Jump to content

T Persei

From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Citation bot (talk | contribs) at 11:05, 8 October 2020 (Alter: pages, journal, title. Add: issue, s2cid, author pars. 1-1. Removed parameters. Formatted dashes. Some additions/deletions were actually parameter name changes. | You can use this bot yourself. Report bugs here. | Suggested by Abductive | Category:Objects with variable star designations | via #UCB_Category). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

T Persei
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 2h 19m 21.87884s[1]
Declination +58° 57′ 40.3271″[1]
Apparent magnitude (V) 8.34-9.70[2]
Characteristics
Spectral type M2Iab[3]
U−B color index +2.62[4]
B−V color index +2.33[4]
Variable type SRc[2]
Astrometry
Radial velocity (Rv)−40.85[5] km/s
Proper motion (μ) RA: 0.31[1] mas/yr
Dec.: −2.42[1] mas/yr
Parallax (π)2.15 ± 1.24 mas[1]
Distance2,345±55[6] pc
Absolute magnitude (MV)−6.90±0.07[6]
Details[6]
Mass9-12 M☉
Radius510±20 R☉
Luminosity45,700+4,400
−4,000 L☉
Surface gravity (log g)0.06±0.05 cgs
Temperature3,750±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
SIMBADdata

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.[7] It lies half a degree away from S Persei, another red supergiant Double Cluster member.

T Per is a semiregular variable star, whose brightness varies from magnitude 8.34 to 9.7 over a period of 2,430 days.[2] Unlike many red supergiants, it does not appear to have a long secondary period.[3][8]

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.[9]

References

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c 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.
  3. ^ a b 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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  4. ^ a b 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.
  5. ^ 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.
  6. ^ a b c 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ 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.
Retrieved from "https://en.wikipedia.org/w/index.php?title=T_Persei&oldid=982473990"