V356 Sagittarii

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V356 Sagittarii
V356SgrLightCurve.png
Light curves for V356 Sagittarii, in three photometric bands. Plotted from data published by Wilson and Woodward (1995). [1]
Observation data
Epoch J2000       Equinox J2000
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 mas/yr [2]
Dec.: −4.847 mas/yr [2]
Parallax (π)1.4783±0.0289  mas [2]
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
V356 Sgr, BD−20°5268, GC 25739, HD 173787, HIP 92235, SAO 187294, PPM 268914 [8]
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]

In 1929, the Japanese astronomer Kanda discovered that the star, then called BD-20°5268, is a variable star. It was given its variable star designation, V356 Sagittarii, in 1930. [9]

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, [10] but now has about 11 times the mass of the Sun. [7] The secondary is an evolved supergiant star [10] with a present-day class of A2II. [4] It has been stripped of much of its original mass, [10] leaving behind the exposed core of a star. [11] The transfer of matter is creating an accretion disk in orbit around the primary. [10]

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. [10] 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. [12]

References

  1. ↑ 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.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 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.
  4. 1 2 3 4 5 6 7 8 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.
  5. 1 2 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.
  6. 1 2 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[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, vol. 508, San Francisco: Astronomical Society of the Pacific, p. 364, Bibcode:2017ASPC..508..367C.
  7. 1 2 3 4 5 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.
  8. ↑ "V356 Sgr". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-03-29.
  9. ↑ Guthnick, P.; Prager, R. (November 1930). "Benennung von veränderlichen Sternen". Astronomische Nachrichten. 240 (15): 233–272. Bibcode:1930AN....240..233G. doi:10.1002/asna.19302401502 . Retrieved 20 October 2025.
  10. 1 2 3 4 5 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 .
  11. ↑ 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.
  12. ↑ 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.

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