 ,S2CID 18283579 . ^ Kraft, Robert P. (March 1960), "Color Excesses for Supergiants and Classical Cepheids. I. Calibration of the Gband Photometry",Astrophysical Journal ,131 : 330,Bibcode :1960ApJ...131..330K ,doi :10.1086/146837 . ^a b Samus', N. N; et al. (2017), "General catalogue of variable stars",Astronomy Reports , GCVS 5.1,61 (1): 80,Bibcode :2017ARep...61...80S ,doi :10.1134/S1063772917010085 ,S2CID 125853869 . ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system",Astronomy Letters ,32 (11):759– 771,arXiv :1606.08053 Bibcode :2006AstL...32..759G ,doi :10.1134/S1063773706110065 ,S2CID 119231169 . ^a b Marconi, Marcella; et al. (July 2020), "Predicted Masses of Galactic Cepheids in the Gaia Data Release 2",The Astrophysical Journal Letters ,898 (1): L7,arXiv :2006.16610 Bibcode :2020ApJ...898L...7M ,doi :10.3847/2041-8213/aba12b S2CID 220265392 , L7. ^a b Postma, Joseph E.; Milone, E. F. (June 2006), "Observations and Analyses of the Cepheid SZ Tauri",Bulletin of the American Astronomical Society ,38 : 144,Bibcode :2006AAS...208.6506P . ^a b c Sanwal, B. B.; Rautela, B. S. (January 1989), "Spectrophotometric Study of the Cepheids DT-Cygni and SZ-Tauri",Astrophysics and Space Science ,151 (2):209– 215,Bibcode :1989Ap&SS.151..209S ,doi :10.1007/BF00648379 ,S2CID 119557969 . ^a b Andrievsky, S. M.; et al. (2013), "Barium abundances in Cepheids",Monthly Notices of the Royal Astronomical Society ,428 (4): 3252,arXiv :1210.6211 Bibcode :2013MNRAS.428.3252A ,doi :10.1093/mnras/sts270 ^a b c d Fadeyev, Yu. A. (November 2015), "Evolution, pulsation and period change in the Cepheid SZ Tau",Astronomy Letters ,41 (11):640– 645,arXiv :1507.04715 Bibcode :2015AstL...41..640F ,doi :10.1134/S1063773715110031 ,S2CID 255192877 . ^ "SZ Tau" ,SIMBAD Centre de données astronomiques de Strasbourg , retrieved2022-03-10 .^ Kervella, Pierre; et al. (March 2019), "Multiplicity of Galactic Cepheids and RR Lyrae stars from Gaia DR2. II. Resolved common proper motion pairs",Astronomy & Astrophysics ,623 : 40,arXiv :1908.00545 Bibcode :2019A&A...623A.117K ,doi :10.1051/0004-6361/201834211 ,S2CID 261941148 , A117. ^ Schwarzschild, Karl (October 1911),"Über den Lichtwechsel des Veränderlichen 41.1910 Tauri" ,Astronomische Nachrichten (in German),189 (20):345– 356,Bibcode :1911AN....189..345S ,doi :10.1002/asna.2101892002 .^ Shapley, H. (May 1913),"Concerning the ellipsoidal variables SZ Tauri and S Antliae" ,Astronomische Nachrichten ,194 (21):353– 359,Bibcode :1913AN....194..353S ,doi :10.1002/asna.19131942102 .^ Leavitt, Henrietta S. ;Pickering, Edward C. (November 1914), "Observations of SZ Tauri",Harvard College Observatory Circular ,186 :1– 4,Bibcode :1914HarCi.186....1L .^ Shapley, H. (December 1916), "The variations in spectral type of twenty Cepheid variables",Astrophysical Journal ,44 :273– 291,Bibcode :1916ApJ....44..273S ,doi :10.1086/142295 . ^a b Turner, David G. (November 1992),"Galactic Clusters With Associated Cepheid Variables. III. NGC 1647 and SZ Tauri" ,Astronomical Journal ,104 : 1865,Bibcode :1992AJ....104.1865T ,doi :10.1086/116363 . ^ Baumgardt, H.; et al. (October 2000), "Absolute proper motions of open clusters. I. Observational data",Astronomy and Astrophysics Supplement ,146 (2):251– 258,arXiv :astro-ph/0010306 Bibcode :2000A&AS..146..251B ,doi :10.1051/aas:2000362 ,S2CID 7180188 . ^ Gieren, W. P. (July 1985), "Physical properties of the cepheids RT Aurigae and SZ Tauri",Astronomy and Astrophysics ,148 :138– 144,Bibcode :1985A&A...148..138G . ^ Trammell, Susan R. (December 1987), "The Changing Period of SZ Tauri",The Journal of the American Association of Variable Star Observers ,16 (2):104– 106,Bibcode :1987JAVSO..16..104T .
