The Equations of Ellipsoidal Star Variability Applied to HR 8427

Morris, Steven L.; Naftilan, S. A.

doi:10.1086/173488

Cited by 142 publications

(156 citation statements)

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“…If the third harmonic was entirely tidal effects, it would be expected to be similar to the effect on a single star in a binary system as described by Morris & Naftilan (1993):…”

Section: Tidal Effectsmentioning

confidence: 96%

“…Using a least-squares fit with a three-harmonic model, we measured the amplitude of the third harmonic. In Morris & Naftilan (1993) tidal effects between binary stars were expected to produce high order harmonics at frequencies that are multiples of the orbital period. These tidal effects were applied to Kepler-13b in Shporer et al Table 2.…”

Section: Tidal Effectsmentioning

confidence: 99%

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High-order harmonics in light curves of Kepler planets

Armstrong

Rein

2015

Monthly Notices of the Royal Astronomical Society: Letters

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The Kepler mission was launched in 2009 and has discovered thousands of planet candidates. In a recent paper, Esteves et al. (2013) found a periodic signal in the light curves of KOI-13 and HAT-P-7, with a frequency triple the orbital frequency of a transiting planet. We found similar harmonics in many systems with a high occurrence rate. At this time, the origins of the signal are not entirely certain.We look carefully at the possibility of errors being introduced through our data processing routines but conclude that the signal is real. The harmonics on multiples of the orbital frequency are a result of non-sinusoidal periodic signals. We speculate on their origin and generally caution that these harmonics could lead to wrong estimates of planet albedos, beaming mass estimates, and ellipsoidal variations.

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“…If the third harmonic was entirely tidal effects, it would be expected to be similar to the effect on a single star in a binary system as described by Morris & Naftilan (1993):…”

Section: Tidal Effectsmentioning

confidence: 96%

Section: Tidal Effectsmentioning

confidence: 99%

High-order harmonics in light curves of Kepler planets

Armstrong

Rein

2015

Monthly Notices of the Royal Astronomical Society: Letters

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“…soidal signal, with Beech 1989;Morris & Naftilan 1993). Here a is the semi-major axis of the companion, q ≡ m p /m c is the mass ratio and f ell (of order unity) depends on the properties of the atmosphere and the CCD response (see §4.1 for details).…”

Section: Tidal Deformation and Direct Irradiationmentioning

confidence: 99%

An Active, Asynchronous Companion to a Redback Millisecond Pulsar

Staden

Antoniadis

2016

ApJL

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PSR J1723−2837 is a "redback" millisecond pulsar (MSP) with a low-mass companion in a 14.8 h orbit. The system's properties closely resemble those of "transitional" MSPs that alternate between spin-down and accretion-powered states. In this paper we report on long-term photometry of the 15.5 mag companion to the pulsar. We use our data to illustrate that the star experiences sporadic activity, which we attribute to starspots. We also find that the companion is not tidally locked and infer P s /P b = 0.9974 (7) for the ratio between the rotational and orbital periods. Finally, we place constraints on various parameters, including the irradiation efficiency and pulsar mass. We discuss similarities with other redback MSPs and conclude that starspots may provide the most likely explanation for the often seen irregular and asymmetric optical lightcurves.

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“…We calculate a similar expression for the secondary and then weight them by the expected blackbody fluxes in order to obtain the total relative variation of the binary. Morris & Naftilan (1993) also provide a prescription for calculating the amplitude of the reflection effect. They assume that each star absorbs some of the bolometric flux of its companion, which heats the stellar hemisphere facing the companion, inducing an asymmetric increased emission.…”

Section: The Amplitude Of the Beaming Effect As Compared With The Ellmentioning

confidence: 99%

Beaming Binaries: A New Observational Category of Photometric Binary Stars

Zucker

Mazeh

Alexander

2007

ApJ

171

162

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The new photometric spaceborne survey missions COROT and Kepler will be able to detect minute flux variations in binary stars due to relativistic beaming caused by the line-of-sight motion of their components. In all but very short period binaries (P > 10 days), these variations will dominate over the ellipsoidal and reflection periodic variability. Thus, COROT and Kepler will discover a new observational class: photometric beaming binary stars. We examine this new category and the information that the photometric variations can provide. The variations that result from the observatory heliocentric velocity can be used to extract some spectral information even for single stars.

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The Equations of Ellipsoidal Star Variability Applied to HR 8427

Cited by 142 publications

References 0 publications

High-order harmonics in light curves of Kepler planets

High-order harmonics in light curves of Kepler planets

An Active, Asynchronous Companion to a Redback Millisecond Pulsar

Beaming Binaries: A New Observational Category of Photometric Binary Stars

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