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

Related Research Articles

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Mu Cephei, also known as Herschel's Garnet Star, Erakis, or HD 206936, is a red supergiant or hypergiant star in the constellation Cepheus. It appears garnet red and is located at the edge of the IC 1396 nebula. It is a 4th magnitude star easily visible to the naked eye under good observing conditions. Since 1943, the spectrum of this star has served as a spectral standard by which other stars are classified.

<span class="mw-page-title-main">VV Cephei</span> Binary star in the constellation Cepheus

VV Cephei, also known as HD 208816, is an eclipsing binary star system located in the constellation Cepheus. It is both a B[e] star and shell star. As a 5th magnitude star, it is visible to the naked eye under good observing conditions.

<span class="mw-page-title-main">R Horologii</span> Variable star in the constellation Horologium

R Horologii is a red giant star approximately 760 light-years away in the southern constellation of Horologium. It is a Mira variable with a period of 404.83 days, ranging from apparent magnitude 4.7 to 14.3—one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. The star is losing mass at the rate of 5.9×10−7 M☉·y−1.

<span class="mw-page-title-main">R Centauri</span> Variable star in the constellation Centaurus

R Centauri is a Mira variable star in the constellation Centaurus. When it is near its maximum brightness, it is faintly visible to the naked eye under very good observing conditions.

V354 Cephei is a red supergiant star located within the Milky Way. It is an irregular variable located over 13,000 light-years away from the Sun. It has an estimated radius of 1,139 solar radii. If it were placed in the center of the Solar System, it would extend to between the orbits of Mars and Jupiter.

<span class="mw-page-title-main">Zeta Cephei</span> Star in the constellation Cepheus

Zeta Cephei is a red supergiant star, located about 1000 light-years away in the constellation of Cepheus. Zeta Cephei marks the left shoulder of Cepheus, the King of Ethiopia. It is one of the fundamental stars of the MK spectral sequence, defined as type K1.5 Ib.

<span class="mw-page-title-main">W Cephei</span> Variable star in the constellation Cepheus

W Cephei is a spectroscopic binary and variable star located in the constellation Cepheus. It is thought to be a member of the Cep OB1 stellar association at about 8,000 light years. The supergiant primary star is one of the largest known stars and as well as one of the most luminous red supergiants.

<span class="mw-page-title-main">R Virginis</span> Star in the constellation Virgo

R Virginis is a Mira variable in the constellation Virgo. Located approximately 530 parsecs (1,700 ly) distant, it varies between magnitudes 6.1 and 12.1 over a period of approximately 146 days. Its variable nature was discovered by Karl Ludwig Harding in 1809.

<span class="mw-page-title-main">R Reticuli</span> Variable star in the constellation Reticulum

R Reticuli, also listed under the duplicate variable star designation S Reticuli, is a Mira variable star in the southern constellation Reticulum. It is an aging red giant star on the asymptotic giant branch with a stellar classification that varies between M4e to M7.5e, being hottest near maximum visual magnitude. The brightness of the star varies between apparent visual magnitudes 6.35 and 14.2 with an average period of 281.08±0.58 d. The mean maximum magnitude is 7.57 and the mean minimum magnitude 13.80.

<span class="mw-page-title-main">W Andromedae</span> Variable star in the constellation Andromeda

W Andromedae is a variable star in the constellation of Andromeda. It is classified as a Mira variable and S-type star, and varies from an apparent visual magnitude of 14.6 at minimum brightness to a magnitude of 6.7 at maximum brightness, with a period of approximately 397.3 days.

V Cephei is a white main sequence star in the constellation Cepheus. It only varies slightly by 0.03 of a magnitude. It was suspected of being variable by American astronomer Seth Carlo Chandler noting in 1890 that it varied by 0.7 magnitude but that it needed more confirmation. Subsequent observers were divided in whether they noted variability or not. A subsequent study with photoelectric photometry showed no variability.

<span class="mw-page-title-main">S Pegasi</span> Variable star in the constellation Pegasus

S Pegasi is a Mira variable star in the constellation Pegasus. It varies between magnitude 7 and 13 with a period of 319.22 days. It is believed to be pulsating in the first overtone. First overtone pulsators have masses less than 1.8 M☉ at a temperature of 2,107 K, and less than 1.4 M☉ at the luminosity of S Pegasi.

<span class="mw-page-title-main">9 Cephei</span> Star in the constellation Cepheus

9 Cephei, also known as V337 Cephei, is a variable star in the constellation Cepheus. It is visible to the naked eye.

<span class="mw-page-title-main">S Canis Minoris</span> Variable star in the constellation Canis Minor

S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of 6.5, so not normally visible to the naked eye. The star is located at a distance of approximately 1,340 light-years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of about +68 km/s.

<span class="mw-page-title-main">R Cancri</span> Variable star in the constellation Cancer

R Cancri is a Mira variable in the constellation Cancer. Located approximately 250 parsecs (830 ly) distant, it varies between magnitudes 6.07 and 12.3 over a period of approximately 357 days. At its brightest, it is very faintly visible to the naked eye.

<span class="mw-page-title-main">AC Herculis</span> Spectroscopic binary star in the constellation Hercules

AC Herculis, is an RV Tauri variable and spectroscopic binary star in the constellation of Hercules. It varies in brightness between apparent magnitudes 6.85 and 9.0.

<span class="mw-page-title-main">W Aquilae</span> Variable star in the constellation Aquila

W Aquilae is a variable star in the constellation of Aquila. It is a type of evolved star known as an S-type star. Due to its relatively close distance of 1,200 light-years and equatorial location, it is easy to observe and heavily studied.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">TU Andromedae</span> Star in the constellation Andromeda

TU Andromedae is a variable star of the Mira type in the constellation Andromeda. It has a spectral type of M5e and a visual magnitude which varies between extremes of 7.6 and 13.5.

<span class="mw-page-title-main">R Chamaeleontis</span> Variable star in the constellation Chamaeleon

R Chamaeleontis, also known as HD 71793, is a Mira variable located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude that ranges from 7.5 to 14.1, which is below the limit for naked eye visibility. Gaia DR3 parallax measurements place it about 3,000 light years away and it is currently approaching with a heliocentric radial velocity of 22 km/s.

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: 175. Bibcode:1879AN.....94..175C. doi:10.1002/asna.18790941105 . Retrieved 21 January 2025.
  13. ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C . Retrieved 21 January 2025.
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