QX Andromedae

Last updated
QX Andromedae
NGC752-Tayson.jpg
Red circle.svg
Location of QX Andromedae (circled) in NGC 752
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 01h 57m 57.7818s [1]
Declination +37° 48′ 22.4500″ [1]
Apparent magnitude  (V)11.28 – 11.5 variable [2]
Characteristics
Spectral type F6 [2]
Apparent magnitude  (B)11.77 [3]
Apparent magnitude  (R)11.23 [3]
Apparent magnitude  (G)11.2929 [1]
Apparent magnitude  (J)10.393 [4]
Apparent magnitude  (H)10.225 [4]
Apparent magnitude  (K)10.163 [4]
Variable type W UMa [2]
Astrometry
Radial velocity (Rv)11.70±0.27 [5]  km/s
Proper motion (μ)RA: 10.016±1.295 [1]   mas/yr
Dec.: −11.926±0.281 [1]   mas/yr
Parallax (π)2.2376 ± 0.0676  mas [1]
Distance 1,460 ± 40  ly
(450 ± 10  pc)
Orbit [6]
Period (P)0.4121716 days
Semi-major axis (a)2.89±0.04M☉
Inclination (i)54.6±0.2°
Details [6]
Primary
Mass 1.47±0.05  M☉
Radius 1.46±0.02  R☉
Surface gravity (log g)4.27±0.03  cgs
Temperature 6,440  K
Age 1.34±0.06 [7]   Gyr
Secondary
Mass 0.45±0.02  M☉
Radius 0.88±0.02  R☉
Surface gravity (log g)4.20±0.03  cgs
Temperature 6420±20  K
Age 1.34±0.06 [7]   Gyr
Other designations
2MASS J01575777+3748224, RX J015758.0+374820, TYC 2816-1950-1
Database references
SIMBAD data

QX Andromedae (often abbreviated to QX And) is an eclipsing binary in the constellation Andromeda. It varies from a maximum apparent visual magnitude of 11.28 to a minimum of 11.50. Since it is impossible to specify the onset time of the eclipses, it is classified as a W Ursae Majoris variable star. [2] It is also observed as an X-ray source [8] and is a member of the open cluster NGC 752. [7]

Contents

System

As a whole, the QX Andromedae system emits light like a stellar blackbody, with a F6 spectral type. [2] The two stars in the system complete an orbit every 9.892 hours; they are so close that their envelopes are touching each other. Their temperature is similar, but they have different radius and mass. [6] Since they belong to an open cluster, the age of this system is equal to the cluster estimated age (1.34±0.06 billion years). [7]

Variability

A visual band light curve of QX Andromedae, adapted from Ren et al. (2011) QXAndLightCurve.png
A visual band light curve of QX Andromedae, adapted from Ren et al. (2011)

The light curve of QX Andromedae shows almost equal eclipses; the primary eclipse occurs when the less massive star pass in front of the other one. The brightness variations are rather small for this system given the low orbital inclination of 55°. [6]

Related Research Articles

<span class="mw-page-title-main">Zeta Andromedae</span> Star system in the constellation Andromeda

Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.

56 Andromedae, abbreviated 56 And, is a probable binary star system in the northern constellation of Andromeda. 56 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 5.69, which is just bright enough to be dimly visible to the naked eye under good seeing conditions. The distance to this system can be ascertained from its annual parallax shift, measured at 9.9 mas with the Gaia space observatory, which yields a separation of 330 light years. It is moving further from the Earth with a heliocentric radial velocity of +62 km/s and is traversing the celestial sphere at a relatively high rate of 0.183″ per year. This pair is positioned near the line of sight to the open cluster NGC 752, located 1,490 light-years away.

<span class="mw-page-title-main">Phi Cassiopeiae</span> Star in the constellation Cassiopeia

Phi Cassiopeiae is a star in the constellation Cassiopeia. φ Cassiopeiae is a multiple star with a combined apparent magnitude of +4.95. The two brightest components are A and C, sometimes called φ1 and φ2 Cas. φ Cas A is an F0 bright supergiant of magnitude 4.95 and φ Cas C is a 7.08 magnitude B6 supergiant at 134".

<span class="mw-page-title-main">Kappa Crucis (star)</span> Star in the constellation Crux

Kappa Crucis is a spectroscopic binary star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">V385 Andromedae</span> Star in the constellation Andromeda

V385 Andromedae is a variable star in the constellation Andromeda, about 360 parsecs (1,200 ly) away. It is a red giant over a hundred times larger than the sun. It has an apparent magnitude around 6.4, just about visible to the naked eye in ideal conditions.

WASP-5 is a magnitude 12 yellow dwarf star located about 910 light-years away in the Phoenix constellation. The star is likely older than Sun, slightly enriched in heavy elements and is rotating rapidly, being spun up by the tides raised by the giant planet on the close orbit.

<span class="mw-page-title-main">KQ Puppis</span> Binary star in the constellation Puppis

KQ Puppis is a spectroscopic binary variable star in the constellation Puppis. A red supergiant star and a hot main sequence star orbit each other every 9,742 days. Its apparent magnitude varies between 4.82 and 5.17.

EQ Pegasi is a nearby binary system of two red dwarfs. Both components are flare stars, with spectral types of M4Ve and M6Ve respectively, and a current separation between the components of 5.8 arcseconds. The system is at a distance of 20.4 light-years, and is 950 million years old. The primary star is orbited by one known exoplanet.

<span class="mw-page-title-main">V520 Persei</span> Star in the constellation Perseus

V520 Persei is a blue supergiant member of NGC 869, one of the Perseus Double Cluster open clusters. It is an irregular variable star.

<span class="mw-page-title-main">BU Crucis</span> Star in the constellation Crux

BU Crucis is a variable star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">65 Ursae Majoris</span> Star system in the constellation Ursa Major

65 Ursae Majoris, abbreviated as 65 UMa, is a star system in the constellation of Ursa Major. With a combined apparent magnitude of about 6.5, it is at the limit of human eyesight and is just barely visible to the naked eye in ideal conditions. It is about 760 light years away from Earth.

<span class="mw-page-title-main">NGC 2539</span> Open cluster in the constellation Puppis

NGC 2539 is an open cluster in the constellation Puppis, located at the north edge of the constellation. It was discovered by William Herschel on January 31, 1785. It is a moderately rich cluster and with little central concentration, with Trumpler class II1m.

<span class="mw-page-title-main">AD Andromedae</span> Eclipsing binary star in the constellation Andromeda

AD Andromedae is an eclipsing binary in the constellation Andromeda. Its maximum apparent visual magnitude is 11.2, but it shows a decrease of 0.62 magnitudes during the main eclipse and 0.58 during the secondary one. It is classified as a Beta Lyrae variable star with a period of almost one day.

<span class="mw-page-title-main">DS Andromedae</span> Eclipsing binary star in the constellation Andromeda

DS Andromedae is an eclipsing binary star in the constellation Andromeda and a member of the open cluster NGC 752. Its maximum apparent visual magnitude is 10.44, but drops down to 10.93 during the main eclipse and to 10.71 during the secondary one.

<span class="mw-page-title-main">PX Andromedae</span> Star in the constellation Andromeda

PX Andromedae is an eclipsing cataclysmic variable star in the constellation Andromeda. It has been classified as a SW Sextantis variable, and its apparent visual magnitude varies between 14.04 and 17.

<span class="mw-page-title-main">QR Andromedae</span> Eclipsing binary star in the constellation Andromeda

QR Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 12.16, but its light curve shows clearly eclipsing events where its brightness can drop to a magnitude of 13.07. This leads to its classification as an Algol variable star.

<span class="mw-page-title-main">WASP-21</span> Star in the constellation Pegasus

WASP-21 is a G-type star that is reaching the end of its main sequence lifetime approximately 850 light years from Earth in the constellation of Pegasus. The star is relatively metal-poor, having 40% of heavy elements compared to the Sun. Kinematically, WASP-21 belongs to the thick disk of the Milky Way. It has an exoplanet named WASP-21b.

BD-07 436, also known as WASP-77 since 2012, is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares.

WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8 billion years. The star does exhibit starspot activity as is typical for its spectral class.

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 N. N. Samus; O. V. Durlevich; et al. "QX And database entry". Combined General Catalog of Variable Stars (2017 ed.). CDS . Retrieved 2018-11-12.
  3. 1 2 Norton, A. J.; Wheatley, P. J.; West, R. G.; Haswell, C. A.; Street, R. A.; Collier Cameron, A.; Christian, D. J.; Clarkson, W. I.; Enoch, B.; Gallaway, M.; Hellier, C.; Horne, K.; Irwin, J.; Kane, S. R.; Lister, T. A.; Nicholas, J. P.; Parley, N.; Pollacco, D.; Ryans, R.; Skillen, I.; Wilson, D. M. (2007). "New periodic variable stars coincident with ROSAT sources discovered using SuperWASP". Astronomy and Astrophysics. 467 (2): 785. arXiv: astro-ph/0702631 . Bibcode:2007A&A...467..785N. doi:10.1051/0004-6361:20077084. S2CID   16358048.
  4. 1 2 3 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  5. ↑ Bilir, S.; Karataș, Y.; Demircan, O.; Eker, Z. (2005). "Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation". Monthly Notices of the Royal Astronomical Society. 357 (2): 497–517. arXiv: astro-ph/0411291 . Bibcode:2005MNRAS.357..497B. doi: 10.1111/j.1365-2966.2005.08609.x .
  6. 1 2 3 4 Djurašević, G.; Yılmaz, M.; Baștürk, Ö.; Kılıçoğlu, T.; Latković, O.; Çalıșkan, Ş.; Christian, D. J.; Enoch, B.; Gallaway, M.; Hellier, C.; Horne, K.; Irwin, J.; Kane, S. R.; Lister, T. A.; Nicholas, J. P.; Parley, N.; Pollacco, D.; Ryans, R.; Skillen, I.; Wilson, D. M. (2011). "Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +079° 3142". Astronomy and Astrophysics. 525: A66. arXiv: 1011.3677 . Bibcode:2011A&A...525A..66D. doi:10.1051/0004-6361/201014895. S2CID   119289612.
  7. 1 2 3 4 Agüeros, M. A.; Bowsher, E. C.; Bochanski, J. J.; Cargile, P. A.; Covey, K. R.; Douglas, S. T.; Kraus, A.; Kundert, A.; Law, N. M.; Ahmadi, A.; Arce, H. G. (July 2018). "A New Look at an Old Cluster: The Membership, Rotation, and Magnetic Activity of Low-mass Stars in the 1.3 Gyr Old Open Cluster NGC 752". The Astrophysical Journal. 862 (1): 33. arXiv: 1804.02016 . Bibcode:2018ApJ...862...33A. doi:10.3847/1538-4357/aac6ed. S2CID   119438236.
  8. ↑ Belloni, T.; Verbunt, F. (January 1996). "Soft X-rays from the intermediate-age open cluster NGC 752". Astronomy and Astrophysics. 305: 806. Bibcode:1996A&A...305..806B.
  9. ↑ Ren, A. B.; Zhang, X. B.; Luo, C. Q.; Luo, Y. P.; Deng, L. C.; Luo, Z. Q. (April 2011). "CCD Photometry of the W UMa type star QX Andromeda". New Astronomy. 16 (3): 194–198. doi:10.1016/j.newast.2010.08.007 . Retrieved 11 October 2021.
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.