Astronomy:SY Muscae
 A visual band light curve for SY Muscae, plotted from ASAS and ASAS-SN data.[1][2] The inset plot shows the same data plotted with respect to the phase of the orbital period. | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Musca |
| Right ascension | 11h 32m 10.0002s[3] |
| Declination | −65° 25′ 11.473″[3] |
| Apparent magnitude (V) | 10.2 (- 11.2) - 12.7[4] |
| Characteristics | |
| Spectral type | M4.5[5] |
| Variable type | Z And[4] |
| Astrometry | |
| Radial velocity (Rv) | +13.708[5] km/s |
| Parallax (π) | 0.08 ± 0.90[3] mas |
| Distance | 1,500[5] pc |
| Orbit[5] | |
| Period (P) | 624.36 days |
| Eccentricity (e) | 0.0 |
| Inclination (i) | 84° |
| Semi-amplitude (K1) (primary) | 7.76 km/s |
| Details | |
| Giant | |
| Mass | 1.5[5] M☉ |
| Radius | 114[5] R☉ |
| Luminosity | 1,556[5] L☉ |
| Temperature | 3,400[5] K |
| Rotational velocity (v sin i) | 7[5] km/s |
| White dwarf | |
| Mass | 0.50[5] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
SY Muscae is a binary star system in the constellation Musca composed of a red giant and a white dwarf.[6] Its apparent magnitude varies from 10.2 to 12.7 over a period of 624.5 days.[7] Although the binary is a symbiotic star system, it is unusual in that it does not have an eruptive component.[6] It is an S-type symbiotic system, which means that the light comes from the stars rather than surrounding dust.[8]
With optical spectrometry, the red giant has been calculated as having a surface temperature of 3500 K and spectral type M4.5III, with around 1.3 times the Sun's mass, 86 times its radius and 1000 times its luminosity. The white dwarf is only 0.43 times the mass of the Sun. The two stars are 1.72 astronomical units (AU) apart, and take 624 days to orbit each other.[6] The red giant also pulsates with a period of 56 days.[8] The surface of the giant star extends to 40% of the distance to the Lagrange point L1, and hence does not fill its Roche Lobe and cause the white dwarf to gain an accretion disc. The system was calculated at being around 850 parsecs (2771 light-years) distant.[6]
References
- ↑ "ASAS All Star Catalogue". The All Sky Automated Survey. http://www.astrouw.edu.pl/asas/?page=aasc.
- ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup.
- ↑ 3.0 3.1 3.2 Gaia Collaboration; Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H. J; Mignard, F; Drimmel, R; Babusiaux, C et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics 595: A2. doi:10.1051/0004-6361/201629512. Bibcode: 2016A&A...595A...2G.
- ↑ 4.0 4.1 Samus, N. N. 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.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 5.9 Fekel, Francis C; Hinkle, Kenneth H; Joyce, Richard R; Wood, Peter R (2017). "Infrared Spectroscopy of Symbiotic Stars. XI. Orbits for Southern S-type Systems: Hen 3-461, SY Mus, Hen 3-828, AND AR Pav". The Astronomical Journal 153 (1): 35. doi:10.3847/1538-3881/153/1/35. Bibcode: 2017AJ....153...35F.
- ↑ 6.0 6.1 6.2 6.3 Schmutz, W.; Schild, H.; Muerset, U.; Schmid, H.M. (1994). "High resolution spectroscopy of symbiotic stars I. SY Muscae: orbital elements, M giant radius, distance". Astronomy and Astrophysics 288: 819–28. Bibcode: 1994A&A...288..819S. http://adsabs.harvard.edu/full/1994A%26A...288..819S.
- ↑ Otero, Sebastian Alberto (13 March 2013). "SY Muscae". AAVSO Website. American Association of Variable Star Observers. http://www.aavso.org/vsx/index.php?view=detail.top&oid=19701. Retrieved 9 March 2014.
- ↑ 8.0 8.1 Gromadzki, M.; Mikołajewska, J.; Soszyński, I. (2013). "Light Curves of Symbiotic Stars in Massive Photometric Surveys II. S and D'-Type Systems". Acta Astronomica 63 (4): 405–28. Bibcode: 2013AcA....63..405G.
 |  |
