1985
DOI: 10.1086/163359
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The ellipsoidal variable stars

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Cited by 216 publications
(220 citation statements)
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“…The mutual gravitational interaction between members of a binary will induce nominally prolate distortions of their surfaces having major axes along the line connecting their centers. As a result, the sky-projected cross-sectional area, and consequently the observed flux, is time variable (Morris 1985; see also Pfahl et al 2008). For a circular orbit, the expected maxima of this variation occur twice per orbit at the quadratures (generating a large cos(2φ) amplitude).…”
Section: Doppler Boostingmentioning
confidence: 98%
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“…The mutual gravitational interaction between members of a binary will induce nominally prolate distortions of their surfaces having major axes along the line connecting their centers. As a result, the sky-projected cross-sectional area, and consequently the observed flux, is time variable (Morris 1985; see also Pfahl et al 2008). For a circular orbit, the expected maxima of this variation occur twice per orbit at the quadratures (generating a large cos(2φ) amplitude).…”
Section: Doppler Boostingmentioning
confidence: 98%
“…For a circular orbit, the expected maxima of this variation occur twice per orbit at the quadratures (generating a large cos(2φ) amplitude). Kopal (1959) calculated the ELV contribution to the out-ofeclipse harmonic content as (where we follow the notation by Morris 1985):…”
Section: Doppler Boostingmentioning
confidence: 99%
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“…where u = 1.2 is the linear limb-darkening coefficient in the Kepler passband, τ g ∼ 0.32 the gravity-darkening coefficient estimated for the primary LHS 6343 A, and we neglected the effects related to the precession constant and the (small) eccentricity of the orbit (cf., Morris 1985). Note that at mid-eclipse, M = M e , and the ellipsoidal variation is at a minimum, while for M = M e ± π/2, that is, in quadrature, it reaches a maximum.…”
Section: Models Of the Doppler-beaming And Ellipticity Effectmentioning
confidence: 90%
“…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). The reflection variation is caused by the brightness difference between A&A 580, A21 (2015) the "day" side and the "night" side of each component (e.g., Wilson 1990;Harrison et al 2003).…”
Section: Introductionmentioning
confidence: 99%