Astronomy:V356 Sagittarii
 Light curves for V356 Sagittarii, in three photometric bands. Plotted from data published by Wilson and Woodward (1995).[1] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 47m 52.331s[2] |
| Declination | −20° 16′ 28.24″[2] |
| Apparent magnitude (V) | 6.84 Min I: 7.66 Min II: 7.24[3] |
| Characteristics | |
| Spectral type | B3V + A2II[4] |
| B−V color index | 0.120±0.029[5] |
| Variable type | Detached Algol(?)[3] |
| Astrometry | |
| Radial velocity (Rv) | 7.0±4.4[5] km/s |
| Proper motion (μ) | RA: +0.525[2] mas/yr Dec.: −4.847[2] mas/yr |
| Parallax (π) | 1.4783 ± 0.0289[2] mas |
| Distance | 2,210 ± 40 ly (680 ± 10 pc) |
| Orbit[6] | |
| Period (P) | 8.896106 d |
| Eccentricity (e) | 0.01566±0.01360 |
| Argument of periastron (ω) (secondary) | 288.71851±0.42683° |
| Semi-amplitude (K1) (primary) | 72.17896±1.25080 km/s |
| Semi-amplitude (K2) (secondary) | 190 km/s |
| Details | |
| Primary | |
| Mass | 11.0[7] M☉ |
| Radius | 9.07[7] R☉ |
| Surface gravity (log g) | 3.96±0.10[4] cgs |
| Temperature | 16,500±750[4] K |
| Rotational velocity (v sin i) | 350[4] km/s |
| Secondary | |
| Mass | 3.0[7] M☉ |
| Radius | 13.2[7] R☉ |
| Surface gravity (log g) | 2.82±0.10[4] cgs |
| Temperature | 8,600±300[4] K |
| Rotational velocity (v sin i) | 90[4] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
V356 Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated V356 Sgr. It has a peak apparent visual magnitude of 6.84, which decreases to 7.66 during the primary eclipse and 7.24 with the secondary eclipse.[3] Based on parallax measurements, this system is located at a distance of approximately 2,210 light years from the Sun.[2]
This is a double-lined spectroscopic binary system with an orbital period of 8.896 days.[6] It is a massive, interacting system with a circular orbit, where the secondary component has filled its Roche lobe and is transferring matter to its companion. The primary is a B-type main-sequence star with a stellar classification of B3V. It was originally the lower mass component,[9] but now has about 11 times the mass of the Sun.[7] The secondary is an evolved supergiant star[9] with a present-day class of A2II.[4] It has been stripped of much of its original mass,[9] leaving behind the exposed core of a star.[10] The transfer of matter is creating an accretion disk in orbit around the primary.[9]
At least some of the material stripped from the current secondary component has likely been lost from the system. A relatively small change in the orbital period has been observed, but the period is fairly stable over time, which may mean the mass transfer is intermittent.[9] Ultraviolet emission has been observed with the FUSE space observatory, indicating the presence of hot circumstellar matter. This emission shows little variation during a total eclipse, suggesting the material lies perpendicular to the accretion disk. This could represent a bipolar jet of matter from the primary.[11]
References
- ↑ Wilson, R. E.; Woodward, E. J. (February 1995). "U, B, V Light Curves of V356 Sagittarii". Publications of the Astronomical Society of the Pacific 107: 132–135. doi:10.1086/133528. Bibcode: 1995PASP..107..132W. https://articles.adsabs.harvard.edu/pdf/1995PASP..107..132W. Retrieved 31 March 2023.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Polidan, R. S. (June 1988), "A new study of the interacting binary star V356 Sgr", ESA, A Decade of UV Astronomy with the IUE Satellite 1: pp. 205–208, Bibcode: 1988ESASP.281a.205P.
- ↑ 5.0 5.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 6.0 6.1 Cabezas, M. et al. (February 2017), Miroshnichenko, Anatoly; Zharikov, Sergey; Korčáková, Daniela et al., eds., "New Spectroscopic Analysis and Light Curve Model of the Eclipsing Binary V356 Sgr", The B[e] Phenomenon: Forty Years of Studies. Proceedings of a Conference held at Charles University, Prague, Czech Republic 27 June - 1 July 2016, ASP Conference Series (San Francisco: Astronomical Society of the Pacific) 508: p. 364, Bibcode: 2017ASPC..508..367C.
- ↑ 7.0 7.1 7.2 7.3 7.4 van Rensbergen, W. et al. (April 2011), "Mass loss out of close binaries. The formation of Algol-type systems, completed with case B RLOF", Astronomy & Astrophysics 528, doi:10.1051/0004-6361/201015596, A16, Bibcode: 2011A&A...528A..16V.
- ↑ "V356 Sgr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V356+Sgr.
- ↑ 9.0 9.1 9.2 9.3 9.4 Lomax, Jamie R. et al. (January 2017), "The complex circumstellar and circumbinary environment of V356 Sgr", Monthly Notices of the Royal Astronomical Society 464 (2): 1936–1947, doi:10.1093/mnras/stw2457, Bibcode: 2017MNRAS.464.1936L.
- ↑ Dominis, D. et al. (April 2005), "In between β Lyrae and Algol: The Case Of V356 Sgr", Astrophysics and Space Science 296 (1–4): 189–192, doi:10.1007/s10509-005-4443-x, Bibcode: 2005Ap&SS.296..189D.
- ↑ Peters, G. J.; Polidan, R. S. (March 2004), "Eclipse mapping of the hot circumstellar plasma in Algol binaries", Astronomische Nachrichten 325 (3): 225–228, doi:10.1002/asna.200310224, Bibcode: 2004AN....325..225P.
Further reading
- Roby, S. W. et al. (September 1999), "Abundance determinations and a hot zone model for the interacting binary, V356 Sgr", Bulletin of the Astronomical Society 31 (4): 1239, 105.09, Bibcode: 1999BAAS...31.1239R.
- Tomkin, J.; Lambert, D. L. (1994), Shafter, Allen W., ed., "V356 Sagittarii – Mass Transfer for the Masses", Interacting binary stars : a symposium held in conjunction with the 105th Meeting of the Astronomical Society of the Pacific, San Diego State University, 13–15 July 1993 (San Francisco, Calif: Astronomical Society of the Pacific) 56: p. 397, Bibcode: 1994ASPC...56..397T.
- Tomkin, Jocelyn; Lambert, David L. (April 1994), "The Carbon Underabundance of the Secondary of V356 Sagittarii", Publications of the Astronomical Society of the Pacific 106: 365, doi:10.1086/133387, Bibcode: 1994PASP..106..365T.
- Daly, R. M. (1992), "A nonsynchronously rotating model for V356 Sagittarii", Bulletin of the Astronomical Society 24 (3): 1076, Bibcode: 1992BAAS...24.1076D.
- Polidan, R. S. (June 1989), "500–3200 Å observations of the interacting binary stars V356 Sgr and β Lyr", Space Science Reviews 50 (1–2): 85–94, doi:10.1007/BF00215921, Bibcode: 1989SSRv...50...85P.
- Polidan, R. S. (September 1987), "A New Study of the Interacting Binary Star V356 Sgr", Bulletin of the American Astronomical Society 19: 1085, Bibcode: 1987BAAS...19.1085P.
- Ziolkowski, J. (1985), "Evolutionary status of V356 Sgr", Acta Astronomica 35: 199–212, Bibcode: 1985AcA....35..199Z.
- Ziolkowski, J. (1981), "V356 Sgr revisited", Bulletin of the American Astronomical Society 13: 924, Bibcode: 1981BAAS...13..924Z.
- Hall, D. S. et al. (1981), "A recent time of minimum for V356 Sgr", Acta Astronomica 31: 383–386, Bibcode: 1981AcA....31..383H.
- Wilson, R. E.; Caldwell, C. N. (May 1978), "A model of V356 Sagittarii", Astrophysical Journal 221: 917–925, doi:10.1086/156095, Bibcode: 1978ApJ...221..917W.
- "The Eclipsing Binary V356 Sagittarii", Astrophysical Journal 121: 56, January 1955, doi:10.1086/145964, Bibcode: 1955ApJ...121...56P.
- Popper, Daniel M. (1953), "Two eclipsing binaries with giant components", Astronomical Journal 58: 224–225, doi:10.1086/106927, Bibcode: 1953AJ.....58R.224P.
- Popper, Daniel M. (October 1950), "Notes on the spectra of eclipsing binaries", Astronomical Journal 55: 78, doi:10.1086/106441, Bibcode: 1950AJ.....55R..78P.
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