Doppler-beaming in the<i>Kepler</i>light curve of LHS 6343 A

Herrero, E.; Lanza, A. F.; Ribas, I.; Jordi, C.; Cameron, A. Collier; Morales, J. C.

doi:10.1051/0004-6361/201323087

Cited by 7 publications

(4 citation statements)

References 22 publications

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“…With 6 quarters of Kepler data, Herrero et al (2013) measured a photometric rotation period of 13.13 ± 0.02 days for LHS 6343 A. The authors also claimed to observe spotcrossing events during the transits of LHS 6343 A, as well as out-of-transit photometric modulation with a period consistent with the orbital period of LHS 6343 C. Herrero et al (2014) updated this work, concluding that the out-of-transit variations are dominated by relativistic Doppler beaming.…”

Section: Introductionmentioning

confidence: 57%

CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C

Montet

Johnson

Muirhead

et al. 2015

ApJ

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We present an updated analysis of LHS 6343, a triple system in the Kepler field which consists of a brown dwarf transiting one member of a widely separated M+M binary system. By analyzing the full Kepler data set and 34 Keck/ HIgh Resolution Echelle Spectrometer radial velocity observations, we measure both the observed transit depth and Doppler semiamplitude to 0.5% precision. With Robo-AO and Palomar/PHARO adaptive optics imaging as well as TripleSpec spectroscopy, we measure a model-dependent mass for LHS 6343 C of 62.1 ± 1.2 M Jup and a radius of 0.783 ± 0.011 R Jup . We detect the secondary eclipse in the Kepler data at 3.5σ , measuring e cos ω = 0.0228 ± 0.0008. We also derive a method to measure the mass and radius of a star and transiting companion directly, without any direct reliance on stellar models. The mass and radius of both objects depend only on the orbital period, stellar density, reduced semimajor axis, Doppler semiamplitude, eccentricity, and inclination, as well as the knowledge that the primary star falls on the main sequence. With this method, we calculate a mass and radius for LHS 6343 C to a precision of 3% and 2%, respectively.

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Section: Introductionmentioning

confidence: 57%

CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C

Montet

Johnson

Muirhead

et al. 2015

ApJ

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“…There is one source of variability which we would expect to produce the observed phase shift between the radial velocities and photometry. Relativistic effects caused by the radial motion of the star in its orbit, dominated by Doppler beaming, are known to result in pho- tometric variability at small levels (Shporer et al 2010;Bloemen et al 2011Bloemen et al , 2012Herrero et al 2014).…”

Section: Modelling Of the Atmosphere Light And Radial Velocity Curves...mentioning

confidence: 99%

Identifying close binary central stars of PN with Kepler

Marco

Long

Jacoby

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Six planetary nebulae (PN) are known in the Kepler space telescope field of view, three newly identified. Of the 5 central stars of PN with useful Kepler data, one, J 193110888+4324577, is a short-period, post common envelope binary exhibiting relativistic beaming effects. A second, the central star of the newly identified PN Pa 5, has a rare O(He) spectral type and a periodic variability consistent with an evolved companion, where the orbital axis is almost aligned with the line of sight. The third PN, NGC 6826 has a fast rotating central star, something that can only be achieved in a merger. Fourth, the central star of the newly identified PN Kn 61, has a PG1159 spectral type and a mysterious semi-periodic light variability which we conjecture to be related to the interplay of binarity with a stellar wind. Finally, the central star of the circular PN A 61 does not appear to have a photometric variability above 2 mmag. With the possible exception of the variability of Kn 61, all other variability behaviour, whether due to binarity or not, would not easily have been detected from the ground. We conclude, based on very low numbers, that there may be many more close binary or close binary products to be discovered with ultra-high precision photometry. With a larger number of high precision photometric observations we will be able to determine how much higher than the currently known 15 per cent, the short period binary fraction for central stars of PN is likely to be.

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“…The theoretical background of the relativistic beaming effect has been discussed for eclipsing binary stars (Zucker et al 2007) as well as for planetary systems (Loeb & Gaudi 2003). Using light curves of CoRoT and the Kepler satellite a few observations of this effect have been reported in the last years (Mazeh & Faigler 2010;van Kerkwijk et al 2010;Bloemen et al 2011;Herrero et al 2014;Faigler et al 2015;Tal-Or et al 2015). For a few transiting systems (Mazeh & Faigler 2010;Bloemen et al 2011;Faigler et al 2015) and even more non-transiting systems (Tal-Or et al 2015) spectroscopic radial velocity measurements are available.…”

Section: Relativistic Beamingmentioning

confidence: 99%

A transiting M-dwarf showing beaming effect in the field of Ruprecht 147

Eigmüller

Csizmadia

Endl

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We report the discovery and characterization of an eclipsing M5V dwarf star, orbiting a slightly evolved F7V main sequence star.In contrast to previous claims in the literature, we confirm that the system does not belong to the galactic open cluster Ruprecht 147. We determine its fundamental parameters combining K2 time-series data with spectroscopic observations from the McDonald Observatory, FIES@NOT, and HIRES@KECK. The very precise photometric data from the K2 mission allows us to measure variations caused by the beaming effect (relativistic doppler boosting), ellipsoidal variation, reflection, and the secondary eclipse. We determined the radial velocity using spectroscopic observations and compare it to the radial velocity determined from the beaming effect observed in the photometric data. The M5V star has a radius of 0.200 +0.007 −0.008 R and a mass of 0.187 +0.012 −0.013 M . The primary star has radius of 1.518 +0.038 −0.049 R and a mass of 1.008 +0.081 −0.097 M . The orbital period is 5.441995 ± 0.000007 days. The system is one of the few eclipsing systems with observed beaming effect and spectroscopic radial velocity measurements and it can be used as test case for the modelling of the beaming effect.Current and forthcoming space missions such as TESS and PLATO might benefit of the analysis of the beaming effect to estimate the mass of transiting companions without the need for radial velocity follow up observations, provided that the systematic sources of noise affecting this method are well understood.

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Doppler-beaming in theKeplerlight curve of LHS 6343 A

Cited by 7 publications

References 22 publications

CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C

CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C

Identifying close binary central stars of PN with Kepler

A transiting M-dwarf showing beaming effect in the field of Ruprecht 147

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