RV Tauri

RV Tauri
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Taurus
Right ascension 04h 47m 6.7281s[1]
Declination 26° 10′ 45.613″[1]
Apparent magnitude (V) 9.0–10.6[2]
Characteristics
Spectral type G2eIa-M2Ia[3]
U−B color index 0.9-1.8[2]
B−V color index 1.5-1.9[2]
Variable type RVb[4]
Astrometry
Radial velocity (Rv)32[5] km/s
Proper motion (μ) RA: -2.20[1] mas/yr
Dec.: -5.00[1] mas/yr
Parallax (π)1.21 ± 0.36[6] mas
Distance2,170[4] pc
Absolute magnitude (MV)-3.65[7]
Details
Mass0.6[8] M☉
Luminosity3,700[4] L☉
Surface gravity (log g)0.0[4] cgs
Temperature4,500[4] (4,225-5,080[2]) K
Metallicity-0.4[4]
Other designations
RV Tauri, RV Tau, 2MASS J04470673+2610455, GSC 01835-01075, BD+25°732, HD 283868, TYC 1835-1075-1, GCRV 2803, AAVSO 0441+26, IRAS 04440+2605
Database references
SIMBADdata

RV Tauri (RV Tau) is a star in the constellation Taurus. It is a yellow supergiant and is the prototype of a class of pulsating variables known as RV Tauri variables.

Variability

RV Tau was discovered to be variable in 1905 by Lydia Ceraski,[9] and by 1907 it was clear that it had minima of alternating brightness.[10] Over a period of 78.5 days it shows two maxima at around magnitude 9.5, a minimum around magnitude 10.0, and another minimum about 0.5 magnitudes fainter.[11] This change in brightness is caused by pulsations: the temperature and radius vary, causing some variation in luminosity but mostly a shift of the emitted radiation from visual to infrared. The spectral type varies in line with the temperature, being classified as G2 at its brightest and M2 at its dimmest. In addition to the fundamental period given, RV Tauri also exhibits small variations in its mean brightness over a period of 1,216 days. The maxima and minima in each period vary by several tenths of a magnitude with no obvious regularity.[11]

Visibility

RV Tau is well placed for northern hemisphere observers during the winter months, and observations can be made from August to April. However it is faint, located in a nondescript patch of sky between The Pleiades and Beta Aurigae.[11]

Properties

The distance to RV Tau has been calculated by various methods, including modelling the atmosphere. RV Tauri stars have been shown to follow a period-luminosity relationship, and this can be used to confirm the luminosity and distance.[12] They have low masses, but are extended cool stars of high luminosity undergoing strong mass loss. RV Tau has a luminosity of 3,700 L☉ but the spectral luminosity class of a bright supergiant, indicating the rarified nature of its atmosphere.

Surface abundances show enhancement of heavy elements, thought to have been dredged up during an earlier AGB phase. Carbon in particular is strongly in excess in RV Tau.[8]

RV Tau is surrounded by a dusty circumstellar disc, a common feature of RV Tauri variables. It has been suggested that the formation of the disk is related to a binary companion, but none has been detected.[4]

Evolution

RV Tau is likely a post-Asymptotic Giant Branch (AGB) star, an originally sun-like star which is in the end stages of its life just prior to the expulsion of a planetary nebula and contraction to a white dwarf. RV Tau gives an insight into the lives and deaths of stars like the Sun. Evolution models show it takes about 10 billion years for a 1 solar mass (1 M☉) star to reach the Asymptotic Giant Branch.[13]

References

  1. 1 2 3 4 Hog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. V.; Roeser, S. (1998). "The TYCHO Reference Catalogue". Astronomy and Astrophysics. 335: L65. Bibcode:1998A&A...335L..65H.
  2. 1 2 3 4 Dawson, D. W. (1979). "A photometric investigation of RV Tauri and yellow semiregular variables". Astrophysical Journal Supplement Series. 41: 97. Bibcode:1979ApJS...41...97D. doi:10.1086/190610.
  3. ↑ Taranova, O. G.; Shenavrin, V. I.; Tatarnikov, A. M. (2009). "Infrared photometry for two RV Tau stars and V1027 Cyg". Astronomy Letters. 35 (7): 472. Bibcode:2009AstL...35..472T. doi:10.1134/S1063773709070044.
  4. 1 2 3 4 5 6 7 Ruyter, S; Winckel; Dominik; Waters; Dejonghe (2005). "Strong dust processing in circumstellar discs around 6 RV Tauri stars. Are dusty RV Tauri stars all binaries?". Astronomy and Astrophysics. 435 (1): 161–166. arXiv:astro-ph/0503290v1Freely accessible. Bibcode:2005A&A...435..161D. doi:10.1051/0004-6361:20041989.
  5. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington: 0. Bibcode:1953GCRV..C......0W.
  6. ↑ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally published in: Astron. Astrophys. 1337. Bibcode:2016yCat.1337....0G.
  7. ↑ Wahlgren, Glenn M. (1992). "The metallicity and luminosity of RV Tauri variables from medium-resolution spectra". Astronomical Journal. 104: 1174. Bibcode:1992AJ....104.1174W. doi:10.1086/116306.
  8. 1 2 Stasińska, G.; Szczerba, R.; Schmidt, M.; Siódmiak, N. (2006). "Post-AGB stars as testbeds of nucleosynthesis in AGB stars". Astronomy and Astrophysics. 450 (2): 701. arXiv:astro-ph/0601504Freely accessible. Bibcode:2006A&A...450..701S. doi:10.1051/0004-6361:20053553.
  9. ↑ Ceraski, W. (1905). "Trois nouvelles variables". Astronomische Nachrichten. 168 (2): 29. Bibcode:1905AN....168...29C. doi:10.1002/asna.19051680207.
  10. ↑ Seares, Frederick Hanley; Haynes, Eli Stuart (1908). "The Variable RV Tauri (45.1905)". Laws Observatory Bulletin. 14: 215. Bibcode:1908LawOB..14..215S.
  11. 1 2 3 Isles, J. E. (1975). "Variable Star Section". Journal of the British Astronomical Society. 85: 156. Bibcode:1975JBAA...85..156I.
  12. ↑ Alcock, C.; Allsman, R. A.; Alves, D. R.; Axelrod, T. S.; Becker, A.; Bennett, D. P.; Cook, K. H.; Freeman, K. C.; Griest, K.; Lawson, W. A.; Lehner, M. J.; Marshall, S. L.; Minniti, D.; Peterson, B. A.; Pollard, Karen R.; Pratt, M. R.; Quinn, P. J.; Rodgers, A. W.; Sutherland, W.; Tomaney, A.; Welch, D. L. (1998). "The MACHO Project LMC Variable Star Inventory. VII. The Discovery of RV Tauri Stars and New Type II Cepheids in the Large Magellanic Cloud". The Astronomical Journal. 115 (5): 1921. arXiv:astro-ph/9708039Freely accessible. Bibcode:1998AJ....115.1921A. doi:10.1086/300317.
  13. ↑ Bloecker, T. (1995). "Stellar evolution of low- and intermediate-mass stars. II. Post-AGB evolution". Astronomy and Astrophysics. 299: 755. Bibcode:1995A&A...299..755B.
This article is issued from Wikipedia - version of the 10/2/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.