Planet-star interactions with precise transit timing - IV. Probing the regime of dynamical tides for GK host stars

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Volume 692 (December 2024)

A&A, 692 (2024) A35

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Table 2

Observational constraints (with 95% confidence) and theoretical predictions on the values of Q′_⋆,WB.

Q′_⋆,WB	Type, source
	HATS-18 b
$> {3.5}_{- 0.7}^{+ 0.5} \times 10^{5}$ $> 3.5_{ - 0.7}^{ + 0.5} \times {10^5}$	Observational, this study
$> {1.29}_{- 0.11}^{+ 0.12} \times 10^{5}$ $> 1.29_{ - 0.11}^{ + 0.12} \times {10^5}$	observ., Southworth et al. (2022)
<2.6 × 10⁵	Theoretical WB^(a), this study
~1.1 × 10⁵	Theoretical WB^(a), Barker (2020)
~1.2 × 10⁵	Theor. WB^(a), Southworth et al. (2022)
~5.5 × 10⁵	Theoretical WNL^(b), this study
~(1–2.4) × 10⁷	spin-up^(c), Penev et al. (2018)

	HIP 65A b
$> {7.6}_{- 0.7}^{+ 0.8} \times 10^{4}$ $> 7.6_{ - 0.7}^{ + 0.8} \times {10^4}$	Observational, this paper
(1.2–1.5) × 10⁵	Theoretical WB^(a), this study
~1.3 × 10⁶	Theoretical WNL^(b), this study
>10⁸	spin-up^(c), Nielsen et al. (2020)

	TrES-3 b
$> {2.50}_{- 0.14}^{+ 0.12} \times 10^{5}$ $> 2.50_{ - 0.14}^{ + 0.12} \times {10^5}$	Observational, this paper
~1.1 × 10⁵	Observ., Mannaday et al. (2020)
>2 8 × 10⁶	Observ., Mannaday et al. (2022)
(4.2–6.4) × 10⁵	Theoretical WB^(a), this study
~6.5 × 10⁵	Theoretical WB^(a), Barker (2020)
~2.5 × 10⁶	Theoretical WNL^(b), this study
>4 × 10⁶	spin-up^(c), Penev et al. (2018)

	WASP-19 b
$> {4.79}_{- 0.29}^{+ 0.31} \times 10^{6}$ $> 4.79_{ - 0.29}^{ + 0.31} \times {10^6}$	Observational, this paper
=(5.0 ± 1.5) × 10⁵	Observational, Patra et al. (2020)
=(7 ± 1) × 10⁵	Observational, KP23
>(1.23 ± 0.23) × 10⁶	Observational, Petrucci et al. (2020)
>(1.26 ± 0.10) × 10⁶	Observational, Rosário et al. (2022)
<0.9 × 10⁵	Theoretical WB^(a), this study
~(0.6-0.8) × 10⁵	Theoretical WB^(a), Barker (2020)
~4.2 × 10⁵	Theoretical WNL^(b), this study
~(6.5-8.1) × 10⁶	spin-up^(c), Penev et al. (2018)

	WASP-43 b
$> {1.15}_{- 0.50}^{+ 0.53} \times 10^{6}$ $> 1.15_{ - 0.50}^{ + 0.53} \times {10^6}$	Observational, this paper
~10⁵	Observational, Jiang et al. (2016)
>10⁵	Observational, Hoyer et al. (2016)
>1.5 × 10⁵	Observational, Sun et al. (2018)
>(2.1 ± 1.4) × 10⁵	Observational, Patra et al. (2020)
>(4.0 ± 1.2) × 10⁵	Observational, Davoudi et al. (2021)
(0.8–1.0) × 10⁵	Theoretical WB^(a), this study
~1.3 10⁵	Theoretical WB^(a), Barker (2020)
~5.9 × 10⁵	Theoretical WNL^(b), this study
~(2.6–6.1) × 10⁷	spin-up^(c), Penev et al. (2018)

	WASP-173A b
$> {1.50}_{- 0.16}^{+ 0.19} \times 10^{5}$ $> 1.50_{ - 0.16}^{ + 0.19} \times {10^5}$	Observational, this paper
<1.5× 10⁶	Theoretical WB^(a), this study
~2 9 × 10⁶	Theoretical WNL^(b), this study
~1.6 × 10⁶	Spin-up^(c) ,LB19

Notes. ^(a) For dissipation of IGWs in radiation zones if WB occurs. ^(b) For dissipation of WNL dynamical tides, interpolated from Table 4 of Weinberg et al. (2024). ^(c) From tidal spin-up of the host star. References: KP23 – Korth & Parviainen (2023), LB19 – Labadie-Bartz et al. (2019).

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