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

Takashi J. Moriya; Norbert Langer

doi:10.1051/0004-6361/201424957

Home

All issues

Volume 573 (January 2015)

A&A, 573 (2015) A18

Full HTML

Free Access

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.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.