T Cephei

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T Cephei
TCepheiLocation.jpg
Region of NGC 7023, T Cephei is marked with a green arrow
Credit: NASA, ESA and Digitized Sky Survey 2
Observation data
Epoch J2000       Equinox J2000
Constellation Cepheus
Right ascension 21h 09m 31.78348s [1]
Declination +68° 29′ 27.2311″ [1]
Apparent magnitude  (V)5.2 - 11.3 [2]
Characteristics
Evolutionary stage AGB [3]
Spectral type M6-9e [4]
U−B color index +0.33 [5]
B−V color index +1.49 [5]
Variable type Mira [3]
Astrometry
Radial velocity (Rv)−8.03 [6] km/s
Proper motion (μ)RA: −44.210 [1] mas/yr
Dec.: −44.921 [1] mas/yr
Parallax (π)5.4400±0.3476  mas [1]
Distance 600 ± 40  ly
(180 ± 10  pc)
Details
Mass 0.55 [7]   M☉
Radius 329+70
−50 [8]   R☉
Luminosity 5,700 [9]   L☉
Temperature 2,400 [9] - 3,347 [10]   K
Other designations
T Cephei, HR  8113, HD  202012, HIP  104451, BD+67°1291, GC  29611, SAO  19229, GSC  04460-02400
Database references
SIMBAD data
The visual band light curve of T Cephei, from AAVSO data TCepLightCurve.png
The visual band light curve of T Cephei, from AAVSO data

T Cephei is a Mira variable star in the constellation Cepheus. Located approximately 600 light-years (180 parsecs) distant, it varies between magnitudes 5.2 and 11.3 over a period of around 388 days. [9] [2] When it is near its maximum brightness, it is faintly visible to the naked eye under good observing conditions.

Contents

Vitold Ceraski announced his discovery that the star is a variable star, in 1879. [12] It appeared with its variable star designation, T Cephei, in Annie Jump Cannon's 1907 publication Second catalogue of variable stars. [13] T Cephei is a red giant of spectral type M6-9e with an effective temperature 2,400 K, a radius of 329 R☉, a mass of 0.55 M☉, and a luminosity of 5,700 L☉. If it were in the place of the Sun, its photosphere would at least engulf the orbit of Mars. This star is believed to be in a late stage of its life, the asymptotic giant branch phase, blowing off its own atmosphere to form a white dwarf in a distant future.

See also

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 VSX (4 January 2010). "T Cep". AAVSO Website. American Association of Variable Star Observers . Retrieved 1 July 2014.
  3. 1 2 Danilovich, T.; Ramstedt, S.; Gobrecht, D.; Decin, L.; De Beck, E.; Olofsson, H. (2018). "Sulphur-bearing molecules in AGB stars". Astronomy & Astrophysics. 617: A132. arXiv: 1807.05144 . doi:10.1051/0004-6361/201833317. S2CID   119225670.
  4. ↑ Keenan, Philip C.; Garrison, Robert F.; Deutsch, Armin J. (1974). "Revised Catalog of Spectra of Mira Variables of Types ME and Se". Astrophysical Journal Supplement. 28: 271. Bibcode:1974ApJS...28..271K. doi: 10.1086/190318 .
  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. ↑ Tuchman, Y. (1991). "The mode of pulsation in Mira variables determined by the observed acceleration data". The Astrophysical Journal. 383: 779. Bibcode:1991ApJ...383..779T. doi:10.1086/170836.
  8. ↑ Weigelt, Gerd; Beckmann, Udo; Berger, Jean-Philippe; Bloecker, Thomas; Brewer, Michael K.; Hofmann, Karl-Heinz; Lacasse, Marc G.; Malanushenko, Victor; Millan-Gabet, Rafael; et al. (2003). "JHK-band spectro-interferometry of T Cep with the IOTA interferometer". In Traub, Wesley A (ed.). Interferometry for Optical Astronomy II. Proc. SPIE. Vol. 4838. Society of Photo-optical Instrumentation Engineers (SPIE). pp. 181–184. Bibcode:2003SPIE.4838..181W. doi:10.1117/12.458659. ISBN   9780819446176. S2CID   123045204.
  9. 1 2 3 Danilovich, T.; Teyssier, D.; Justtanont, K.; Olofsson, H.; Cerrigone, L.; Bujarrabal, V.; Alcolea, J.; Cernicharo, J.; Castro-Carrizo, A.; García-Lario, P.; Marston, A. (2015). "New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme". Astronomy & Astrophysics. 581: A60. arXiv: 1506.09065 . Bibcode:2015A&A...581A..60D. doi:10.1051/0004-6361/201526705. S2CID   55109956.
  10. ↑ Guha Niyogi, Suklima; Speck, Angela K.; Onaka, Takashi (2011). "A Temporal Study of the Oxygen-rich Pulsating Variable Asymptotic Giant Branch Star, T Cep: Investigation on Dust Formation and Dust Properties". The Astrophysical Journal. 733 (2): 93. arXiv: 1103.5040 . Bibcode:2011ApJ...733...93G. doi:10.1088/0004-637X/733/2/93. S2CID   118332811.
  11. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  12. ↑ Ceraski, W. (February 1879). "Über einen neuen Veränderlichen". Astronomische Nachrichten. 94 (11): 175. Bibcode:1879AN.....94..175C. doi:10.1002/asna.18790941105.
  13. ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C.
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