The Telltale Heartbeat: Detection and Characterization of Eccentric Orbiting Planets via Tides on Their Host Star

Penoyre, Zephyr; Stone, Nicholas C.

doi:10.3847/1538-3881/aaf965

Cited by 11 publications

(6 citation statements)

References 71 publications

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“…The very similar issues for observations of stars with dynamical tides have also been discussed (e.g. Arras et al 2012, Penoyre & Stone 2019 recently.…”

Section: Data Ava I L a B I L I T Ysupporting

confidence: 54%

A unicorn in monoceros: the 3 M⊙ dark companion to the bright, nearby red giant V723 Mon is a non-interacting, mass-gap black hole candidate

Jayasinghe

Stanek

Thompson

et al. 2021

Monthly Notices of the Royal Astronomical Society

104

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We report the discovery of the closest known black hole candidate as a binary companion to V723 Mon. V723 Mon is a nearby ($d\sim 460\, \rm pc$), bright (V ≃ 8.3 mag), evolved (Teff, giant ≃ 4440 K, and Lgiant ≃ 173 L⊙) red giant in a high mass function, f(M) = 1.72 ± 0.01 M⊙, nearly circular binary (P = 59.9 d, e ≃ 0). V723 Mon is a known variable star, previously classified as an eclipsing binary, but its All-Sky Automated Survey, Kilodegree Extremely Little Telescope, and Transiting Exoplanet Survey Satellite light curves are those of a nearly edge-on ellipsoidal variable. Detailed models of the light curves constrained by the period, radial velocities, and stellar temperature give an inclination of $87.0^{\circ ^{+1.7^\circ }}_{-1.4^\circ }$, a mass ratio of q ≃ 0.33 ± 0.02, a companion mass of Mcomp = 3.04 ± 0.06 M⊙, a stellar radius of Rgiant = 24.9 ± 0.7 R⊙, and a giant mass of Mgiant = 1.00 ± 0.07 M⊙. We identify a likely non-stellar, diffuse veiling component with contributions in the B and V band of ${\sim }63{{\ \rm per\ cent}}$ and ${\sim }24{{\ \rm per\ cent}}$, respectively. The SED and the absence of continuum eclipses imply that the companion mass must be dominated by a compact object. We do observe eclipses of the Balmer lines when the dark companion passes behind the giant, but their velocity spreads are low compared to observed accretion discs. The X-ray luminosity of the system is $L_{\rm X}\simeq 7.6\times 10^{29}~\rm ergs~s^{-1}$, corresponding to L/Ledd ∼ 10−9. The simplest explanation for the massive companion is a single compact object, most likely a black hole in the ‘mass gap’.

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“…The very similar issues for observations of stars with dynamical tides have also been discussed (e.g. Arras et al 2012, Penoyre & Stone 2019 recently.…”

Section: Data Ava I L a B I L I T Ysupporting

confidence: 54%

A unicorn in monoceros: the 3 M⊙ dark companion to the bright, nearby red giant V723 Mon is a non-interacting, mass-gap black hole candidate

Jayasinghe

Stanek

Thompson

et al. 2021

Monthly Notices of the Royal Astronomical Society

104

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“…The gravitational effect of a hot Jupiter, however, provides external forcing of the oscillation through the time-varying tidal potential. Such tidally excited oscillations have been studied in various regimes, from stellar binaries (Quataert et al 1995) to planetary companions (Terquem et al 1998), including studies with orbital eccentricities both small ) and large ; Fuller (2017); Penoyre & Stone (2018)). mation.…”

Section: Introductionmentioning

confidence: 99%

Non–adiabatic tidal oscillations induced by a planetary companion

Bunting

Papaloizou

Terquem

2019

Monthly Notices of the Royal Astronomical Society

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We calculate the dynamical tides raised by a close planetary companion on nonrotating stars of 1 M and 1.4 M . Using the Henyey method, we solve the fully nonadiabatic equations throughout the star. The horizontal Lagrangian displacement is found to be 10 to 100 times larger than the equilibrium tide value in a thin region near the surface of the star. This is because non-adiabatic effects dominate in a region that extends from below the outer edge of the convection zone up to the stellar surface, and the equilibrium tide approximation is inconsistent with non-adiabaticity. Although this approximation generally applies in the low frequency limit, it also fails in the parts of the convection zone where the forcing frequency is small but larger than the Brunt-Väisälä frequency. We derive analytical estimates which give a good approximation to the numerical values of the magnitude of the ratio of the horizontal and radial displacements at the surface. The relative surface flux perturbation is also significant, on the order of 0.1% for a system modelled on 51 Pegasi b. Observations affected by the horizontal displacement may therefore be more achievable than previously thought, and brightness perturbations may be the result of flux perturbations rather than due to the radial displacement. We discuss the implication of this on the possibility of detecting such tidally excited oscillations, including the prospect of utilising the large horizontal motion for observations of systems such as 51 Pegasi.

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“…Tidal oscillations have also been investigated more directly, as they lead to the surface of the star varying periodically. This can result in both photometric and spectroscopic variations, and has been investigated in the context of stellar binaries (Quataert et al 1996) and planetary companions, for eccentricities both small (Terquem et al (1998); Arras et al (2012)) and large (Burkart et al (2012); Fuller (2017); Penoyre & Stone (2019)).…”

Section: Introductionmentioning

confidence: 99%

Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables

Bunting

Terquem

2020

Monthly Notices of the Royal Astronomical Society

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We calculate the conversion from non–adiabatic, non–radial oscillations tidally induced by a hot Jupiter on a star to observable spectroscopic and photometric signals. Models with both frozen convection and an approximation for a perturbation to the convective flux are discussed. Observables are calculated for some real planetary systems to give specific predictions. Time–dependent line broadening and the radial velocity signal during transit are both investigated as methods to provide further insight into the nature of the stellar oscillations. The photometric signal is predicted to be proportional to the inverse square of the orbital period, P−2, as in the equilibrium tide approximation. However, the radial velocity signal is predicted to be proportional to P−1, and is therefore much larger at long orbital periods than the signal corresponding to the equilibrium tide approximation, which is proportional to P−3. The prospects for detecting these oscillations and the implications for the detection and characterisation of planets are discussed.

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The Telltale Heartbeat: Detection and Characterization of Eccentric Orbiting Planets via Tides on Their Host Star

Cited by 11 publications

References 71 publications

A unicorn in monoceros: the 3 M⊙ dark companion to the bright, nearby red giant V723 Mon is a non-interacting, mass-gap black hole candidate

A unicorn in monoceros: the 3 M⊙ dark companion to the bright, nearby red giant V723 Mon is a non-interacting, mass-gap black hole candidate

Non–adiabatic tidal oscillations induced by a planetary companion

Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables

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