Determining the mass loss limit for close-in exoplanets: what can we learn from transit observations?

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Table 3:

The mass loss from ``Hot Jupiters'' and ``Hot Neptunes'' with low and high densities at four different orbital distances around a G star ( $1~M_{\rm Sun}$ ) and a K star ( $0.8~M_{\rm Sun}$ ).
	$\frac{M_{{\rm pl}}}{M_{{\rm Jup}}}$	$\frac{\rho_{\rm pl}}{\rho_{\rm Jup}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}^{10\%}}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}^{25\%}}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}^{60\%}}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}^{100\%}}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}}^{10 \%-60\%}}$	$\frac{\Delta M_{{\rm pl}}}{M_{{\rm pl}}^{10 \%-25\%}}$	$\zeta$
0.01 AU, G star						Mass loss [%]
	1	1.24	2.95	7.74	21.59	52.42	2.95	2.95	8.24
	0.5	1.24	6.09	17.12	-	-	6.09	6.09	8.24
	0.054	1.61	38.17	-	-	-	38.17	38.17	5.90
	1	0.4	77.43	-	-	-	77.43	77.43	>100
	0.5	0.4	-	-	-	-	-	-	>100
	0.054	0.4	-	-	-	-	-	-	>100
0.017 AU, G star
	1	1.24	0.38	0.94	2.28	3.84	0.45	0.40	2.40
	0.5	1.24	0.75	1.90	4.64	7.90	0.90	0.80	2.40
	0.054	1.61	4.40	11.54	32.03	87.08	5.21	4.64	2.17
	1	0.4	2.08	5.34	13.80	25.71	2.46	2.19	4.82
	0.5	0.4	4.23	11.24	33.23	-	5.02	4.47	4.82
	0.054	0.4	51.47	-	-	-	-	56.79	4.82
0.020 AU, G star
	1	1.24	0.23	0.59	1.42	2.37	0.31	0.26	2.02
	0.5	1.24	0.47	1.18	2.86	4.82	0.62	0.52	2.02
	0.054	1.61	2.79	7.16	18.48	34.41	3.62	3.04	1.87
	1	0.4	1.11	2.80	6.93	12.02	1.45	1.21	3.32
	0.5	0.4	2.23	5.73	14.74	27.26	2.93	2.44	3.32
	0.054	0.4	20.29	-	-	-	27.06	22.23	3.32
0.025 AU, G star
	1	1.24	0.13	0.32	0.78	1.30	0.20	0.15	1.69
	0.5	1.24	0.26	0.65	1.56	2.62	0.40	0.30	1.69
	0.054	1.61	1.56	3.96	9.84	17.16	2.34	1.79	1.60
	1	0.4	0.53	1.34	3.26	5.52	0.82	0.62	2.37
	0.5	0.4	1.07	2.71	6.68	11.51	1.64	1.24	2.37
	0.054	0.4	9.08	25.53	-	-	13.71	10.44	2.37
0.01 AU, K star						Mass loss [%]
	1	1.24	0.88	2.23	5.51	9.54	1.01	0.92	6.16
	0.5	1.24	1.77	4.55	11.69	21.46	2.03	1.85	6.16
	0.054	1.61	9.17	26.80	-	-	10.41	9.54	4.71
	1	0.4	76.58	87.37	-	-	80.24	77.83	247
	0.5	0.4	84.14	-	-	-	87.83	85.37	247
	0.054	0.4	-	-	-	-	-	-	247
0.017 AU, K star
	1	1.24	0.13	0.33	0.80	1.34	0.22	0.16	2.20
	0.5	1.24	0.27	0.67	1.61	2.71	0.43	0.32	2.20
	0.054	1.61	1.55	3.93	9.80	17.15	2.44	1.81	2.02
	1	0.4	0.67	1.70	4.15	7.09	1.07	0.79	3.99
	0.5	0.4	1.35	3.44	8.61	15.16	2.16	1.59	3.99
	0.054	0.4	11.47	35.21	-	-	18.23	13.41	3.99
0.020 AU, K star
	1	1.24	0.09	0.21	0.51	0.85	0.16	0.11	1.89
	0.5	1.24	0.17	0.42	1.02	1.71	0.31	0.21	1.89
	0.054	1.61	1.00	2.53	6.21	10.63	1.78	1.23	1.77
	1	0.4	0.38	0.95	2.30	3.87	0.68	0.47	2.92
	0.5	0.4	0.76	1.91	4.67	7.98	1.37	0.94	2.92
	0.054	0.4	6.24	16.87	56.87	-	11.07	7.65	2.92
0.025 AU, K star
	1	1.24	0.05	0.12	0.29	0.48	0.10	0.06	1.62
	0.5	1.24	0.10	0.24	0.57	0.95	0.21	0.13	1.62
	0.054	1.61	0.57	1.44	3.49	5.90	1.20	0.76	1.54
	1	0.4	0.19	0.48	1.15	1.92	0.41	0.26	2.18
	0.5	0.4	0.38	0.95	2.31	3.88	0.82	0.51	2.18
	0.054	0.4	3.10	8.00	20.99	40.46	6.52	4.11	2.18

The superscripts 10%-25% and 10%-60% correspond to a time depended $\eta$ which has a low heating efficiency of 10% if the EUV flux is $\geq$ 10⁴ erg cm^-2 s^-1 and 25% and 60% for EUV flux values <10⁴ erg cm^-2 s^-1 (Murray-Clay et al. 2009).

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