S Antliae
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Antlia[2] |
| Right ascension | 09h 32m 18.38648s[3] |
| Declination | −28° 37′ 39.9685″[3] |
| Apparent magnitude (V) | 6.27 to 6.83[4] |
| Characteristics | |
| Spectral type | A9V |
| B−V color index | 0.33 |
| Variable type | Eclipsing binary W UMa type |
| Astrometry | |
| Proper motion (μ) | RA: −89.375 mas/yr[3] Dec.: +44.049 mas/yr[3] |
| Parallax (π) | 12.6116±0.0203 mas[3] |
| Distance | 258.6 ± 0.4 ly (79.3 ± 0.1 pc) |
| Absolute magnitude (MV) | 1.963[5] (2.25 + 3.42)[6] |
| Orbit[7] | |
| Period (P) | 0.59145447(30) days |
| Semi-major axis (a) | 3.82±0.02 R☉ |
| Inclination (i) | 74.02±0.14° |
| Semi-amplitude (K1) (primary) | 75±1 km/s |
| Semi-amplitude (K2) (secondary) | 234±1 km/s |
| Details[6] | |
| A | |
| Mass | 1.66±0.10 M☉ |
| Radius | 2.09±0.11 R☉ |
| Luminosity | 10.0±2.2 L☉ |
| Surface gravity (log g) | 4.02±0.03 cgs |
| Temperature | 7,100±200 K |
| B | |
| Mass | 0.55±0.05 M☉ |
| Radius | 1.31±0.06 R☉ |
| Luminosity | 3.4±0.7 L☉ |
| Temperature | 6,859±200 K |
| Age | 1.9[7] Gyr |
| Other designations | |
| CD-28°7373, HD 82610, SAO 177619, HIP 46810, HR 3798. | |
| Database references | |
| SIMBAD | data |
S Antliae is a W Ursae Majoris-type eclipsing binary star in Antlia.
Characteristics
S Antiliae is classed as an A-type W Ursae Majoris variable, since the primary is hotter than the secondary and the drop in magnitude is caused by the latter passing in front of the former. S Antiliae varies in apparent magnitude from 6.27 to 6.83 over a period of 15.6 hours.[4] The system shines with a combined spectrum of A9V.
The system's orbital period is about 0.591 days. The stars' centres are an average of 3.82 times the Sun's radius apart. The system will evolve into an Algol variable.[6]
Calculating the properties of the component stars indicates that the primary star has a mass 1.66 times and a diameter 2.09 times that of the Sun, and the secondary has a mass 0.55 times and a diameter 1.31 times that of the Sun. The primary has a surface temperature of 7,100 K, while the secondary is a little cooler at 6,859 K.[6] The two stars have similar luminosity and spectral type as they have a common envelope and share stellar material. The system is thought to be around two billion years old.[7]
Based upon an annual parallax shift of 12.6116 milliarc seconds as measured by the Gaia satellite,[3] this system is 259 light-years (79.3 parsecs) from Earth. Analysing and recalibrating yields a parallax of 13.30 and hence a distance of 250 light-years (76 parsecs).[5]
History
The star's variability was first recorded in 1888 by H.M. Paul,[8] when 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.[9]
References
- ^ Hogg, A. R.; Bowe, P. W. A. (August 1950). "Photoelectric Observations of S Antliae". Monthly Notices of the Royal Astronomical Society. 110 (4): 373–380. doi:10.1093/mnras/110.4.373.
- ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
- ^ a b c d e 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.
- ^ a b Watson, Christopher (4 January 2010). "S Antliae". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 May 2014.
- ^ a b 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. S2CID 15071352.
- ^ a b c d Bakis, Volkan; Budding, Edwin; Erdem, Ahmet; Love, Tom; Blackford, Mark G.; Zihao, Wu; Tang, Adam; Rhodes, Michael D.; Banks, Timothy S. (2024-09-25). "Comparative study of the W UMa type binaries S Ant and Epsilon CrA". Publications of the Astronomical Society of Australia. 41. arXiv:2409.17303. Bibcode:2024PASA...41...83B. doi:10.1017/pasa.2024.92.
- ^ a b c Latković, Olivera; Čeki, Atila; Lazarević, Sanja (2021). "Statistics of 700 Individually Studied W UMa Stars". The Astrophysical Journal Supplement Series. 254 (1): 10. arXiv:2103.06693. Bibcode:2021ApJS..254...10L. doi:10.3847/1538-4365/abeb23. S2CID 232185576.
- ^ 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.