22 Vulpeculae

Last updated
22 Vulpeculae
QSVulLightCurve.png
A blue band light curve for QS Vulpeculae, adapted from Eaton and Shaw (2007) [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vulpecula
Right ascension 20h 15m 30.2386s [2]
Declination +23° 30 32.051 [2]
Apparent magnitude  (V)5.15 [3]
Characteristics
Spectral type G9Ib-II + B8V [4]
U−B color index +1.03 [5]
B−V color index +0.68 [5]
Variable type Algol [3]
Astrometry
Radial velocity (Rv)−22.8±0.9 [6]  km/s
Proper motion (μ)RA: 2.852±0.067 [2]   mas/yr
Dec.: −7.278±0.071 [2]   mas/yr
Parallax (π)2.1872 ± 0.0850  mas [2]
Distance 1,490 ± 60  ly
(460 ± 20  pc)
Absolute magnitude  (MV)−3.67 [7]
(−3.5 / −0.1) [8]
Orbit [4]
Period (P)249.18±0.010 d
Eccentricity (e)0.011
Inclination (i)81.34±0.02 [1] °
Argument of periastron (ω)
(secondary)
0 (assumed)°
Semi-amplitude (K1)
(primary)
27.10±0.21 km/s
Semi-amplitude (K2)
(secondary)
40.0±1.0 km/s
Details
22 Vul A
Mass 4.649 [4]   M
Radius 96 [4]   R
Luminosity 2,188 [1]   L
Temperature 4,699 [4]   K
Rotation 142 - 165 days [1]
Rotational velocity (v sin i)16 - 20 [1]  km/s
22 Vul B
Mass 3.150 [4]   M
Radius 3.4 [4]   R
Luminosity123 [1]   L
Temperature 11,995 [4]   K
Age 135.1 [4]   Myr
Other designations
QS Vul, BD+23 3944, HD  192713, HIP  99853, HR  7741, SAO  88416 [9]
Database references
SIMBAD data

22 Vulpeculae is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,490 light-years away, [2] and it has an apparent magnitude of about 5.2, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.

The pair have an orbital period of 249 d in an almost-circular orbit. The primary component is a G-type bright giant. It is over four times as massive as the Sun, and over 96 times as wide. Its companion is a B-type main-sequence star, 3.4 times as massive as the Sun. [8] Although the secondary has an effective temperature of nearly 12,000  K and the primary just 4,700 K, the large size of the cooler star means it is nearly 20 times as luminous at 2,200  L. The primary star is rotating slowly with a rotation period that appears to be between about 140 and 165 days, unexpectedly faster than the orbital period. Different parts of its atmosphere may be rotating at different speeds. [1] The hot secondary is rotating much faster, possibly at 350 km/s. [10]

The two stars have an orbit that is oriented in such a way that they periodically eclipse each other, each star alternately blocking the light of the other. For that, it has been given the variable star designation QS Vulpeculae; [9] 22 Vulpeculae is the Flamsteed designation. The maximum drop in visual apparent magnitude is 0.05 magnitudes when the hot secondary is completely hidden by the large cool primary. The eclipses are deeper at shorter wavelengths because a greater proportion of the short-wavelength radiation comes from the hot star. The primary eclipses last for eight days at visual wavelengths, but partial phases can be detected for up to 17 days at ultraviolet wavelengths due to the expanded atmosphere and wind of the primary star. Secondary eclipse, where the hot star transits the cooler one, are undetectable, and ellipsoidal variations due to distortion of the large primary produce brightness changes of less than 1.5%. [1]

Related Research Articles

<span class="mw-page-title-main">Alpha Vulpeculae</span> Star in the constellation Vulpecula

Alpha Vulpeculae, officially named Anser, is the brightest star in the constellation of Vulpecula. It is approximately 291 light-years from Earth. It forms a wide optical binary with 8 Vulpeculae.

<span class="mw-page-title-main">Psi Velorum</span> Binary star in the constellation Vela

Psi Velorum, Latinized from ψ Velorum, is a binary star system in the southern constellation of Vela. Based upon an annual parallax shift of 53.15 mas as seen from Earth, it is located 61.4 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +3.58. The motion of this system through space makes it a candidate member of the Castor stellar kinematic group.

<span class="mw-page-title-main">9 Aurigae</span> Multiple star system in the constellation Auriga

9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.

26 Aurigae is a binary star system in the northern constellation of Auriga. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.41.

<span class="mw-page-title-main">AR Aurigae</span> Binary star system in the constellation Auriga

AR Aurigae, also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 461 light-years from Earth.

<span class="mw-page-title-main">31 Vulpeculae</span> Star in the constellation Vulpecula

31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s.

<span class="mw-page-title-main">15 Vulpeculae</span> Star in the constellation Vulpecula

15 Vulpeculae is a variable star in the northern constellation of Vulpecula, located approximately 243 light years away based on parallax. It has the variable star designation NT Vulpeculae; 15 Vulpeculae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66. This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

<span class="mw-page-title-main">9 Vulpeculae</span> Star in the constellation Vulpecula

9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.

<span class="mw-page-title-main">HR 2554</span> Star in the constellation Carina

HR 2554, also known as V415 Carinae and A Carinae, is an eclipsing spectroscopic binary of the Algol type in the constellation of Carina whose apparent visual magnitude varies by 0.06 magnitude and is approximately 4.39 at maximum brightness. Its primary is a G-type bright giant star and its secondary is an A-type main-sequence star. It is approximately 553 light-years from Earth.

<span class="mw-page-title-main">LY Aurigae</span> Binary star in the constellation Auriga

LY Aurigae is a multiple star system in the constellation Auriga. It is an eclipsing binary variable star, dropping in brightness by 0.7 magnitudes every 4 days. The system is around a thousand light years away in the Auriga OB1 stellar association.

<span class="mw-page-title-main">1 Geminorum</span> Triple star system in the constellation Gemini

1 Geminorum is a star in the constellation Gemini. Its apparent magnitude is 4.15.

<span class="mw-page-title-main">Delta Sagittae</span> Binary star system in the constellation Sagitta

Delta Sagittae is a binary star in the constellation of Sagitta, with an apparent magnitude of +3.68. The primary component is a red M-type bright giant, and the secondary is a B-type main-sequence star. It is approximately 430 light years from Earth, based on its Gaia Data Release 2 parallax.

<span class="mw-page-title-main">1 Persei</span> Star in the constellation Perseus

1 Persei is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.

<span class="mw-page-title-main">31 Cygni</span> Triple star system in the constellation Cygnus

31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.

<span class="mw-page-title-main">25 Serpentis</span> Star in the constellation Serpens

25 Serpentis is a star system in the constellation of Serpens Caput. With an apparent magnitude of 5.37, it is just barely visible to the naked eye. The system is estimated to be some 450 light-years based on its parallax.

<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">U Vulpeculae</span> Variable star in the constellation Vulpecula

U Vulpeculae is a variable and binary star in the constellation Vulpecula.

Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

<span class="mw-page-title-main">WR 12</span> Star in the constellation Vela

WR 12 is a spectroscopic binary in the constellation Vela. It is an eclipsing binary consisting of a Wolf-Rayet star and a luminous companion of unknown spectral type. The primary is one of the most luminous stars known.

References

  1. 1 2 3 4 5 6 7 8 Eaton, Joel A.; Shaw, Felecia G. (June 2007). "Properties of the ζ Aur-Type Binary System 22 Vul = QS Vul". The Astronomical Journal. 133 (6): 2669–2678. Bibcode:2007AJ....133.2669E. doi: 10.1086/512186 . S2CID   120632154.
  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 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  4. 1 2 3 4 5 6 7 8 9 Eggleton, Peter P.; Yakut, Kadri (2017). "Models for 60 double-lined binaries containing giants". Monthly Notices of the Royal Astronomical Society. 468 (3): 3533. arXiv: 1611.05041 . Bibcode:2017MNRAS.468.3533E. doi: 10.1093/mnras/stx598 .
  5. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  6. Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  7. Gray, David F.; Pugh, Teznie (2012). "The Third Signature of Granulation in Bright-Giant and Supergiant Stars". The Astronomical Journal. 143 (4): 92. Bibcode:2012AJ....143...92G. doi: 10.1088/0004-6256/143/4/92 .
  8. 1 2 Schroeder, K.-P.; Griffin, R. E. M.; Hunsch, M. (1994). "Optical spectra of zeta Aurigae binary systems. 6: The chromosphere of 22 Vulpeculae". Astronomy and Astrophysics. 288 (1): 273–281. Bibcode:1994A&A...288..273S.
  9. 1 2 "* 22 Vul". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 13 May 2017.
  10. Griffin, R. E. M.; et al. (July 1993). "Optical spectra of zeta Aurigae binary systems. V. The 1988 eclipse of 22 Vulpeculae". Astronomy and Astrophysics. 274: 225. Bibcode:1993A&A...274..225G.