Radiation hydrodynamical simulations of eruptive mass loss from progenitors of Type Ibn/IIn supernovae

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Table 1

Properties of SNe progenitors.

Model	M_ZAMS	Z	R	T_eff	M_He core	M_H env	E_outer^(a)	Time to CC	Burning stage	SN type^(b)
RSG1	11M_⊙	0.02	730 R_⊙	3400 K	3.9 M_⊙	6.1 M_⊙	− 2.2 × 10⁴⁷ erg	10 yr	Ne burning	IIn
RSG2	20 M_⊙	0.02	1085 R_⊙	3500 K	6.3 M_⊙	12.7 M_⊙	− 4.7 × 10⁴⁷ erg	0.8 yr	Ne burning	IIn
BSG	15 M_⊙	2 × 10⁻⁴	58 R_⊙	11000 K	3.7 M_⊙	10.3 M_⊙	− 1.9 × 10⁴⁹ erg	8 yr	Ne burning	IIn
YSG	50 M_⊙	0.01	1380 R_⊙	4700 K	20.6 M_⊙	0.5 M_⊙	− 3.1 × 10⁴⁶ erg	10 yr	C burning	IIn
WR1	50 M_⊙	0.01	0.7 R_⊙	220000 K	19.8 M_⊙	−^(c)	− 5.3 × 10⁵⁰ erg	0.5 yr	C burning	Ibn
WR2	50 M_⊙	0.01	0.6 R_⊙	240000 K	19.8 M_⊙	−^(c)	− 6.0 × 10⁵⁰ erg	15 day	C burning	Ibn

Notes. ^(a) Total energy of Hydrogen-rich envelope (Helium envelope for models WR). ^(b)Type of expected SN. ^(c)Models WR completely lose Hydrogen-rich envelope.

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