A POSSIBLE LOW-MASS TYPE-IA SUPERNOVA

被引:66
作者
RUIZLAPUENTE, P
JEFFERY, DJ
CHALLIS, PM
FILIPPENKO, AV
KIRSHNER, RP
HO, LC
SCHMIDT, BP
SANCHEZ, F
CANAL, R
机构
[1] UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720
[2] UNIV CALIF BERKELEY,CTR PARTICLE ASTROPHYS,BERKELEY,CA 94720
[3] INST ASTROFIS CANARIAS,LA LAGUNA,SPAIN
[4] UNIV BARCELONA,DEPT ASTRON METEOROL,BARCELONA 7,SPAIN
关键词
D O I
10.1038/365728a0
中图分类号
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号
07 ; 0710 ; 09 ;
摘要
IN the standard model for type Ia supernovae1, a massive white dwarf in a binary system accretes matter from the companion star until it reaches the Chandrasekhar mass (the stability limit for degenerate-electron stars, corresponding to approximately 1.4 solar masses), and a runaway thermonuclear explosion ensues. In a popular variant of this model2, the companion star is also a white dwarf. But regardless of the nature of the companion, the invariance of the Chandrasekhar mass implies that all type Ia supernovae will be similar in luminosity3, making them ideal 'standard candles' for determining extragalactic distances, and hence the Hubble constant. In the context of the standard model, the recent type Ia supernova SN1991bg is hard to explain: it was underluminous at all observed epochs, leading to suggestions4,5 that the mass of the progenitor was unusually low. Here we present model calculations, based on more recent spectra, which point to a mass of the white dwarf of approximately 0.7 solar masses-well below the Chandrasekhar mass. Moreover, the late spectrum shows evidence of emission from low-velocity hydrogen gas, which might originate in material stripped from an extended, hydrogen-rich companion star. If our interpretation is correct, SN1991bg challenges both the double white-dwarf scenario, and the standard model for type Ia supernovae.
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页码:728 / 730
页数:3
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