Pulsations of red supergiant pair-instability supernova progenitors leading to extreme mass loss

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Table 1

Properties of our stellar models.

ε	M _ini	M _fin			R _fin	T _eff,fin	L _fin
	(M_⊙)	(M_⊙)	(M_⊙)	(M_⊙)	(10³R_⊙)	(10³ K)	(10⁶L_⊙)

	150	147	73	74	3.14	4.63	4.09
0^a	200	190	87	103	3.78	4.71	6.31
	250	236	111	126	4.16	4.72	7.73

	150	104	30	74	2.70	4.99	4.13
0.1^b	200	136	32	104	3.44	4.94	6.34
	250	164	40	124	3.81	4.94	7.82

	150	104	31	73	2.75	4.97	4.13
0.3^b	200	129	25	104	3.52	4.90	6.40
	250	170	45	125	3.90	4.89	7.78

Notes. Columns: conversion efficiency, initial mass, final mass, final hydrogen-rich envelope mass, final helium core mass, final radius, final effective temperature, and final luminosity.

^(a)

Models with radiation-driven wind only.

^(b)

Models in which pulsation-driven mass loss with the indicated value of ε is considered.

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