Erosion of an exoplanetary atmosphere caused by stellar winds

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Volume 630 (October 2019)

A&A, 630 (2019) A52

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Table A.1

Physical characteristics of the stars described in Sect. 4.2.

Star	Spectral	Mass	Radius	Period	T_eff	R_o	Magnetic	Rotation	Calculated	D₂	D₃
	type	(in M_⊙)	(in R_⊙)	(days)	(K)		field (G)	regime	R_o	(AU)	(AU)
Sun ⁽¹⁾	G2V	1.00	1.00	28.0	5780	2.17	–	Unsaturated	2.17	0.95	1.68
GJ 182 ⁽²⁾	M0.5	0.75	0.82	4.4	3950	0.17	172	Unsaturated	0.17	0.40	0.75
DT Vir ⁽²⁾	M0.5	0.59	0.53	2.9	3790	0.09	149	Saturated	0.09	0.24	0.45
DS Leo ⁽²⁾	M0	0.58	0.52	15.7 ⁽⁷⁾	3770	–	87	Unsaturated	0.50	0.23	0.44
GJ 49 ⁽²⁾	M1.5	0.57	0.51	0.74 ⁽⁸⁾	3750	–	27	Saturated	0.02	0.22	0.43
OT Ser ⁽²⁾	M1.5	0.55	0.49	3.4	3690	0.10	123	Saturated	0.10	0.21	0.40
CE Boo ⁽²⁾	M2.5	0.48	0.43	14.7	3570	0.35	103	Unsaturated	0.39	0.17	0.33
AD Leo ⁽³⁾	M3	0.42	0.38	2.24	3540	0.05	180	Saturated	0.05	0.15	0.29
EQ Peg A ⁽³⁾	M3.5	0.39	0.35	1.06	3530	0.02	480	Saturated	0.02	0.14	0.26
EV Lac ⁽³⁾	M3.5	0.32	0.30	4.4	3480	0.07	490	Saturated	0.08	0.11	0.22
V374 Peg ⁽³⁾	M4	0.28	0.28	0.45	3410	0.006	640	Saturated	0.007	0.10	0.20
EQ Peg B ⁽³⁾	M4.5	0.25	0.25	0.4	3340	0.005	450	Saturated	0.006	0.09	0.17
GJ 1156 ⁽⁴⁾	M5	0.14	0.16	0.49	3160	0.005	100	Saturated	0.004	0.05	0.10
GJ 1245 B ⁽⁴⁾	M5.5	0.12	0.14	6.87 ⁽⁸⁾	3030	–	60	Saturated	0.006	0.04	0.08
WX Uma ⁽⁴⁾	M6	0.1	0.12	0.78	2770	0.008	1060	Saturated	0.006	0.03	0.06
DX Cnc ⁽⁴⁾	M6	0.1	0.11	0.46	2770	0.005	80	Saturated	0.003	0.03	0.05
Kepler-22 ⁽⁹⁾	G5	0.97	0.98	25.6	5518	–	–	Unsaturated	2.08	0.86	1.53
Kepler-1185 ⁽⁹⁾	–	0.96	0.87	12.7	5622	–	–	Unsaturated	0.78	0.79	1.40
Kepler-62 ⁽⁹⁾	K2V	0.69	0.63	36.0	4869	–	–	Unsaturated	1.34	0.45	0.81
K2-3 ⁽⁹⁾	M0V	0.61	0.55	10.1	3951	–	–	Unsaturated	0.34	0.27	0.51
Kepler-442 ⁽⁹⁾	–	0.61	0.60	48.7	4402	–	–	Unsaturated	1.60	0.35	0.66
Kepler-1229 ⁽⁹⁾	–	0.54	0.51	17.7	3784	–	–	Unsaturated	0.52	0.23	0.43
Kepler-186 ⁽⁹⁾	M1V	0.48	0.47	34.3	3788	–	–	Unsaturated	0.90	0.21	0.40
GJ 581 ⁽⁹⁾	M2.5V	0.31	0.30	132.5	3498	–	–	Unsaturated	2.36	0.11	0.22
Wolf 1061 ⁽⁹⁾	M3V	0.25	0.31	119.3	3342	–	–	Unsaturated	1.71	0.11	0.21
Kepler-1649 ⁽⁹⁾	M5V	0.22	0.25	57.5	3240	–	–	Unsaturated	0.74	0.08	0.16
Ross 128 ⁽⁹⁾	M4V	0.17	0.20	0.5	3192	–	–	Saturated	0.01	0.06	0.12
GJ 3323 ⁽⁹⁾	M4V	0.16	0.12	88.5	3159	–	–	Unsaturated	1.03	0.04	0.07
Barnard’s ⁽¹⁰⁾	M3.5V	0.16	0.18	140.0	3278	–	–	Unsaturated	1.44	0.06	0.12
YZ Cet ⁽⁹⁾	M4.5V	0.13	0.17	69.2	3056	–	–	Unsaturated	0.57	0.05	0.10
Prox. Cen ⁽⁵⁾	M5.5	0.12	0.14	83.0	3050	0.65	–	Unsaturated	0.67	0.04	0.08
Teegarden’s ⁽¹¹⁾	M7.0V	0.089	0.107	100	2904	–	–	Unsaturated	0.66	0.03	0.06
Trappist-1 ⁽⁶⁾	M8	0.08	0.117	3.3	2550	0.03	–	Saturated	0.02	0.02	0.05

Notes. The magnetic fields were obtained through Zeeman–Doppler imaging. The rotation regime consists of the two different regimes described by Eq. (4). R_o was calculated with Eqs. (8) and (9). D₂ and D₃ are the boundaries of the HZ for an Earth-like exoplanet orbiting the star.

References. ⁽¹⁾ Matt et al. (2015), ⁽²⁾ Donati et al. (2008), ⁽³⁾ Morin et al. (2008), ⁽⁴⁾ Morin et al. (2010), ⁽⁵⁾ Anglada-Escudé et al. (2016), ⁽⁶⁾ Gillon et al. (2017), ⁽⁷⁾ Reiners et al. (2018), ⁽⁸⁾ Newton et al. (2016), ⁽⁹⁾ http://exoplanet.eu/ ⁽¹⁰⁾ Ribas et al. (2018), ⁽¹¹⁾ Zechmeister et al. (2019).

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