Simulating the escaping atmospheres of hot gas planets in the solar neighborhood

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Table 2

Uncertainties on the result of the simulations.

Source	Trend^a	Impact	Ref.

Stellar wind	(−)	uncert.	4
Three dimensional structure^b	(−)	× 4	1
Irradiation strength	(±)	× 3	2
Magnetic fields	(−)	× 3	3
Metals	(−)	× 2
Molecules^c (H₂)	(−)	× 2
Boundary density	(±)	50%
Temperature in lower atmosphere	(±)	10%

Notes.

^(a)

A negative trend indicates that the effect will reduce the simulated mass loss rates.

^(b)

Our mass-loss rates are reduced by this factor and the remaining uncertainty is smaller.

^(c)

Only moderately irradiated smaller planets host molecular winds.

Reference. Phenomena without reference are discussed in the text. (1) Stone & Proga (2009); (2) Salz et al. (2015b); (3) Trammell et al. (2014); (4) Murray-Clay et al. (2009).

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