RV Tauri variable
RV Tauri variables are luminous variable stars that have distinctive light variations with alternating deep and shallow minima.
History and discovery
German astronomer Friedrich Wilhelm Argelander monitored the distinctive variations in brightness of R Scuti from 1840 to 1850. R Sagittae was noted to be variable in 1859, but it was not until the discovery of RV Tauri by Russian astronomer Lydia Ceraski in 1905 that the class of variable was recognised as distinct.
RV Tau variables exhibit changes in luminosity which are tied to radial pulsations of their surfaces. Their changes in brightness are also correlated with changes in their spectral type. While at their brightest, the stars have spectral types F or G. At their dimmest, their spectral types change to K or M. The difference between maximum and minimum brightness can be as much as four magnitudes.The period of brightness fluctuations from one deep minimum to the next is typically around 30 to 150 days, and exhibits alternating primary and secondary minima, which can change relative to each other. For comparison with other type II Cepheids such as W Virginis variables, this formal period is twice the fundamental pulsation period. Therefore although the approximate division between W Vir variables and RV Tau variables is at a fundamental pulsation period of 20 days, RV Tau variables are typically described with periods of 40-150 days.
RV Tauri stars are further subclassified into two types:
- RVa variables: these are RV Tauri variables which do not vary in mean brightness
- RVb variables: these are RV Tauri variables which show periodic variations in their mean brightness, so that their maxima and minima change on 600 to 1500 day timescales
The prototype of these variables, RV Tauri is a RVb type variable which exhibits brightness variations between magnitudes +9.8 and +13.3 with a formal period of 78.7 days. The brightest member of the class, R Scuti, is an RVa type, with an apparent magnitude varying from 4.6 to 8.9 and a formal period of 146.5 days. AC Herculis is an example of an RVa type variable.
The luminosity of RV Tau variables is typically a few thousand times the sun, which places them at the upper end of the W Virginis instability strip. Therefore RV Tau variables along with W Vir variables are sometimes considered a subclass of Type II Cepheids. They exhibit relationships between their periods, masses, and luminosity, although not with the precision of more conventional Cepheid variables. Although the spectra appear as supergiants, usually Ib, occasionally Ia although this may just need better measurements, the actual luminosities are only a few thousand times the sun which would make them bright giants.
The spectral classification of RV Tau stars is typically Ib: supergiant, although with peculiarities. However, these are not typical supergiants. These are post-AGB objects with low masses and they have lower luminosities than the bulk of the supergiants, so the spectral luminosity class is indicative of an evolved expanded star undergoing mass loss rather than an exceptionally luminous star. They have ceased fusion and are rapidly losing their atmospheres on their way to becoming a white dwarf, Although this should happen in a period measured in thousands of years, even hundreds for the more massive examples, the known RV Tau stars have not shown the secular increase in temperature that would be expected. The main sequence progenitor of this type of star has a mass near to that of the sun, although they have already lost about half of that during red giant and AGB phases. They are also thought to be mostly binaries surrounded by a dusty disc. Such stars are clearly metal-deficient Population II stars since it takes around 10 billion years for stars of that mass to evolve beyond the AGB.
|R Sct||4.9||6.9||140.2||750 ± 290||9400 ± 7100|
|U Mon||5.1||7.1||92.26||770 ± 280||3800 ± 2700|
|AC Her||6.4||8.7||75.4619||1130 ± 390||2400 ± 1600|
|RV Tau||8.8||12.3||76.698||2170 ± 720||3700 ± 2600|
|TW Cam||9.4||10.5||85.6||3100 ± 1100||3700 ± 2600|
|UY CMa||9.8||11.8||113.9||8400 ± 3100||4500 ± 3300|
|SU Gem||9.9||12.2||50.12||2110 ± 660||1200 ± 770|
TW Cam distance estimate may be too large.
R Sct may be less luminous than given in the table. It may be a thermal-pulsing AGB star, observed in a helium-burning phase instead of a post-AGB star.
- Gerasimovič, B.P. (1929). "Investigations of Semiregular Variables. VI. A General Study of RV Tauri Variables". Harvard College Observatory Circular 341: 1–15. Bibcode:1929HarCi.341....1G.
- De Ruyter, S.; Van Winckel, H.; Dominik, C.; Waters, L. B. F. M.; Dejonghe, H. (2005). "Strong dust processing in circumstellar discs around 6 RV Tauri stars". Astronomy and Astrophysics 435: 161. arXiv:astro-ph/0503290. Bibcode:2005A&A...435..161D. doi:10.1051/0004-6361:20041989.
- "GCVS Variability Types". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. 12 Feb 2009. Retrieved 2010-11-24.
- "List of the brighest RV Tauri stars". AAVSO. Retrieved 2010-11-20. (source article)
Samus N.N., Durlevich O.V., et al. Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)
- GCVS: List of RV variable stars
- AAVSO: Quick Look View of AAVSO Observations (get recent magnitude estimates)
- OGLE Atlas of Variable Star Light Curves - RV Tauri stars