 Light curves for V356 Sagittarii, in three photometric bands. Plotted from data published by Wilson and Woodward (1995). | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18 47 52.331 |
| Declination | −20° 16′ 28.24″ |
| Apparent magnitude (V) | 6.84 Min I: 7.66 Min II: 7.24 |
| Characteristics | |
| Spectral type | B3V + A2II |
| B−V color index | 0.120±0.029 |
| Variable type | Detached Algol(?) |
| Astrometry | |
| Radial velocity (Rv) | 7.0±4.4 km/s |
| Proper motion (μ) | RA: +0.525 mas/yr Dec.: −4.847 mas/yr |
| Parallax (π) | 1.4783 ± 0.0289 mas |
| Distance | 2,210 ± 40 ly (680 ± 10 pc) |
| Orbit | |
| 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 M☉ |
| Radius | 9.07 R☉ |
| Surface gravity (log g) | 3.96±0.10 cgs |
| Temperature | 16,500±750 K |
| Rotational velocity (v sin i) | 350 km/s |
| Secondary | |
| Mass | 3.0 M☉ |
| Radius | 13.2 R☉ |
| Surface gravity (log g) | 2.82±0.10 cgs |
| Temperature | 8,600±300 K |
| Rotational velocity (v sin i) | 90 km/s |
| Other designations | |
| V356 Sgr, BD−20°5268, GC 25739, HD 173787, HIP 92235, SAO 187294, PPM 268914 | |
| 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. Based on parallax measurements, this system is located at a distance of approximately 2,210 light years from the Sun.
This is a double-lined spectroscopic binary system with an orbital period of 8.896 days. 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, but now has about 11 times the mass of the Sun. The secondary is an evolved supergiant star with a present-day class of A2II. It has been stripped of much of its original mass, leaving behind the exposed core of a star. The transfer of matter is creating an accretion disk in orbit around the primary.
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. 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.
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. Bibcode:1995PASP..107..132W. doi:10.1086/133528. S2CID 121011912. Retrieved 31 March 2023.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ 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, vol. 1, pp. 205–208, Bibcode:1988ESASP.281a.205P.
- ^ 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, S2CID 119257644.
- ^ Cabezas, M.; et al. (February 2017), Miroshnichenko, Anatoly; et al. (eds.), "New Spectroscopic Analysis and Light Curve Model of the Eclipsing Binary V356 Sgr", The B Phenomenon: Forty Years of Studies. Proceedings of a Conference held at Charles University, Prague, Czech Republic 27 June - 1 July 2016, ASP Conference Series, vol. 508, San Francisco: Astronomical Society of the Pacific, p. 364, Bibcode:2017ASPC..508..367C.
- ^ 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, arXiv:1008.2620, Bibcode:2011A&A...528A..16V, doi:10.1051/0004-6361/201015596, S2CID 118417156, A16.
- "V356 Sgr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-03-29.
- ^ 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, arXiv:1609.07489, Bibcode:2017MNRAS.464.1936L, doi:10.1093/mnras/stw2457.
- 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, Bibcode:2005Ap&SS.296..189D, doi:10.1007/s10509-005-4443-x, S2CID 121917890.
- Peters, G. J.; Polidan, R. S. (March 2004), "Eclipse mapping of the hot circumstellar plasma in Algol binaries", Astronomische Nachrichten, 325 (3): 225–228, Bibcode:2004AN....325..225P, doi:10.1002/asna.200310224.
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, Bibcode:1999BAAS...31.1239R, 105.09.
- 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, vol. 56, San Francisco, Calif: Astronomical Society of the Pacific, 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, Bibcode:1994PASP..106..365T, doi:10.1086/133387, S2CID 121742430.
- Daly, R. M.; Linnell, A. P. (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, Bibcode:1989SSRv...50...85P, doi:10.1007/BF00215921, S2CID 125116416.
- 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, Bibcode:1978ApJ...221..917W, doi:10.1086/156095.
- Popper, Daniel M. (January 1955), "The Eclipsing Binary V356 Sagittarii", Astrophysical Journal, 121: 56, Bibcode:1955ApJ...121...56P, doi:10.1086/145964.
- Popper, Daniel M. (1953), "Two eclipsing binaries with giant components", Astronomical Journal, 58: 224–225, Bibcode:1953AJ.....58R.224P, doi:10.1086/106927.
- Popper, Daniel M. (October 1950), "Notes on the spectra of eclipsing binaries", Astronomical Journal, 55: 78, Bibcode:1950AJ.....55R..78P, doi:10.1086/106441.
