S Antliae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Antlia |
| Right ascension | 09h 32m 18.386s[1] |
| Declination | −28° 37′ 39.97″[1] |
| Apparent magnitude (V) | 6.27 to 6.83[2] |
| Characteristics | |
| Spectral type | A9V |
| B−V color index | 0.33 |
| Variable type | Eclipsing binary W UMa type |
| Astrometry | |
| Parallax (π) | 13.30 ± 0.71[3] mas |
| Distance | 250 ± 10 ly (75 ± 4 pc) |
| Absolute magnitude (MV) | 1.963[3] |
| Details | |
| Mass | 1.82 M☉ |
| Radius | 2.23 R☉ |
| Luminosity | 17 L☉ |
| Temperature | 7900 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
S Antliae is a W Ursae Majoris-type eclipsing binary variable star in Antlia. It varies in apparent magnitude from 6.27 to 6.83 over a period of 15.6 hours.[2] The system shines with a combined spectrum of A9V. Based upon an annual parallax shift of 11.84 milliarc seconds as measured by the Hipparcos satellite,[1] this system is 270 light-years (84 parsecs) from Earth. Analysing and recalibrating yields a parallax of 13.30 and hence a distance of 250 light-years (76 parsecs).[3] The system is classed as an A-type W Ursae Majoris variable—the primary is hotter than the secondary and the drop in magnitude is caused by the latter passing in front of the former. Calculating the properties of the component stars from the orbital period indicates that the primary star has a mass 1.94 times and a diameter 2.026 times that of the Sun, and the secondary has a mass 0.76 times and a diameter 1.322 times that of the Sun.[4] The primary has a surface temperature of 7800 K, while the secondary is a little cooler at 7340 K. The two stars have similar luminosity and spectral type as they have a common envelope and share stellar material.[5] The system is thought to be around 5-6 billion years old. The two stars will eventually merge to form a single fast-spinning star.[4]
Its variability was first recorded in 1888 by H.M. Paul,[6] and at the time it had the shortest known period of any variable star. It was initially thought to be an Algol-type eclipsing binary, but this was discounted by E.C. Pickering on account of it lacking a shallow minimum in its maximum and the width of its minimum period. Alfred H. Joy noted the similarity of its light curve to W Ursae Majoris in 1926, concluding the system was indeed an eclipsing binary with two stars of spectral type A8.[7]
References
- 1 2 3 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752
. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.Vizier catalog entry - 1 2 Watson, Christopher (4 January 2010). "S Antliae". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 May 2014.
- 1 2 3 Eker, Z.; Bilir, S.; Yaz, E.; Demircan, O.; Helvaci, M. (2009). "New absolute magnitude calibrations for W Ursa Majoris type binaries". Astronomische Nachrichten. 330 (1): 68–77. arXiv:0807.4989. Bibcode:2009AN....330...68E. doi:10.1002/asna.200811041.
- 1 2 Gazeas, K.; Stȩpień, K. (2008). "Angular momentum and mass evolution of contact binaries". Monthly Notices of the Royal Astronomical Society. 390 (4): 1577–86. arXiv:0803.0212. Bibcode:2008MNRAS.390.1577G. doi:10.1111/j.1365-2966.2008.13844.x.
- ↑ Csizmadia, Sz.; Klagyivik, P. (2004). "On the properties of contact binary stars". Astronomy and Astrophysics. 426: 1001–05. arXiv:astro-ph/0408049. Bibcode:2004A&A...426.1001C. doi:10.1051/0004-6361:20040430.
- ↑ Paul, H. M. (1891). "Observations of 3407 S Antliae". Astronomical Journal. 10 (234): 139–142. Bibcode:1891AJ.....10..139P. doi:10.1086/101491.
- ↑ Joy, Alfred H. (1926). "Provisional elements and dimensions of S Antliae considered as an eclipsing binary". Astrophysical Journal. 64: 287–94. Bibcode:1926ApJ....64..287J. doi:10.1086/143015.