研究生: |
嚴子晴 Yen, Tzu-Ching |
---|---|
論文名稱: |
毫秒脈衝星PSR J2339-0533於X光波段之研究 X-Ray Studies of the Redback Millisecond Pulsar PSR J2339-0533 |
指導教授: |
江國興
Kong, Albert K. H. |
口試委員: |
張祥光
陳林文 |
學位類別: |
碩士 Master |
系所名稱: |
理學院 - 天文研究所 Institute of Astronomy |
論文出版年: | 2016 |
畢業學年度: | 104 |
語文別: | 英文 |
論文頁數: | 58 |
中文關鍵詞: | 毫秒脈衝星 、X光天文學 |
外文關鍵詞: | Millisecond Pulsar, X-ray Astronomy |
相關次數: | 點閱:1 下載:0 |
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我們用XMM牛頓太空望遠鏡觀測毫秒脈衝星PSR J2339-0533。在X光波段,我們發現光度的變化與軌道週期有關連。其X光有一個與軌道週期(4.6小時)相符的週期,具有兩個高峰和兩個凹陷,其中凹陷處光譜明顯能量較低。我們認為X射線可以分解成一個能量較高的變化分量,加上一個能量較低的穩定分量。
在0.5-8.0千電子伏能量範圍的解析光譜分析證實PSR J2339-0533在不同軌道相位發射的熱X射線成分小於30%,符合先前的研究結果。
我們的結論是多數的X射線來自一個冪律分量,並且可能來自於脈衝風和輔助星吹散物質之間的界面。
我們在各個不同能量X射線頻帶都沒有發現毫秒的脈動,也沒有發現和伽瑪射線/無線電相合的脈動。
我們也探討了雙星配置的幾何形狀。我們嘗試以多普勒升壓模式解釋光變曲線的形狀,得出的結論是,衝擊可能位於附近的內拉格朗日點(L1)。通過研究該系統的熱力學,我們推斷,在衝擊前的震盪有利於發射磁能為主的脈衝星風。我們最後並且討論在觀測時,吸積盤是否可能存在。
We report on the XMM-Newton observations of the redback pulsar PSR J2339−0533. For the X-ray emission we found confirmation for a binary-phase dependence. The emission appears to be orbitally modulated at the 4.6-hour orbital period, with two peaks and two dips, where the dips concurred by a softening in the spectrum. We suggest that the X-rays could be decomposed into a hard variable component plus a soft-steady component.
The broad band (0.5 − 8.0 keV) binary-phase resolved spectral analysis discloses a thermal X-ray component (< 30%) of the emission from PSR J2339−0533 at various orbital phases, confirming the results from previous studies.
We conclude that the majority of X-ray emissions are from a power-law component and can be attributed to intra-binary shock emission from the interface between pulsar wind and the ablated material from the secondary star.
We also report non-detection of pulsation on various X-ray energy bands; we did not find any pulsation at the gamma-ray/radio timing solution.
The geometry of the binary configuration is explored in our study. We explain the shape of the orbitally phase-folded lightcurve with the Doppler boosting model, concluding that the shock is possibly located near the inner Lagrangian point (L1). By exploring the energetics of the system, we infer that the shock emission at the shock front favors a magnetically-dominated (σ ≫ 1) pulsar wind. Lastly we discuss the possibility of the presence of an accretion disk on the time of observation.
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