Tidally induced migration of <i>TESS</i> gas giants orbiting M dwarfs

Alvarado-Montes, Jaime A.

doi:10.1093/mnras/stac2741

Cited by 4 publications

(1 citation statement)

References 67 publications

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“…In addition, the mass of the planet is not sufficient for wave breaking to occur, and thus internal gravity waves in radiative zones would not be fully damped by tidal forcing (Barker 2020). The results presented here agree with those in Alvarado-Montes (2022), where the orbital evolution of TOI-1899 b induced by stellar tides is also minimum and not significant for most stellar rotation periods, with migration timescales being generally 10 Gyr.…”

Section: Tidally Induced Evolutionsupporting

confidence: 79%

The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters

Lin

Libby-Roberts

Alvarado-Montes

et al. 2023

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TOI-1899 b is a rare exoplanet, a temperate warm Jupiter orbiting an M dwarf, first discovered by Cañas et al. (2020) from a TESS single-transit event. Using new radial velocities (RVs) from the precision RV spectrographs HPF and NEID, along with additional TESS photometry and ground-based transit follow-up, we are able to derive a much more precise orbital period of P = 29.090312 − 0.000035 + 0.000036 days, along with a radius of R p = 0.99 ± 0.03 R J. We have also improved the constraints on planet mass, M p = 0.67 ± 0.04 M J, and eccentricity, which is consistent with a circular orbit at 2σ ( e = 0.044 − 0.027 + 0.029 ). TOI-1899 b occupies a unique region of parameter space as the coolest known (T eq ≈ 380 K) Jovian-sized transiting planet around an M dwarf; we show that it has great potential to provide clues regarding the formation and migration mechanisms of these rare gas giants through transmission spectroscopy with JWST, as well as studies of tidal evolution.

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Section: Tidally Induced Evolutionsupporting

confidence: 79%

The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters

Lin

Libby-Roberts

Alvarado-Montes

et al. 2023

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The GAPS programme at TNG

Maldonado¹,

Petralia²,

Mantovan³

et al. 2023

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Context. Massive substellar companions orbiting active low-mass stars are rare. They, however, offer an excellent opportunity to study the main mechanisms involved in the formation and evolution of substellar objects. Aims. We aim to unravel the physical nature of the transit signal observed by the TESS space mission on the active M dwarf TOI-5375. Methods. We analysed the available TESS photometric data as well as high-resolution (R ~ 115 000) HARPS-N spectra. We combined these data to characterise the star TOI-5375 and to disentangle signals related to stellar activity from the companion transit signal in the light-curve data. We ran a Markov chain Monte Carlo analysis to derive the orbital solution and applied state-of-the-art Gaussian process regression to deal with the stellar activity signal. Results. We reveal the presence of a companion in the boundary between the brown dwarfs and the very-low-mass stars orbiting around the star TOI-5375. The best-fit model corresponds to a companion with an orbital period of 1.721564 ± 10−6 d, a mass of 77 ± 8 MJ, and a radius of 0.99 ± 0.16 RJ. Conclusions. We derive a rotation period for the host star of 1.9692 ± 0.0004 d, and we conclude that the star is very close to synchronising its rotation with the orbital period of the companion.

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Constraints on tidal quality factor in Kepler eclipsing binaries using tidal synchronization: a frequency-dependent approach

Patel

Penev

Schussler

2023

Monthly Notices of the Royal Astronomical Society

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Tidal dissipation in binary systems is the primary source for synchronization and circularization of the objects in the system. The efficiency of the dissipation of tidal energy inside stars or planets results in significant changes in observed properties of the binary system and is often studied empirically using a parameter, commonly known as the modified tidal quality factor (${Q_{\star }^{\prime }}$). Though often assumed constant, in general that parameter will depend on the particular tidal wave experiencing the dissipation and the properties of the tidally distorted object. In this work we study the frequency dependence of ${Q_{\star }^{\prime }}$ for Sun-like stars. We parameterize ${Q_{\star }^{\prime }}$ as a saturating power-law in tidal frequency and obtain constraints using the stellar rotation period of 70 eclipsing binaries observed by Kepler. We use Bayesian analysis to account for the uncertainties in the observational data required for tidal evolution. Our analysis shows that ${Q_{\star }^{\prime }}$ is well constrained for tidal periods >15 days, with a value of ${Q_{\star }^{\prime }}\sim 10^8$ for periods >30 days and a slight suggested decrease at shorter periods. For tidal periods <15 days, ${Q_{\star }^{\prime }}$ is no longer tightly constrained, allowing for a broad range of possible values that overlaps with the constraints obtained using tidal circularization in binaries, which point to much more efficient dissipation: ${Q_{\star }^{\prime }}\sim 10^6$.

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Tidally induced migration of TESS gas giants orbiting M dwarfs

Cited by 4 publications

References 67 publications

The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters

The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters

The GAPS programme at TNG

Constraints on tidal quality factor in Kepler eclipsing binaries using tidal synchronization: a frequency-dependent approach

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