The Dwarf project: Eclipsing binaries – precise clocks to discover exoplanets

Pribulla, T.; Vaňko, M.; Eiff, M. Ammler‐von; Андреев, М. В.; Aslantürk, A.; Awadalla, N. S.; Baludansky, D.; Bonanno, A.; Bozic, H.; Catanzaro, G.; Çelik, L.; Christopoulou, P. E.; Covino, E.; Cusano, F.; Dimitrov, D.; Dubovský, Pavol A.; Eigmueller, P.; Esmer, Ekrem Murat; Frasca, A.; Hambálek, Ľ.; Hanna, Magdy A.; Hanslmeier, A.; Kalomeni, B.; Kjurkchieva, D.; Krushevska, V.; Kudzej, Igor; Kundra, E.; Kuznyetsova, Yu.; Lee, J.W.; Leitzinger, M.; Maciejewski, G.; Moldovan, Dan; Morais, M. H. M.; Mugrauer, M.; Neuhäuser, R.; Niedzielski, A.; Odert, P.; Ohlert, J.; Özavcı, İ.; Παπαγεωργίου, Αθανάσιος; Parimucha, Š.; Poddaný, S.; Pop, Alexandru; Raetz, M.; Raetz, St.; Romanyuk, Ya. O.; Ruždjak, Domagoj; Schulz, J.; Şenavcı, H. V.; Srdoč, Gregor; Szalai, T.; Székely, P.; Sudar, D.; Tezcan, Cihan Tuğrul; Törün, M.E.; Turcu, Vlad; Vince, O.; Zejda, Miloslav

doi:10.1002/asna.201211722

Cited by 68 publications

(19 citation statements)

References 65 publications

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“…More advanced amateurs with similar equipment might become interested to join the enterprise of searching for long-period planets via the LTT effect in collaboration with professionals. Potential targets and work in this direction are described by Pribulla et al (2012) and Backhaus et al (2012).…”

Section: Discussionmentioning

confidence: 99%

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On the ephemeris of the eclipsing polar HU Aquarii

Schwope

Thinius

2014

Astron Nachr

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The magnetic cataclysmic variable HU Aquarii displayed pronounced quasi-periodic modulations of its eclipse timing. These were interpreted in terms of the light-travel time (LTT) effect caused by a circumbinary planet or planetary system. We report new photometric observations that revealed another precise eclipse timing for the October 2013 epoch, the first obtained in a high accretion state after many years in low or intermediate states. The eclipse was observed to occur earlier by 95.3 ± 2.0 s or 62.8 ± 2.0 s than expected for an assumed linear or quadratic ephemeris, respectively. The implied apparent strong evolution of the orbital period calls for a revision of the current planetary model or the planetary parameters. The object deserves further monitoring to uncover the true nature of the observed variability and to constrain the properties of the proposed planet or planetary system. The new observations prove that advanced amateur equipment can successfully be used in the growing field of planet search in wide circumbinary orbits via the LTT effect.

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Section: Discussionmentioning

confidence: 99%

“…with M 1 , M 2 , M 3 being the masses of the three bodies and P 3 the period of the third body around the binary (Pribulla et al 2012). Taken the measured peak-to-peak amplitudes at face value, planetary masses of 22 and 38 Jupiter masses for an assumed period of 6.9 years are derived.…”

Section: Discussionmentioning

confidence: 99%

On the ephemeris of the eclipsing polar HU Aquarii

Schwope

Thinius

2014

Astron Nachr

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“…To distinguish between Applegate modulations and period variations caused by planets via the light travel time effect (see, e.g. Pribulla et al 2012), long-term measurements are necessary to find correlations between activity indicators, luminosity variations due to photospheric temperature changes and the binary period modulation (Applegate 1992, see, e.g.). Changes in the rotational profile on the 1 % level may lead to tiny deformations on a similar order of magnitude as the active component oscillates between an oblate and a prolate state which is also expected to correlate with the activity cycle (Applegate 1992;Lanza et al 1998;Rüdiger et al 2002, see, e.g.).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Physics of the Applegate mechanism: Eclipsing time variations from magnetic activity

Völschow

Schleicher

Banerjee

et al. 2018

A&A

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Since its proposal in 1992, the Applegate mechanism has been discussed as a potential intrinsical mechanism to explain transit timing variations in various kinds of close binary systems. Most analytical arguments presented so far focused on the energetic feasibility of the mechanism, while applying rather crude one-or two-zone prescriptions to describe the exchange of angular momentum within the star. In this paper, we present the most detailed approach to date to describe the physics giving rise to the modulation period from kinetic and magnetic fluctuations. Assuming moderate levels of stellar parameter fluctuations, we find that the resulting binary period variations are one or two orders of magnitude lower than the observed values in RS-CVn like systems, supporting the conclusion of existing theoretical work that the Applegate mechanism may not suffice to produce the observed variations in these systems. The most promising Applegate candidates are low-mass post-common-envelope binaries (PCEBs) with binary separations 1 R ⊙ and secondary masses in the range of 0.30 M ⊙ and 0.36 M ⊙ .

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“…The standard deviation of the phase shifts was adopted as the error value. In order to compare this phase shift to O-C data acquired in the optical regime, we combine data derived by Lohr et al (2013), Zhang et al (2014) and Pribulla et al (2012). The resulting O-C diagram is displayed in Figure 4, along with a quadratic fit of all available optical data.…”

Section: Uv Rangementioning

confidence: 99%

“…) with black dots. The DWARF project data (Pribulla et al 2012) are displayed as blue diamonds. The XMM-Newton OM minimum is highlighted in red.…”

Section: Uv Rangementioning

confidence: 99%

X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

Perdelwitz

Czesla

Robrade

et al. 2018

A&A

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Context. Close binary systems provide an excellent tool to determine stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, which has been postulated to be the underlying reason for radius inflation in many of the components. Aims. We aim to extend the sample of low-mass binary systems with well-known X-ray properties. Methods. For this, we analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve is modeled with the eclipsing binary modeling tool phoebe and data acquired with the EPIC cameras is analyzed to search for hints of orbital modulation. Results. We find clear evidence of orbital modulation in the UV light curve and show that phoebe is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on phoenix models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

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The Dwarf project: Eclipsing binaries – precise clocks to discover exoplanets

Abstract: We present a new observational campaign, DWARF, aimed at detection of circumbinary extrasolar planets using the timing www.an-journal.org

Cited by 68 publications

References 65 publications

On the ephemeris of the eclipsing polar HU Aquarii

On the ephemeris of the eclipsing polar HU Aquarii

Physics of the Applegate mechanism: Eclipsing time variations from magnetic activity

X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

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