Constraints on PDS 70 b and c from the dust continuum emission of the circumplanetary discs considering in situ dust evolution

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Volume 687 (July 2024)

A&A, 687 (2024) A166

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Table 2

Estimates of important properties by previous works.

PDS 70 b	Value	Observation types	Reference
Planet mass (M_J)	5–9	IR colours and evolution model	Keppler et al. (2018)
	2–17	SED (IR)⁽¹⁾	Müller et al. (2018)
	12	Hα 10% and 50% width	Aoyama & Ikoma (2019)
	1.1–11.6	Dynamical stability (95%)	Wang et al. (2021)
	4	Gap depth	Portilla-Revelo et al. (2023)

Gas accretion rate (M_J yr⁻¹)	1 × 10^−8±1	SED (IR) and TTS empirical relation⁽¹⁾	Wagner et al. (2018)
	2 × 10^−8±0.4	Hα 10% width and TTS empirical relation	Haffert et al. (2019)
	1 × 10^−8±0.6	Hα luminosity and magnetospheric accretion^(1,2)	Thanathibodee et al. (2019)
	4 × 10⁻⁸	Hα 10% and 50% width and Hα luminosity⁽¹⁾	Aoyama & Ikoma (2019)

MMdot $(M_{J}^{2} {y r}^{- 1})$ $\[\left(M_{\mathrm{J}}^2 \mathrm{~yr}^{-1}\right)\]$	<1.26 × 10⁻⁶	Brγ luminosity and TTS empirical relation⁽¹⁾	Christiaens et al. (2019b)
	10⁻⁶⁸−10⁻⁶³	SED (IR) and CPD model⁽¹⁾	Christiaens et al. (2019a)
	4.8 × 10⁻⁷	Hα luminosity⁽¹⁾	Aoyama & Ikoma (2019)
	(2.5–7.5) × 10⁻⁷	SED (IR)⁽¹⁾	Stolker et al. (2020)
	(1–10) × 10⁻⁷	SED (IR) and CPD model	Wang et al. (2021)
	(1.6 ± 0.23) × 10⁻⁸	UV and Hα luminosity⁽¹⁾	Zhou et al. (2021)

PDS 70 c

Planet mass	4–12	K-L colour and evolution model	Haffert et al. (2019)
	10	Hα 10% and 50% width	Aoyama & Ikoma (2019)
	1.4–14.5	Dynamical stability (95%)	Wang et al. (2021)
	4	Gap depth	Portilla-Revelo et al. (2023)

Gas accretion rate	1 × 10^−8±0.4	Hα 10% width and TTS empirical relation⁽¹⁾	Haffert et al. (2019)
	1 × 10^−81±0.6	Hα luminosity and magnetospheric accretion^(1,2)	Thanathibodee et al. (2019)
	1 × 10⁻⁸	Hα 10% and 50% width and Hα luminosity⁽¹⁾	Aoyama & Ikoma (2019)

MMdot	1 × 10⁻⁷	Hα luminosity⁽¹⁾	Aoyama & Ikoma (2019)
	(1–10) × 10⁻⁷	SED (IR) and CPD model	Wang et al. (2021)

PDS 70

Gas accretion rate	(1.4 ± 0.8) × 10⁻⁷	Hα profiles and magnetospheric accretion	Thanathibodee et al. (2020)

Notes. ⁽¹⁾The effects of the extinction is not included. ⁽²⁾The planet mass is assumed as 6 M_J.

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