核心塌縮超新星之爆炸前恆星(CCSN progenitor)的詳細結構，對於研究超新
星爆炸機制以及其發出的多信使訊號，有著極為重要之影響。這篇研究主要探
討恆星旋轉速度對雙星系統的影響，我們選擇30太陽質量的主星以及20太陽質
量的伴星，並使用恆星演化程式MESA進行模擬。我們發現透過雙星間的質量轉
移，在特定初始雙星週期下可產生高速旋轉的超新星爆炸前恆星，但初始週期
與最終旋轉並無線性相關。
我們得出的結果是在相同質量比例的雙心系統下，超新星最終質量、鐵核質
量、緻密性參數(compactness parameter)以及最終旋轉速度根據初始週期可產生
很大的不同。舉例來說，藍超巨星形成的爆炸前恆星與單星系統的爆炸前恆星
相比有著較薄的矽殼以及分布較廣的氧殼。
此外，我們對透過雙星系統產生的高速旋轉爆炸前恆星使用二維自洽核心塌
縮超新星爆炸並包含微中子傳遞進行模擬。我們發現這些雙星系統形成的爆炸
前恆星所產生的微中子和重力波訊號也有著很大的差異，較大的緻密性參數會
形成較強的重力波訊號。再者，緊密的內核會導致更強的質量吸積並釋放更強
的微中子訊號。

The detailed structure of core-collapse supernova progenitors is
crucial for studying supernova explosion engines and the corresponding multimessenger signals. In this thesis, we investigate the influence of stellar rotation on binary systems consisting of a 30 solar mass donor star and a 20 solar mass accretor using the MESA stellar evolution code. We find that through mass transfer in binary systems, fast-rotating red-supergiant and blue-supergiant progenitors can be formed within a certain range of initial orbital periods, albeit the correlation is not linear.
We find that even with the same initial mass ratio of the binary system, the resulting final mass of the collapsars, the iron core mass, the compactness parameters, and the final rotational rates can vary widely, depending on the initial orbital periods. For instance, the blue-supergiant progenitors have a thinner Si-shell and a wider O-shell compared to those in single-star systems.
In addition, we conduct two-dimensional self-consistent core-collapse supernova simulations with neutrino transport for these rotating progenitors from binary stellar evolution. We find that the neutrino and gravitational-wave signatures of these binary progenitors could exhibit significant variations. Progenitors with larger compactness parameters produce more massive proto-neutron stars, have higher mass-accretion rates, and therefore emit brighter neutrino luminosity and louder gravitational emissions.

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