Table 4: Interior surviving planets at 170 000 years compared with the four currently known "hot Neptune'' systems. Data include the closest giant planet.
Scenario ID Mass ( ${M}_\oplus$ ) a (AU) e Resonances

I OLI8 15.65 0.055 0.052 None

GIA1 160.3 0.100 0.003

II OLI9 2.33 0.047 0.148 5:4 with ICE9, 5:3 with ICE1

ICE9 6.69 0.054 0.071 4:3 with ICE1

ICE1 5.58 0.065 0.022

GIA1 160.9 0.100 0.005

III ICE1 4.89 0.023 0.110 None

GIA1 160.3 0.100 0.001

IV OLI28 2.86 0.036 0.035 None

GIA1 159.8 0.100 0.002

GJ 436 b 21.3 $\sin i$ 0.028 0.12 None

55 Cancri e 14.3 $\sin i$ 0.038 0.174 None

b 267.3 $\sin i$ 0.11 0.02

$\mu$ Arae d 13.4 $\sin i$ 0.09 0.0 None

b 541.0 $\sin i$ 1.5 0.31

GJ 876 d 5.89 $\sin i$ 0.021 0.0 None

c 177.9 $\sin i$ 0.13 0.27

**Table 4:** Interior surviving planets at 170 000 years compared with the four currently known "hot Neptune'' systems. Data include the closest giant planet.
Scenario	ID	Mass ( ${M}_\oplus$ )	a (AU)	e	Resonances
I	OLI8	15.65	0.055	0.052	None
	GIA1	160.3	0.100	0.003
II	OLI9	2.33	0.047	0.148	5:4 with ICE9, 5:3 with ICE1
	ICE9	6.69	0.054	0.071	4:3 with ICE1
	ICE1	5.58	0.065	0.022
	GIA1	160.9	0.100	0.005
III	ICE1	4.89	0.023	0.110	None
	GIA1	160.3	0.100	0.001
IV	OLI28	2.86	0.036	0.035	None
	GIA1	159.8	0.100	0.002
GJ 436	b	21.3 $\sin i$	0.028	0.12	None
55 Cancri	e	14.3 $\sin i$	0.038	0.174	None
	b	267.3 $\sin i$	0.11	0.02
$\mu$ Arae	d	13.4 $\sin i$	0.09	0.0	None
	b	541.0 $\sin i$	1.5	0.31
GJ 876	d	5.89 $\sin i$	0.021	0.0	None
	c	177.9 $\sin i$	0.13	0.27

Source LaTeX | All tables | In the text

	1 Introduction.
	2 Description of the model
	3 Results
	4 Caveats and future model improvements
	5 Conclusions
	References