V356 Sagittarii

Last updated
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]

Related Research Articles

<span class="mw-page-title-main">W Sagittarii</span> Star in the constellation Sagittarius

W Sagittarii is a multiple star system star in the constellation Sagittarius, and a Cepheid variable star.

<span class="mw-page-title-main">Upsilon Sagittarii</span> Binary star system in the constellation Sagittarius

Upsilon Sagittarii is a spectroscopic binary star system in the constellation Sagittarius. Upsilon Sagittarii is the prototypical hydrogen-deficient binary (HdB), and one of only four such systems known. The unusual spectrum of hydrogen-deficient binaries has made stellar classification of Upsilon Sagittarii difficult.

Nu<sup>1</sup> Sagittarii Triple star system in the constellation Sagittarius

Nu1 Sagittarii (ν1 Sagittarii, abbreviated Nu1 Sgr, ν1 Sgr) is a triple star system about 1,100 light-years from Earth. Its three components are designated Nu1 Sagittarii A (officially named Ainalrami, the traditional name for the system), B and C. A and B themselves form a spectroscopic binary. The system is 0.11 degree north of the ecliptic.

<span class="mw-page-title-main">V4641 Sagittarii</span> Binary star in the constellation Sagittarius

V4641 Sagittarii is a variable X-ray binary star system in the constellation Sagittarius. It is the source of one of the fastest superluminal jets in the Milky Way galaxy.

VX Sagittarii is an asymptotic giant branch star located more than 1.5 kiloparsec away from the Sun in the constellation of Sagittarius. It is a pulsating variable star with an unusually large magnitude range. It is one of the largest stars discovered, with a radius varying between 1,350 and 1,940 solar radii (940,000,000 and 1.35×109 km; 6.3 and 9.0 au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is brighter than the theoretical limit at –8.0.

<span class="mw-page-title-main">V3903 Sagittarii</span> Binary star system in the constellation Sagittarius

V3903 Sagittarii is an eclipsing binary star system in the constellation Sagittiarus. It creates an H II region LBN 29 1,070 parsecs away from the Sun.

<span class="mw-page-title-main">ZZ Boötis</span>

ZZ Boötis is a star system in the constellation Boötes. It varies from magnitude 6.79 to 7.44 over five days. Based on its parallax, measured by the Gaia spacecraft, it is about 350 light-years away.

<span class="mw-page-title-main">DN Orionis</span> Star in the constellation Orion

DN Orionis is an Algol variable located in the constellation of Orion. The primary star is a spectral type A0 star and the secondary is an evolved giant star of type G5III. The pair form a classical Algol-type system in which each star eclipses the other once per orbit, dropping the visual magnitude from 9.14 down to 9.62 at primary minimum and 9.25 at secondary minimum. Their orbital period is close to 13 days long.

<span class="mw-page-title-main">U Sagittae</span>

U Sagittae is an eclipsing binary star system in the northern constellation of Sagitta. It has been actively studied since its discovery in 1901. The maximum apparent visual magnitude of this system is 6.50, which is near the lower limit of visibility to the naked eye. The system is located at a distance of approximately 868 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −17 km/s. It is positioned about 2° from the middle of the Collinder 399 asterism, but lies much further away than the purported member stars.

<span class="mw-page-title-main">HS Hydrae</span> Triple star in the constellation of Hydra

HS Hydrae is a triple star system in the equatorial constellation of Hydra. The inner pair were an eclipsing binary during the period 1920 until 2019, with HS Hya being the variable star designation. With a base apparent visual magnitude of 8.08, HS Hya is too dim to be viewed with the naked eye. During the primary eclipse, the magnitude dropped to 8.61; the secondary eclipse lowered the magnitude to 8.55. Based on parallax measurements, the system is located at a distance of approximately 335 light years from the Sun. It is drifting closer with a mean radial velocity of −7 km/s.

<span class="mw-page-title-main">TX Ursae Majoris</span> Eclipsing binary star system in the constellation of Ursa Major

TX Ursae Majoris is an eclipsing binary star system in the northern circumpolar constellation of Ursa Major. With a combined apparent visual magnitude of 6.97, the system is too faint to be readily viewed with the naked eye. The pair orbit each other with a period of 3.063 days in a circular orbit, with their orbital plane aligned close to the line of sight from the Earth. During the primary eclipse, the net brightness decreases by 1.74 magnitudes, while the secondary eclipse results in a drop of just 0.07 magnitude. TX UMa is located at a distance of approximately 780 light years from the Sun based on parallax measurements, but is drifting closer with a mean radial velocity of −13 km/s.

KS Persei is a binary system in the equatorial constellation of Perseus. It is sometimes known as Bidelman's Star, named after William P. Bidelman. The star is invisible to the naked eye with a mean apparent visual magnitude of 7.70. As of 2018, the structure and evolutionary history of this system remain uncertain, although some form of mass transfer is likely to have occurred to explain the observed properties.

<span class="mw-page-title-main">BH Virginis</span> Eclipsing binary star in the constellation Virgo

BH Virginis is a binary star system in the equatorial constellation of Virgo. With a typical apparent visual magnitude of 9.6, it is too faint to be visible to the naked eye. Based on parallax measurements, it is located at a distance of approximately 488 light years from the Sun. The system is drifting closer with a net radial velocity of −23 km/s.

<span class="mw-page-title-main">RW Tauri</span> Eclipsing binary star in the constellation Taurus

RW Tauri is a binary star system in the equatorial constellation of Taurus. It has the designation HD 25487 in the Henry Draper Catalogue, while RW Tauri is the variable star designation. With a peak apparent visual magnitude of 8.05, it is too faint to be visible to the naked eye. The distance to this system is approximately 940 light years based on parallax measurements.

<span class="mw-page-title-main">UV Piscium</span> Binary star system in the Pisces constellation

UV Piscium is a binary star system in the constellation of Pisces. With a peak apparent visual magnitude of 8.98, it is too faint to be visible to the naked eye. This is an eclipsing binary system that decreases to magnitude 10.05 during the primary eclipse, then to magnitude 9.54 with the secondary eclipse. It is located at a distance of 232 light years from the Sun based on parallax measurements, and is receding with a radial velocity of 6.5 km/s. The position of this star near the ecliptic means it is subject to lunar occultation.

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

SW Lyncis is a binary or possibly a multiple-star system in the northern constellation of Lynx, abbreviated SW Lyn. With a combined apparent visual magnitude of 9.58, it is too faint to be visible to the naked eye. The system is located at a distance of approximately 970 light years based on parallax measurements, and is drifting further away with a net radial velocity of about +32 km/s.

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

VV Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated VV UMa. It is a variable star system with a brightness that cycles around an apparent visual magnitude of 10.19, making it too faint to be visible to the naked eye. The system is located at a distance of approximately 1,500 light years based on parallax measurements.

<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.

Further reading


This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.