HU Aquarii

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HU Aquarii
HUAqrLightCurve.png
The visual band light curve of HU Aquarii, adapted from Shengbang et al. (2016) [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Aquarius
Right ascension 21h 07m 58.19445s [2]
Declination −05° 17′ 40.5577″ [2]
Apparent magnitude  (V)+15.3
Characteristics
Spectral type DAm / M4.5V
Variable type AM Herculis
Astrometry
Proper motion (μ)RA: -64.579 [2]   mas/yr
Dec.: -62.732 [2]   mas/yr
Parallax (π)5.2354 ± 0.0457  mas [2]
Distance 623 ± 5  ly
(191 ± 2  pc)
Details
Mass 0.88/0.2  M☉
Radius 0.01/0.22  R☉
Luminosity 0.0022/0.0052  L☉
Temperature 12,500/3,400  K
Orbit
Period (P)2.08 hours [3]
Semi-major axis (a)0.0032 au
Eccentricity (e)0.0
Inclination (i)85°
Other designations
HU Aqr, RBS 1724, RE J210755-051621, 1RXS J210758.5-051744, 1AXG J210759-0518, 2RE J210755-051630, RE J2107-051, EUVE J2108-05.2, 2RE J2107-051, RX J2107.9-0518, AAVSO 2102-05, GSC 05200-00849, RE J2107-05, RX J2107.9-0517, 2MASS J21075818-0517404, Gaia DR2 6911950900211768704 [4]
Database references
SIMBAD data

HU Aquarii (abbreviated HU Aqr) is an eclipsing binary system approximately 620 light-years away from the Sun, [2] forming a cataclysmic variable of AM Herculis-type. The two stars orbit each other every 2.08 hours [3] and the ultra-short binary system includes an eclipsing white dwarf and red dwarf.

Contents

Eclipse timing variations

The HU Aquarii binary system exhibits variations in the timing of the eclipses. Schwarz et al. (2009) note that the variations are too large to be caused by the Applegate mechanism, and are within the expected range of magnetic braking but 30 times too large to be caused by gravitational radiation alone. As an alternative explanation, they suggested that the variations might be caused by an object in orbit around the binary, causing it to move back and forth along the line-of-sight to the system. [5] In March 2011, Qian et al. claimed the presence of two planets, [6] though the proposed orbits were subsequently shown to be unstable [7] and on orbits determined from a more thorough and precise analysis of the observational data. [8] Indeed, it seems likely that the signal that was interpreted as being the result of planetary companions might be instead the result of not well-studied interactions between the white dwarf and its red dwarf companion: as of 2014 all proposed orbital solutions have been refuted and it appears that the full set of timing measurements is inconsistent with any 1, 2 or 3-planet system due to poor fits to the data and unstable orbital configurations. [9] With new data gathered by 2018, the existence of planetary system remains elusive, as no model fitting all observations can be made. [10]

See also

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References

  1. ↑ Shengbang, Qian; Zhongtao, Han; Fernández Lajús, E; liying, Zhu; Wenping, Liao; Miloslav, Zejda; Linjia, Li; Voloshina, Irina; Liang, Liu; Jiajia, He (July 2016). "Interactions between planets and evolved stars". Journal of Physics: Conference Series. 728 (4): 042006. Bibcode:2016JPhCS.728d2006S. doi: 10.1088/1742-6596/728/4/042006 . S2CID   125620672.
  2. 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.
  3. 1 2 Howell; et al. (2002). "An Exploration of the Paradigm for the 2-3 Hour Period Gap in Cataclysmic Variables". The Astrophysical Journal . 550 (2): 897–918. arXiv: astro-ph/0005435 . Bibcode:2002MNRAS.336.1129B. doi: 10.1046/j.1365-8711.2002.05841.x . S2CID   609324.
  4. ↑ V* HU Aqr -- CV of AM Her type (polar)
  5. ↑ Schwarz; et al. (2009). "Hunting high and low: XMM monitoring of the eclipsing polar HU Aquarii". Astronomy and Astrophysics . 496 (3): 833–840. arXiv: 0901.4902 . Bibcode:2009A&A...496..833S. doi:10.1051/0004-6361/200811485. S2CID   14243402.
  6. ↑ Qian, S.-B.; Liu, L.; Liao, W.-P.; Li, L.-J.; Zhu, L.-Y.; Dai, Z.-B.; He, J.-J.; Zhao, E.-G.; Zhang, J.; Li, K. (2011). "Detection of a planetary system orbiting the eclipsing polar HU Aqr". Monthly Notices of the Royal Astronomical Society. 414 (1): L16–L20. arXiv: 1103.2005 . Bibcode:2011MNRAS.414L..16Q. doi:10.1111/j.1745-3933.2011.01045.x. S2CID   119165158.
  7. ↑ Horner, Jonathan; Marshall, J. P.; Wittenmyer, Robert A.; Tinney, C. G. (September 2011). "A dynamical analysis of the proposed HU Aquarii planetary system". Monthly Notices of the Royal Astronomical Society: Letters . 416 (1): L11–L15. arXiv: 1106.0777 . Bibcode:2011MNRAS.416L..11H. doi:10.1111/j.1745-3933.2011.01087.x. S2CID   59135141.
  8. ↑ Wittenmyer, Robert; Horner, J.; Marshall, J. P.; Butters, O. W.; Tinney, C. G. (February 2012). "Revisiting the proposed planetary system orbiting the eclipsing polar HU Aquarii". Monthly Notices of the Royal Astronomical Society. 419 (4): 3258–3267. arXiv: 1110.2542 . Bibcode:2012MNRAS.419.3258W. doi: 10.1111/j.1365-2966.2011.19966.x . S2CID   49524325.
  9. ↑ M. Bours; T. Marsh; E. Breedt; C. Copperwheat; V. Dhillon; A. Leckngam; S. Littlefair; S. Parsons; A. Prasit (2014). "Testing the planetary models of HU Aquarii". Monthly Notices of the Royal Astronomical Society. 445 (2): 1924–1931. arXiv: 1409.3586 . Bibcode:2014MNRAS.445.1924B. doi: 10.1093/mnras/stu1879 . S2CID   53630677.
  10. ↑ Schwope, A. D.; Thinius, B. D. (2018), "On the ephemeris of the eclipsing polar HU Aquarii. II: New eclipse epochs obtained 2014–2018", Astronomische Nachrichten, 339 (7–8): 540–544, arXiv: 1810.12886 , Bibcode:2018AN....339..540S, doi:10.1002/asna.201813526, S2CID   96446931
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