Pre-supernova outbursts via wave heating in massive stars - I. Red supergiants

被引:171
作者
Fuller, Jim [1 ,2 ]
机构
[1] CALTECH, TAPIR, Walter Burke Inst Theoret Phys, Mailcode 350-17, Pasadena, CA 91125 USA
[2] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Kohn Hall, Santa Barbara, CA 93106 USA
基金
美国国家科学基金会;
关键词
waves; stars: evolution; stars: massive; stars: mass-loss; supergiants; supernovae: general; STELLAR ASTROPHYSICS MESA; DENSE CIRCUMSTELLAR MATERIAL; ANGULAR-MOMENTUM TRANSPORT; CORE-COLLAPSE SUPERNOVAE; INTERNAL GRAVITY-WAVES; II SUPERNOVAE; LIGHT CURVES; SN; 2009IP; TURBULENT CONVECTION; MAGNETIC-FIELDS;
D O I
10.1093/mnras/stx1314
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Early observations of supernovae (SNe) indicate that enhanced mass-loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical 15 M-circle dot red supergiant SN progenitors. Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry similar to 10(7) L-circle dot of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. The waves damp via shocks and radiative diffusion at the base of the hydrogen envelope, which heats up fast enough to launch a pressure wave into the overlying envelope that steepens into a weak shock near the stellar surface, causing a mild stellar outburst and ejecting a small (less than or similar to 1 M-circle dot) amount of mass at low speed (less than or similar to 50 km s(-1)) roughly one year before the SN. The wave heating inflates the stellar envelope but does not completely unbind it, producing a non-hydrostatic pre-SN envelope density structure different from prior expectations. In our models, wave heating is unlikely to lead to luminous Type IIn SNe, but it may contribute to flash-ionized SNe and some of the diversity seen in II-P/II-L SNe.
引用
收藏
页码:1642 / 1656
页数:15
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