Astronomy:QX Andromedae

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Short description: Eclipsing binary star system in the constellation Andromeda
QX Andromedae
NGC752-Tayson.jpg
Red circle.svg
Location of QX Andromedae (circled) in NGC 752
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas
Distance1,460 ± 40 ly
(450 ± 10 pc)
Orbit[6]
Period (P)0.4121716 days
Semi-major axis (a)2.89±0.04 M☉
Inclination (i)54.6±0.2°
Details[6]
Primary
Mass1.47±0.05 M☉
Radius1.46±0.02 R☉
Surface gravity (log g)4.27±0.03 cgs
Temperature6,440 K
Age1.34±0.06[7] Gyr
Secondary
Mass0.45±0.02 M☉
Radius0.88±0.02 R☉
Surface gravity (log g)4.20±0.03 cgs
Temperature6420±20 K
Age1.34±0.06[7] Gyr
Other designations
2MASS J01575777+3748224, RX J015758.0+374820, TYC 2816-1950-1
Database references
SIMBADdata

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]

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)[9]

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]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 "QX And database entry". Combined General Catalog of Variable Stars. CDS. http://webviz.u-strasbg.fr/viz-bin/VizieR-S?V*%20QX%20And. 
  3. ↑ 3.0 3.1 Norton, A. J.; Wheatley, P. J.; West, R. G.; Haswell, C. A.; Street, R. A.; Collier Cameron, A.; Christian, D. J.; Clarkson, W. I. et al. (2007). "New periodic variable stars coincident with ROSAT sources discovered using SuperWASP". Astronomy and Astrophysics 467 (2): 785. doi:10.1051/0004-6361:20077084. Bibcode: 2007A&A...467..785N. 
  4. ↑ 4.0 4.1 4.2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (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. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246. 
  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. doi:10.1111/j.1365-2966.2005.08609.x. Bibcode: 2005MNRAS.357..497B. 
  6. ↑ 6.0 6.1 6.2 6.3 Djurašević, G.; Yılmaz, M.; Baștürk, Ö.; Kılıçoğlu, T.; Latković, O.; Çalıșkan, Ş.; Christian, D. J.; Enoch, B. et al. (2011). "Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +079° 3142". Astronomy and Astrophysics 525: A66. doi:10.1051/0004-6361/201014895. Bibcode: 2011A&A...525A..66D. 
  7. ↑ 7.0 7.1 7.2 7.3 Agüeros, M. A.; Bowsher, E. C.; Bochanski, J. J.; Cargile, P. A.; Covey, K. R.; Douglas, S. T.; Kraus, A.; Kundert, A. et al. (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. doi:10.3847/1538-4357/aac6ed. Bibcode: 2018ApJ...862...33A. 
  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. Bibcode: 2011NewA...16..194R. https://www.sciencedirect.com/science/article/pii/S1384107610000990. Retrieved 11 October 2021. 



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