T Persei

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T Persei
TPerLightCurve.png
A visual band light curve For T Persei, plotted from AAVSO data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 2h 19m 21.87717s [2]
Declination +58° 57′ 40.3455″ [2]
Apparent magnitude  (V)8.34-9.70 [3]
Characteristics
Spectral type M2Iab [4]
U−B color index +2.62 [5]
B−V color index +2.33 [5]
Variable type SRc [3]
Astrometry
Radial velocity (Rv)−40.85 [6] km/s
Proper motion (μ)RA: −1.237 [2] mas/yr
Dec.: −0.186 [2] mas/yr
Parallax (π)0.4119±0.0237  mas [2]
Distance 2345±55 [7]   pc
Absolute magnitude  (MV)−6.90±0.07 [7]
Details [7]
Mass 9-12  M☉
Radius 510±20  R☉
Luminosity 45,700+4,400
−4,000  L☉
Surface gravity (log g)0.06±0.05  cgs
Temperature 3,750±60  K
Metallicity [Fe/H]−0.35  dex
Other designations
T  Per, HD 14142, HIP  10829, BD+58°439, WDS  J02194+5858, 2MASS  J02192186+5857403, AAVSO  0212+58
Database references
SIMBAD data

T Persei is a red supergiant located in the constellation Perseus. It varies in brightness between magnitudes 8.3 and 9.7 and is considered to be a member of the Double Cluster.

T Persei is a member of the Perseus OB1 association around the h and χ Persei open clusters, around 2 degrees north of the centre of the clusters. It is generally treated as an outlying member of the clusters. [8] It lies half a degree away from S Persei, another red supergiant Double Cluster member.

Vojtěch Šafařík discovered that the star is a variable star in 1882. [9] It was listed with its variable star designation, T Persei, in Annie Jump Cannon's 1907 work Second Catalog of Variable Stars. [10] T Per is a semiregular variable star, whose brightness varies from magnitude 8.34 to 9.7 over a period of 2,430 days. [3] Unlike many red supergiants, it does not appear to have a long secondary period. [4] [11] It is relatively inactive for the red supergiant star, with low mass loss rate 8×10−6  Solar_mass /year and no detectable dust shell. [12]

The Washington Double Star Catalog lists T Persei as having a 9th magnitude companion 0.1  arc-seconds away. This is derived from Hipparcos measurements. However, no other sources report a companion. [13]

References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 4 5 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 at VizieR.
  3. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. 1 2 Kiss, L. L.; Szabó, Gy. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society. 372 (4): 1721–1734. arXiv: astro-ph/0608438 . Bibcode:2006MNRAS.372.1721K. doi: 10.1111/j.1365-2966.2006.10973.x . S2CID   5203133.
  5. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  6. ↑ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv: astro-ph/0409579 . Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID   17804304.
  7. 1 2 3 Baron, F.; Monnier, J. D.; Kiss, L. L.; Neilson, H. R.; Zhao, M.; Anderson, M.; Aarnio, A.; Pedretti, E.; Thureau, N.; Ten Brummelaar, T. A.; Ridgway, S. T.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Turner, N. (2014). "Chara/mirc Observations of Two M Supergiants in Perseus Ob1: Temperature, Bayesian Modeling, and Compressed Sensing Imaging". The Astrophysical Journal. 785 (1): 46. arXiv: 1405.4032 . Bibcode:2014ApJ...785...46B. doi:10.1088/0004-637X/785/1/46. S2CID   17085548.
  8. ↑ Gonzalez, Guillermo; Wallerstein, George (2000). "Elemental Abundances in Evolved Supergiants. II. The Young Clusters H and χ Persei". The Astronomical Journal. 119 (4): 1839. Bibcode:2000AJ....119.1839G. doi: 10.1086/301319 .
  9. ↑ Payne-Gaposchkin, Cecilia (1952). "Variable stars in Milton field 3". Annals of Harvard College Observatory. 118: 193–203. Bibcode:1952AnHar.118..193P . Retrieved 19 December 2024.
  10. ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C . Retrieved 18 December 2024.
  11. ↑ Percy, John R.; Sato, Hiromitsu (2009). "Long Secondary Periods in Pulsating Red Supergiant Stars". Journal of the Royal Astronomical Society of Canada. 103 (1): 11. Bibcode:2009JRASC.103...11P.
  12. ↑ Gordon, Michael S.; Humphreys, Roberta M.; Jones, Terry J.; Shenoy, Dinesh; Gehrz, Robert D.; Helton, L. Andrew; Marengo, Massimo; Hinz, Philip M.; Hoffmann, William F. (2017). "Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S per, and the Normal Red Supergiants RS per and T per". The Astronomical Journal. 155 (5): 212. arXiv: 1708.00018 . Bibcode:2018AJ....155..212G. doi: 10.3847/1538-3881/aab961 . S2CID   73650032.
  13. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
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