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]

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]

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<span class="mw-page-title-main">RR Lyncis</span> Variable star in the constellation Lynx

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<span class="mw-page-title-main">SW Lyncis</span> Variable star in the constellation of Lynx

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<span class="mw-page-title-main">VV Ursae Majoris</span> Variable star system in the constellation Ursa Major

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<span class="mw-page-title-main">RS Sagittarii</span> Eclipsing binary star system in the constellation Sagittarius

RS Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated RS Sgr. It is a double-lined spectroscopic binary with an orbital period of 2.416 days, indicating that the components are too close to each other to be individually resolved. The system has a combined apparent visual magnitude of 6.01, which is bright enough to be faintly visible to the naked eye. During the primary eclipse the brightness drops to magnitude 6.97, while the secondary eclipse is of magnitude 6.28. The distance to this system is approximately 1,420 light years based on parallax measurements.

<span class="mw-page-title-main">RY Persei</span> Star in the constellation Perseus

RY Persei is a variable star in the northern constellation of Perseus, abbreviated RY Per. It is an Algol variable with a period of 6.8635663 days, which indicates this is an eclipsing binary star system with an orbital plane oriented close to the line of sight from the Earth. The system has a maximum apparent visual magnitude of 8.50, which drops down to magnitude 10.25 during the eclipse of the primary component, then to 8.65 with the secondary eclipse. Based on parallax measurements, this system is located at a distance of approximately 2,960 light years from the Sun, but is drifting closer with a radial velocity of −12 km/s.

<span class="mw-page-title-main">RT Persei</span> Star system in the constellation Perseus

RT Persei is a variable star system in the northern constellation of Perseus, abbreviated RT Per. It is an eclipsing binary system with an orbital period of 0.84940032 d (20.386 h). At peak brightness the system has an apparent visual magnitude of 10.46, which is too faint to be viewed with the naked eye. During the eclipse of the primary this decreases to magnitude 11.74, then to magnitude 10.67 with the secondary eclipse. The distance to this system is approximately 628 light years based on parallax measurements. It is drifting closer with a heliocentric radial velocity of about −12 km/s.

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. 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 .
  10. ↑ 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.
  11. ↑ 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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