Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

T Persei

From Wikipedia, the free encyclopedia
Star in the constellation Perseus
T Persei

Avisual bandlight curve For T Persei, plotted from AAVSO data[1]
Observation data
Epoch J2000      Equinox J2000
ConstellationPerseus
Right ascension2h 19m 21.87717s[2]
Declination+58° 57′ 40.3455″[2]
Apparent magnitude (V)8.34-9.70[3]
Characteristics
Spectral typeM2Iab[4]
U−Bcolor index+2.62[5]
B−Vcolor index+2.33[5]
Variable typeSRc[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]
Distance2345±55[7] pc
Absolute magnitude (MV)−6.90±0.07[7]
Details[7]
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 ared supergiant located in theconstellation Perseus. It varies in brightness between magnitudes 8.3 and 9.7 and is considered to be a member of theDouble Cluster.

T Persei is a member of thePerseus OB1 association around the h and χ Perseiopen 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 fromS Persei, another red supergiant Double Cluster member.

Vojtěch Šafařík discovered that the star is avariable star in 1882.[9] It was listed with itsvariable star designation, T Persei, inAnnie Jump Cannon's 1907 workSecond Catalog of Variable Stars.[10] T Per is asemiregular 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 along secondary period.[4][11] It is relatively inactive for the red supergiant star, with low mass loss rate8×10−6 Solar_mass/year and no detectable dust shell.[12]

TheWashington Double Star Catalog lists T Persei as having a 9th magnitude companion0.1 arc-seconds away. This is derived fromHipparcos measurements. However, no other sources report a companion.[13]

References

[edit]
  1. ^"Download Data".aavso.org. AAVSO. Retrieved1 October 2021.
  2. ^abcdeBrown, 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.
  3. ^abcSamus, 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. ^abKiss, 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. ^abDucati, 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. ^abcBaron, 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. Retrieved19 December 2024.
  10. ^Cannon, Annie J. (1907)."Second catalogue of variable stars".Annals of Harvard College Observatory.55:1–94.Bibcode:1907AnHar..55....1C. Retrieved18 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.
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Star
clusters
NGC
Other
Nebulae
NGC
Other
Galaxies
NGC
Other
Galaxy clusters
Astronomical events
Retrieved from "https://en.wikipedia.org/w/index.php?title=T_Persei&oldid=1266538603"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2025 Movatter.jp