Detection of a planetary system orbiting the eclipsing polar HU Aqr

  1. S.-B. Qian1,2,3,*,
  2. L. Liu1,2,3,
  3. W.-P. Liao1,2,
  4. L.-J. Li1,2,3,
  5. L.-Y. Zhu1,2,3,
  6. Z.-B. Dai1,2,
  7. J.-J. He1,2,
  8. E.-G. Zhao1,2,
  9. J. Zhang1,2,3,
  10. K. Li1,2,3

Article first published online: 1 APR 2011

DOI: 10.1111/j.1745-3933.2011.01045.x

Issue

Monthly Notices of the Royal Astronomical Society: Letters

Monthly Notices of the Royal Astronomical Society: Letters

Volume 414, Issue 1, pages L16–L20, June 2011

Additional Information

How to Cite

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. and Li, K. (2011), Detection of a planetary system orbiting the eclipsing polar HU Aqr. Monthly Notices of the Royal Astronomical Society: Letters, 414: L16–L20. doi: 10.1111/j.1745-3933.2011.01045.x

Author Information

  1. 1

    National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, 650011 Kunming, China

  2. 2

    Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, PO Box 110, 650011 Kunming, China

  3. 3

    Graduate University of the Chinese Academy of Sciences, Yuquan Road 19, Sijingshang Block, 100049 Beijing, China

* E-mail: qsb@ynao.ac.cn

Publication History

  1. Issue published online: 1 JUN 2011
  2. Article first published online: 1 APR 2011
  3. Accepted 2011 March 7. Received 2011 March 3; in original form 2011 January 11

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Keywords:

  • binaries: close;
  • binaries: eclipsing;
  • stars: individual: HU Aqr;
  • planetary systems;
  • white dwarfs

ABSTRACT

Using the precise times of mid-egress of the eclipsing polar HU Aqr, we discovered that this polar is orbited by two or more giant planets. The two planets detected so far have masses of at least 5.9 and 4.5MJup. Their respective distances from the polar are 3.6 and 5.4 au with periods of 6.54 and 11.96 yr, respectively. The observed rate of decrease of period derived from the downward parabolic change in the observed − calculated (O − C) curve is a factor of 15 larger than the value expected for gravitational radiation. This indicates that it may be only a part of a long-period cyclic variation, revealing the presence of one more planet. It is interesting to note that the two detected circumbinary planets follow the Titus–Bode law of solar planets with n= 5 and 6. We estimate that another 10 yr of observations will reveal the presence of the predicted third planet.

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