Feedback from multiple supernova explosions inside a wind-blown bubble
✍ Scribed by Hyunjin Cho; Hyesung Kang
- Publisher
- Elsevier Science
- Year
- 2008
- Tongue
- English
- Weight
- 758 KB
- Volume
- 13
- Category
- Article
- ISSN
- 1384-1076
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✦ Synopsis
We study the evolution of multiple supernova (SN) explosions inside a pre-exiting cavity blown by winds from massive progenitor stars. Hydrodynamic simulations in one-dimensional spherical geometry, including radiative cooling and thermal conduction, are carried out to follow first the development of the wind-blown bubble during the main sequence and then the evolution of the SN-driven bubble. We find the size and mass of the SN-driven bubble shell depend on the structure of the pre-existing wind bubble as well as the SN explosion energy E SN (=N SN 10 51 ergs). The hot cavity inside the bubble is 2-3 times bigger in volume and hotter than that of a bubble created by SNe exploded in a uniform interstellar medium (ISM). For an association with 10 massive stars in the average ISM, the SN-driven shell has an outer radius of R ss % ð85 pcÞN 0:1 SN and a mass of M ss % ð10 4:8 M ÞN 0:3 SN at 10 6 years after the explosion. By that time most of the explosion energy is lost via radiative cooling, while [10% remains as kinetic energy and $10% as thermal energy. We also calculate the total integrated spectrum of diffuse radiation emitted by the shock-heated gas of the SN bubble. Total number of H Lymann-limit photons scales roughly as U 13.6 % 10 61 N SN and those photons carry away 20-55% of the explosion energy. For the models with 0.1 solar metalicity, the radiative energy loss is smaller and the fraction of non-ionizing photons is larger, compared to those with solar metalicity. We conclude the photoionization/heating by diffuse radiation is the most dominant form of feedback from SN explosions into the surrounding medium.