探討中子超流體在脈衝星上所扮演的角色

Investigating the role played by neutron superfluid for pulsars

康潤(Ren Kang)

指導教授 ： 黃偉彥

國立臺灣大學/理學院/物理研究所/碩士(2008年)

https://doi.org/10.6342/NTU.2008.10220

摘要

真空磁偶極輻射模型合理的解釋了脈衝星本身輻射能量的來源，這個模型的特點在於利用經典電動力學理論來描述脈衝星的輻射是由中子星的轉動動能來提供，但是脈衝星的制動過程則還無法獲得一致的見解，特別是年輕脈衝星的制動指數總小於理論值，本論文把焦點放在半徑與轉動慣量的演化上，基本上聯繫了脈衝星的週期躍變現象及星體內部中子超流體的物理行為。

關鍵字

制動指數 ； 週期躍變 ； 中子超流體 ； 中子星 ； 脈衝星

並列摘要

The magnetic dipole radiation model application of the classical electrodynamics theory to the description of how the pulsar's radiation is powered by the neutron star's rotational energy. But there has not been any unanimous explanation for pulsar braking process, especially explanation for why the braking index for a young pulsar is always less than the theoretical index. In this thesis, we only focus on the evolution of radius and moment of inertia. Basically, it has built a connection between the glitch phenomenon of pulsars and the physical behaviors of neutron superfluid.

並列關鍵字

braking index ； glitch ； neutron superfluid ； neutron star ； pulsar

參考文獻

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Camilo, F., V. M. Kaspi, et al. (2000). "DISCOVERY OF TWO HIGH MAGNETIC FIELD RADIO PULSARS." The Astrophysical Journal 541: 367.

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