WW Geminorum: An early B-type eclipsing binary evolving into the contact phase

Yang, Y. -G.; Dai, H. -F.; Yin, X. -G.

doi:10.1088/0004-6256/148/5/90

Title: WW Geminorum: An early B-type eclipsing binary evolving into the contact phase

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Abstract

WW Gem is a B-type eclipsing binary with a period of 1.2378 days. The CCD photometry of this binary was performed in 2013 December using the 85 cm telescope at the Xinglong Stations of the National Astronomical Observatories of China. Using the updated W-D program, the photometric model was deduced from the VRI light curves. The results imply that WW Gem is a near-contact eclipsing binary whose primary component almost fills its Roche lobe. The photometric mass ratio is q {sub ph} = 0.48(± 0.05). All collected times of minimum light, including two new ones, were used for the period studies. The orbital period changes of WW Gem could be described by an upward parabola, possibly overlaid by a light-time orbit with a period of P {sub mod} = 7.41(± 0.04) yr and a semi-amplitude of A = 0.0079 days(± 0.0005 days), respectively. This kind of cyclic oscillation may be attributed to the light-travel time effect via the third body. The long-term period increases at a rate of dP/dt = +3.47(±0.04) × 10{sup –8} day yr{sup –1}, which may be explained by the conserved mass transfer from the less massive component to the more massive one. With mass transfer, themore »« less

Authors:

Yang, Y. -G.; Dai, H. -F.; Yin, X. -G. ^[1]

School of Physics and Electronic Information, Huaibei Normal University, 235000 Huaibei, Anhui Province (China)

Publication Date:: Sat Nov 01 00:00:00 EDT 2014

OSTI Identifier:: 22342226

Resource Type:: Journal Article

Journal Name:: Astronomical Journal (New York, N.Y. Online)

Additional Journal Information:: Journal Volume: 148; Journal Issue: 5; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 1538-3881

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; AMPLITUDES; BINARY STARS; CHARGE-COUPLED DEVICES; CHINA; ECLIPSE; MASS TRANSFER; ORBITS; OSCILLATIONS; PARABOLAS; PHOTOMETRY; ROCHE EQUIPOTENTIALS; STARS; TELESCOPES; VISIBLE RADIATION

Citation Formats


                    Yang, Y. -G., Dai, H. -F., Yin, X. -G., and Yang, Y., E-mail: yygcn@163.com, E-mail: yangyg@chnu.edu.cn, E-mail: yangy818@yeah.net. WW Geminorum: An early B-type eclipsing binary evolving into the contact phase.  United States: N. p., 2014. 
        Web.  doi:10.1088/0004-6256/148/5/90.

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                    Yang, Y. -G., Dai, H. -F., Yin, X. -G., & Yang, Y., E-mail: yygcn@163.com, E-mail: yangyg@chnu.edu.cn, E-mail: yangy818@yeah.net. WW Geminorum: An early B-type eclipsing binary evolving into the contact phase.  United States.  https://doi.org/10.1088/0004-6256/148/5/90

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                    Yang, Y. -G., Dai, H. -F., Yin, X. -G., and Yang, Y., E-mail: yygcn@163.com, E-mail: yangyg@chnu.edu.cn, E-mail: yangy818@yeah.net. 2014.  
        "WW Geminorum: An early B-type eclipsing binary evolving into the contact phase".  United States.  https://doi.org/10.1088/0004-6256/148/5/90.

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@article{osti_22342226,

  title        = {WW Geminorum: An early B-type eclipsing binary evolving into the contact phase},

  author       = {Yang, Y. -G. and Dai, H. -F. and Yin, X. -G. and Yang, Y., E-mail: yygcn@163.com, E-mail: yangyg@chnu.edu.cn, E-mail: yangy818@yeah.net},

  abstractNote = {WW Gem is a B-type eclipsing binary with a period of 1.2378 days. The CCD photometry of this binary was performed in 2013 December using the 85 cm telescope at the Xinglong Stations of the National Astronomical Observatories of China. Using the updated W-D program, the photometric model was deduced from the VRI light curves. The results imply that WW Gem is a near-contact eclipsing binary whose primary component almost fills its Roche lobe. The photometric mass ratio is q {sub ph} = 0.48(± 0.05). All collected times of minimum light, including two new ones, were used for the period studies. The orbital period changes of WW Gem could be described by an upward parabola, possibly overlaid by a light-time orbit with a period of P {sub mod} = 7.41(± 0.04) yr and a semi-amplitude of A = 0.0079 days(± 0.0005 days), respectively. This kind of cyclic oscillation may be attributed to the light-travel time effect via the third body. The long-term period increases at a rate of dP/dt = +3.47(±0.04) × 10{sup –8} day yr{sup –1}, which may be explained by the conserved mass transfer from the less massive component to the more massive one. With mass transfer, the massive binary WW Gem may be evolving into a contact binary.},

  doi          = {10.1088/0004-6256/148/5/90},

  url          = {https://www.osti.gov/biblio/22342226},
  journal      = {Astronomical Journal (New York, N.Y. Online)},

  issn         = {1538-3881},

  number       = 5,

  volume       = 148,

  place        = {United States},

  year         = {Sat Nov 01 00:00:00 EDT 2014},

  month        = {Sat Nov 01 00:00:00 EDT 2014}

}

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