第一部分：脈衝星伽瑪射線與X射線輻射之間的統計關係

為了提供關於脈衝星高能輻射所涉及物理機制的觀測線索，我們研究了伽瑪射線光度與X射線光譜性質之間的相關性。我們發現，脈衝星的伽瑪射線光度與非熱X射線輻射的光度有明顯的正相關，並與其光子指數呈反相關。具有與不具有熱輻射的脈衝星在這些關係中似乎表現出不同的依賴性，這可能暗示著兩種類型脈衝星的存在。

第二部分：研究第谷超新星遺跡中的磁擾動本質

超新星遺跡（SNRs）被廣泛認為是銀河宇宙線加速的主要來源，粒子在SNR的激波前緣透過擴散性激波加速（DSA）機制獲得能量，藉由反覆穿越激波而加速。磁擾動在將這些粒子反射來回的過程中扮演關鍵角色，因此研究磁擾動對理解加速過程至關重要。在本研究中，我們應用了二點相關函數法，從第谷超新星遺跡的非熱X射線輻射影像中導出磁能譜。此影像是使用基於卜瓦松模型的廣義形態成分分析（pGMCA）獲得的。所得頻譜中觀察到的擾動長度尺度比Shimoda等人（2018）以無線電觀測導出的第谷擾動尺度更短。此外，我們也利用整個第谷所測得的X射線邊緣厚度作為磁場強度的指標，來估算磁能譜。由此方法推導出的擾動尺度與非熱X射線輻射分析所得結果一致。

Part 1: Statistical relationship between gamma-ray and X-ray emissions from pulsars
Correlations between gamma-ray luminosity and X-ray spectral properties of pulsars are investigated in order to provide observatinal hints on physics involved in pulsars’ high-energy emissions. We found that pulsars gamma-ray luminosity
clearly correlates with the luminosity of non-thermal X-ray emission and anti-correlates with its photon index. Pulsars with and without detected thermal emissions seem to show different dependences in those relations, suggesting possible existence of two different kinds of pulsars.
Part 2: Investigating the nature of magnetic turbulence in Tycho’s
SNR
Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic ray acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration (DSA) mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal
X-ray flux image of Tycho's SNR. This image was obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale observed in the resulting spectrum is shorter than the turbulence scale derived from radio observations of Tycho's SNR (Shimoda et al. 2018). Additionally,
we use the X-ray rim thickness measured across Tycho which is an indicator of magnetic field strength to estimate the magnetic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.