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Eclipsing Binaries: Precise Clocks to Detect Extrasolar Planets

Published online by Cambridge University Press:  29 April 2014

Emil Kundra ,
Theodor Pribulla ,
Martin Vaňko  and
Ľubomír Hambálek
Emil Kundra
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences059 60 Tatranská Lomnica, Slovakia, email: kundra@ta3.sk
Theodor Pribulla
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences059 60 Tatranská Lomnica, Slovakia, email: kundra@ta3.sk
Martin Vaňko
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences059 60 Tatranská Lomnica, Slovakia, email: kundra@ta3.sk
Ľubomír Hambálek
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences059 60 Tatranská Lomnica, Slovakia, email: kundra@ta3.sk
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Abstract

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Project Dwarf is a new observing campaign focused on the detection of substellar companions to low-mass (composed of late-type, subdwarf (sd) or/and white dwarf (WD) components) detached eclipsing binaries using minima timing. The crucial condition for the object selection for this campaign is possibility to determine times of the minima with high precision. This is naturally fullfilled for eclipsing binaries with deep and narrow minima or systems hosting a WD component showing fast ingress or egress.

The observing project includes three groups of close eclipsing binaries indicating presence of substellar circum-binary components:

  1. (i) systems with K or/and M dwarf components

  2. (ii) systems with hot subdwarf (sd) and M dwarf components

  3. (iii) systems with white dwarf (WD) component(s).

The sample of the eclipsing systems have orbital periods in range of 0.1 to almost 3 days and their brightness fits possibilities of small telescopes equipped with a low-end CCD camera and at least VRI filter set. Such kind of telescopes allow us to develop observing network including also amateur astronomers.

Keywords

stars: planetary systemsbinaries: eclipsingtechniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 165 - 167
Copyright
Copyright © International Astronomical Union 2014 

References

Broucke, R. A. 2001, Celestial Mechanics and Dynamical Astronomy, 81, 321Google Scholar
Doyle, R. L., Carter, J. A., Fabrycky, D. C., et al. 2011, Science, 333, 1602CrossRefGoogle Scholar
Dvorak, R. 1984 (Celestial Mechanics), 34, 369Google Scholar
Konacki, M., Muterspaugh, M. W., Kulkami, S. R., & Helminiak, K. G. 2009, ApJ, 704, 513Google Scholar
Lee, J. W., Kim, S. L., Kim, Ch. H., et al. 2009, AJ, 137, 3181Google Scholar
Muterspaugh, M. W., Konacki, M., Lane, B. F., & Pfahl, E. 2007, in PLANETS IN BINARY STAR SYSTEMS, ed. Haghighipour, N. (Springer).Google Scholar
Pierens, A. & Nelson, R. P. 2008, A&A, 483, 633Google Scholar
Pribulla, T., Rucinksi, S. M., Blake, R. M., et al. 2009, AJ, 137, 3655CrossRefGoogle Scholar
Pribulla, T., et al. 2012, Astron. Nachr., 333, 754Google Scholar
Qian, S. B., Liu, L., Zhu, L. Y., et al. 2012, MNRAS, 422, 24CrossRefGoogle Scholar
Welsh, W. F., Orosz, S. A., Carter, J. A., et al. 2012, Nature, 481, 475CrossRefGoogle Scholar