RT Trianguli Australis

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RT Trianguli Australis
RTTrALightCurve.png
A light curve for RT Trianguli Australis, plotted from TESS data [1]
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Triangulum Australe
Right ascension 16h 34m 30.89188s [2]
Declination −63° 08′ 00.8395″ [2]
Apparent magnitude  (V)9.43 - 10.18 [3]
Characteristics
Spectral type F8:(R)-G2I-II [3]
Variable type BL Her [3]
Astrometry
Proper motion (μ)RA: -4.00 ± 1.48 [2]   mas/yr
Dec.: -14.25 ± 1.43 [2]   mas/yr
Parallax (π)1.26 ± 1.50  mas [2]
Details
Mass 0.48 [4]   M☉
Radius 9.4 [4]   R☉
Metallicity [Fe/H]+0.04 [5]   dex
Minimum
Luminosity 138 [6]   L☉
Temperature 5,200 [6]   K
Maximum
Luminosity200 [6]   L☉
Temperature 6,500 [6]   K
Other designations
RT  TrA, CPD−62° 5377, HIP  81157, 2MASS  J16343089-6308009, AAVSO  1625-62
Database references
SIMBAD data

RT Trianguli Australis, or RT TrA, is a BL Herculis variable (type II Cepheid) in the constellation of Triangulum Australe.

Contents

Variable

RT TrA varies between apparent magnitudes 9.4 and 10.2 over a period of 1.95 days. It was first discovered to be variable by Annie Jump Cannon in 1910 and initially classified as an RR Lyrae variable. Later authors segregated it and the similar V533 Centauri as RW Aurigae stars. [7] In time it became clear that RT TrA was unrelated to RW Aur, instead being a member of a group of stars on the instability strip somewhat above the horizontal branch. [8] These stars were then named as a group after BL Herculis, the brightest known member. [9] BL Her stars have periods shorter than eight days. [3] Like other BL Her variables, the light curve of RT TrA has a hump, in this case on the descending branch. The light curve is slightly asymmetric, with the minimum occurring at phase 0.6. [6]

Properties

RT TrA is a cool giant star with a radius of 9.4 R☉, although its spectral luminosity class verges on the supergiant level at times during its pulsations. As it pulsates, the effective temperature varies between 5,200 and 6,500 K and its luminosity between 138 and 200 L☉. Its physical properties place it on the instability strip of the H–R diagram.

Carbon star

RT TrA is unusual in that it is a carbon-rich cepheid variable. Unlike true carbon stars, it does not show an excess of s-process elements. It has very high surface abundances of carbon, nitrogen, iron, and some light metals, but not oxygen. The unusual abundances are believed to result from the convection of triple-alpha fusion products to the surface, and so it is expected that there will also be a high proportion of helium. Most other BL Her stars such as U TrA, do not show the same surface carbon excess. The elemental abundances are comparable to the cooler type-R stars. [5]

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References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  3. 1 2 3 4 Samus, 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. 1 2 Petersen, Jørgen Otzen (1980). "Bump Masses and Radii of Bl-Herculis Variables". Space Science Reviews. 27 (3–4): 495. Bibcode:1980SSRv...27..495P. doi:10.1007/BF00168341. S2CID   123182160.
  5. 1 2 Wallerstein, George; Matt, Sean; Gonzalez, Guillermo (2000). "The Carbon Cepheid RT Trianguli Australis: Additional Evidence of Triple-α and CNO Cycling". Monthly Notices of the Royal Astronomical Society. 311 (2): 414–22. Bibcode:2000MNRAS.311..414W. doi: 10.1046/j.1365-8711.2000.03064.x .
  6. 1 2 3 4 5 Bergeat, J.; Knapik, A.; Rutily, B. (2002). "Carbon-rich giants in the HR diagram and their luminosity function". Astronomy and Astrophysics. 390 (3): 967. Bibcode:2002A&A...390..967B. doi: 10.1051/0004-6361:20020525 .
  7. ↑ Hoffmeister, Cuno (1957). "On Two Abnormal Stars of Delta Cephei Type". Astrophysical Journal. 125: 824. Bibcode:1957ApJ...125..824H. doi: 10.1086/146358 .
  8. ↑ King, D. S.; Cox, A. N.; Hodson, S. W. (1981). "Linear and nonlinear studies of BL Herculis variables". Astrophysical Journal. 244: 242. Bibcode:1981ApJ...244..242K. doi:10.1086/158701.
  9. ↑ Smith, H. A.; Jacques, J.; Lugger, P. M.; Deming, D.; Butler, D. (1978). "Strömgren photometry of field BL Herculis stars. I. BL Herculis and XX Virginis". Publications of the Astronomical Society of the Pacific. 90: 422. Bibcode:1978PASP...90..422S. doi:10.1086/130351. S2CID   120328719.
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