Beaming Binaries: A New Observational Category of Photometric Binary Stars

Zucker, S.; Mazeh, T.; Alexander, Tal

doi:10.1086/521389

Cited by 171 publications

(172 citation statements)

References 17 publications

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“…Doing so, we estimate that observing all 481 selected candidates would have brought the number of confirmed binaries to ∼110, and that the expected number of beaming binaries that can be detected in CoRoT long-run light curves is ∼300. This confirms the prediction made by Zucker et al (2007): CoRoT and Kepler will be capable of detecting hundreds of non-eclipsing beaming binaries.…”

Section: Mass Ratio and Orbital Period Distribution Of The Beer Corotsupporting

confidence: 89%

“…However, as mentioned by Loeb & Gaudi (2003) and by Zucker et al (2007), for short-period binaries and planets, the amplitude of the beaming effect might be comparable to (or even smaller than) another two photometric effectsthe ellipsoidal and the reflection light variations. The ellipsoidal variation is caused by tidal interactions between the two components of the binary (e.g., Morris 1985;Mazeh 2008).…”

Section: Introductionmentioning

confidence: 90%

“…Using Kepler data, Mosser et al (2013) A21, page 11 of 27 A&A 580, A21 (2015) have shown that solar-like oscillations of 1-2 M red giants have frequencies of 1-10 μHz (periods of 1.2-12 days), amplitudes (A max ) of 0.1-1 mmag, and that the amplitude increases with the period as a power law. For BEER binaries, the photometric amplitude decreases with the period (Zucker et al 2007). However, it appears that for periods of about 1-10 days, these two phenomena might have similar photometric amplitudes.…”

Section: Spectral Typementioning

confidence: 98%

“…For stellar binaries with typical RV semi-amplitudes of 10−100 km s −1 , the beaming amplitudes are in the range of 10 −3 -10 −4 . For this reason, Zucker et al (2007) have predicted that CoRoT and Kepler will also detect hundreds of non-eclipsing binaries of this type, and create a new observational category: beaming binaries.…”

Section: Introductionmentioning

confidence: 99%

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BEER analysis ofKeplerand CoRoT light curves

Tal-Or

Faigler

Mazeh

2015

A&A

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Context. The BEER algorithm searches stellar light curves for the BEaming, Ellipsoidal, and Reflection photometric modulations that are caused by a short-period companion. These three effects are typically of very low amplitude and can mainly be detected in light curves from space-based photometers. Unlike eclipsing binaries, these effects are not limited to edge-on inclinations. Aims. Applying the algorithm to wide-field photometric surveys such as CoRoT and Kepler offers an opportunity to better understand the statistical properties of short-period binaries. It also widens the window for detecting intrinsically rare systems, such as shortperiod brown-dwarf and massive-planetary companions to main-sequence stars. Methods. Applying the search to the first five long-run center CoRoT fields, we identified 481 non-eclipsing candidates with periodic flux amplitudes of 0.5-87 mmag. Optimizing the Anglo-Australian-Telescope pointing coordinates and the AAOmega fiberallocations with dedicated softwares, we acquired six spectra for 231 candidates and seven spectra for another 50 candidates in a seven-night campaign. Analysis of the red-arm AAOmega spectra, which covered the range of 8342-8842 Å, yielded a radial-velocity precision of ∼1 km s −1 . Spectra containing lines of more than one star were analyzed with the two-dimensional correlation algorithm TODCOR. Results. The measured radial velocities confirmed the binarity of seventy of the BEER candidates -45 single-line binaries, 18 doubleline binaries, and 7 diluted binaries. We show that red giants introduce a major source of false candidates and demonstrate a way to improve BEER's performance in extracting higher fidelity samples from future searches of CoRoT light curves. The periods of the confirmed binaries span a range of 0.3-10 days and show a rise in the number of binaries per ΔlogP toward longer periods. The estimated mass ratios of the double-line binaries and the mass ratios assigned to the single-line binaries, assuming an isotropic inclination distribution, span a range of 0.03-1. On the low-mass end, we have detected two brown-dwarf candidates on a ∼1 day period orbit. Conclusions. This is the first time non-eclipsing beaming binaries are detected in CoRoT data, and we estimate that ∼300 such binaries can be detected in the CoRoT long-run light curves.

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Section: Mass Ratio and Orbital Period Distribution Of The Beer Corotsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 90%

Section: Spectral Typementioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

BEER analysis ofKeplerand CoRoT light curves

Tal-Or

Faigler

Mazeh

2015

A&A

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“…It was first observed by Maxted et al (2000). Its expected detection in Kepler light curves was suggested and discussed by Loeb & Gaudi (2003) and Zucker et al (2007). Van Kerkwijk et al (2010) report the detection of Doppler beaming in the long cadence Kepler light curve of the binary KOI-74.…”

Section: Doppler Beaming Factormentioning

confidence: 91%

Kepler Observations of the Beaming Binary KPD 1946+4340

Bloemen

2014

High-Precision Studies of Compact Variable Stars

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The Kepler Mission has acquired 33.5 d of continuous one-minute photometry of KPD 1946+4340, a short-period binary system that consists of a subdwarf B star (sdB) and a white dwarf. In the light curve, eclipses are clearly seen, with the deepest occurring when the compact white dwarf crosses the disc of the sdB (0.4 per cent) and the more shallow ones (0.1 per cent) when the sdB eclipses the white dwarf. As expected, the sdB is deformed by the gravitational field of the white dwarf, which produces an ellipsoidal modulation of the light curve. Spectacularly, a very strong Doppler beaming (also known as Doppler boosting) effect is also clearly evident at the 0.1 per cent level. This originates from the sdB's orbital velocity, which we measure to be 164.0 ± 1.9 km s −1 from supporting spectroscopy. We present light curve models that account for all these effects, as well as gravitational lensing, which decreases the apparent radius of the white dwarf by about 6 per cent when it eclipses the sdB. We derive system parameters and uncertainties from the light curve using Markov Chain Monte Carlo simulations. Adopting a theoretical white dwarf mass-radius relation, the mass of the subdwarf is found to be 0.47 ± 0.03 M ⊙ and the mass of the white dwarf 0.59 ± 0.02 M ⊙ . The effective temperature of the white dwarf is 15 900 ± 300 K. With a spectroscopic effective temperature of T eff = 34 730 ± 250 K and a surface gravity of log g = 5.43 ± 0.04, the subdwarf has most likely exhausted its core helium, and is in a shell He burning stage.The detection of Doppler beaming in Kepler light curves potentially allows one to measure radial velocities without the need of spectroscopic data. For the first time, a photometrically observed Doppler beaming amplitude is compared to a spectroscopically established value. The sdB's radial velocity amplitude derived from the photometry (168 ± 4 km s −1 ) is in perfect agreement with the spectroscopic value. After subtracting our best model for the orbital effects, we searched the residuals for stellar oscillations but did not find any significant pulsation frequencies.

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Mass Ratio from Doppler Beaming and Rømer Delay Versus Ellipsoidal Modulation in the Kepler Data of KOI-74

Bloemen

2014

High-Precision Studies of Compact Variable Stars

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Beaming Binaries: A New Observational Category of Photometric Binary Stars

Cited by 171 publications

References 17 publications

BEER analysis ofKeplerand CoRoT light curves

BEER analysis ofKeplerand CoRoT light curves

Kepler Observations of the Beaming Binary KPD 1946+4340

Mass Ratio from Doppler Beaming and Rømer Delay Versus Ellipsoidal Modulation in the Kepler Data of KOI-74

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