本文關(guān)鍵詞：伽馬暴X射線余輝研究與Fermi LAT未證認(rèn)源的統(tǒng)計(jì)分類　出處：《華中師范大學(xué)》2013年博士論文　論文類型：學(xué)位論文

  更多相關(guān)文章： 伽馬射線暴 星風(fēng) 費(fèi)米伽馬射線源

【摘要】：本文的研究?jī)?nèi)容屬于伽馬射線天文學(xué)的范疇。近年來,隨著伽馬射線空間和地面望遠(yuǎn)鏡的更新升級(jí)以及與其它多波段觀測(cè)的緊密結(jié)合,伽馬射線天文學(xué)取得了極大發(fā)展,其研究領(lǐng)域也被大大拓寬。本文的研究主要包括兩個(gè)部分,一是對(duì)伽馬暴X射線余輝的理論研究,二是對(duì)一些未證認(rèn)的Fermi伽馬射線穩(wěn)態(tài)源的統(tǒng)計(jì)分類。 伽馬暴是伽馬射線天文學(xué)研究的主要對(duì)象之一。自1967年發(fā)現(xiàn)至今,經(jīng)過數(shù)十年的研究人們對(duì)伽馬暴的認(rèn)識(shí)已較為深入。但是,伽馬暴的中心能源問題仍然是一個(gè)未解之謎。近年來,Swift衛(wèi)星觀測(cè)到伽馬暴X射線余輝新特征(主要包括早期余輝的緩慢衰減和X射線耀發(fā)現(xiàn)象)為人們了解伽馬暴的中心能源機(jī)制提供了重要線索。在標(biāo)準(zhǔn)外激波余輝模型下,這些X射線余輝新特征無法得到有效解釋。因此,本文第一個(gè)研究工作將主要針對(duì)這一問題。為了有效解釋X射線余輝的早期變平現(xiàn)象,一般認(rèn)為伽馬暴的中心致密天體很可能是一顆高速旋轉(zhuǎn)的磁星,它可能在很長(zhǎng)一段時(shí)間內(nèi)為外激波注入能量。但是,本文認(rèn)為,磁星能量的釋放實(shí)際上很可能是通過攜帶了大量正負(fù)電子對(duì)的Poynting流的形式。而由于磁重聯(lián)的原因,Poynting流有可能在追上伽馬暴外激波之前就已經(jīng)轉(zhuǎn)化為相對(duì)論性的正負(fù)電子對(duì)星風(fēng)。因此,星風(fēng)與伽馬暴拋射物質(zhì)相互作用產(chǎn)生的終止激波將直接導(dǎo)致很強(qiáng)的X射線余輝輻射,甚至完全超過伽馬暴外激波的輻射(即使有部分能量注入)。我們的數(shù)值計(jì)算結(jié)果顯示,在星風(fēng)磁化率滿足一定條件的時(shí)候,這種情況是完全可能發(fā)生的。因此,我們提出某些觀測(cè)到的伽馬暴X射線余輝有可能直接來源于磁星星風(fēng)終止激波的輻射,而不是傳統(tǒng)的外激波。一定程度上講,磁星星風(fēng)終止激波輻射可被認(rèn)為是一種內(nèi)耗散起源的余輝輻射機(jī)制。 2008年以來,Fermi衛(wèi)星的LAT探測(cè)器觀測(cè)到了大量的穩(wěn)態(tài)伽馬射線源,這些源的屬性是人們所關(guān)心的一個(gè)重要問題。Fermi合作組的證認(rèn)結(jié)果顯示,2年時(shí)間內(nèi)觀測(cè)到的1873個(gè)源中,有127個(gè)源的性質(zhì)被完全確定,另有1171個(gè)源和候選對(duì)應(yīng)體成協(xié),但是剩下575個(gè)源未找到候選對(duì)應(yīng)體。本文第二個(gè)工作就是對(duì)這575個(gè)未證認(rèn)的源進(jìn)行統(tǒng)計(jì)分類研究。和具體去找候選對(duì)應(yīng)體的證認(rèn)方法不同,我們這里并不是對(duì)單個(gè)源進(jìn)行分析,而是選取反映未證認(rèn)源的物理性質(zhì)的觀測(cè)量進(jìn)行統(tǒng)計(jì)分析,其中包含空間分布、譜指數(shù)和光變指數(shù)。通過和已證認(rèn)的源進(jìn)行比較研究,討論這575個(gè)未證認(rèn)源的可能候選對(duì)應(yīng)體。我們的統(tǒng)計(jì)分析結(jié)果顯示,這些未證認(rèn)源可能主要包括：超新星遺跡/脈沖星風(fēng)星云,蝎虎座BL天體,射電平譜類星體和其他類型的活動(dòng)星系,它們的比例分別為25%,29%,41%和5%。
[Abstract]:In recent years, with the updating and upgrading of gamma ray space and ground telescopes and the close integration with other multi-band observations, the research contents of this paper belong to the field of gamma ray astronomy. Gamma-ray astronomy has made great progress, and its research field has been greatly broadened. This paper mainly includes two parts, one is the theoretical study of X-ray afterglow of gamma-ray storms. The second is the statistical classification of some unauthenticated Fermi gamma ray steady-state sources. Gamma-ray storm is one of the main objects of gamma ray astronomy. Since its discovery in 1967, after decades of research people have been more in-depth understanding of gamma storms. The central energy problem of gamma storms remains an unsolved mystery in recent years. New characteristics of X-ray afterglow of gamma-ray storms observed by Swift satellite (mainly including slow decay of early afterglow and X-ray luminescence). It provides an important clue for people to understand the central energy mechanism of gamma storms, under the standard external shock afterglow model. These new characteristics of X-ray afterglow can not be effectively explained. Therefore, the first study in this paper will focus on this problem, in order to effectively explain the early flattening phenomenon of X-ray afterglow. It is generally believed that the central dense object of the gamma storm is probably a high speed rotating magnetic star which may inject energy into the external shock waves for a long time. The release of energy from magnetic stars may in fact be in the form of a Poynting stream that carries a large number of positron and negative electron pairs, and due to magnetic reconnection. The Poynting current may have been transformed into relativistic positron to star winds before catching up with the external shock waves of gamma storms. The terminating shock produced by the interaction between the starwind and the gamma ray ejection will directly lead to strong X-ray afterglow radiation. Even beyond the radiation of the external shock wave (even if there is partial energy injection), our numerical results show that when the susceptibility of the star wind meets certain conditions. Therefore, we suggest that some observed X-ray afterglow of gamma storms may be directly derived from the radiation of the magnetic star wind terminating shock waves. To some extent, the termination of shock wave radiation by magnetic star wind can be considered as a mechanism of afterglow radiation from the origin of internal dissipation. Since 2008, a large number of steady state gamma ray sources have been observed by the LAT detector of the Fermi satellite. The attributes of these sources are an important issue of concern. The results of the Fermi team's identification show that 127 of the 1 873 sources observed in the 2-year period have been fully identified. In addition, there are 1171 source and candidate counterpart consortia. However, the remaining 575 sources have not found candidate correspondence. The second work of this paper is to study the 575 unauthenticated sources by statistical classification, which is different from the method of identifying candidates. We do not analyze a single source here, but select observations reflecting the physical properties of unauthenticated sources for statistical analysis, including spatial distribution. Spectral index and photovariation index. By comparing with the identified sources, we discuss the possible candidates for these 575 unauthenticated sources. Our statistical analysis results show that: 1. These unidentified sources may include: supernova remnants / pulsar winds nebulae, BL objects in the constellation Scorpius, emissive spectrum quasars and other types of active galaxies, which account for 25% or 29% respectively. 41% and 5.
【學(xué)位授予單位】：華中師范大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2013
【分類號(hào)】：P172.3

【共引文獻(xiàn)】

相關(guān)期刊論文 前10條

1 ;A fast onboard star-extraction algorithm optimized for the SVOM Visible Telescope[J];Science China(Physics,Mechanics & Astronomy);2010年S1期

2 ;Spectral states and state preference of galactic X-ray binaries[J];Science China(Physics,Mechanics & Astronomy);2010年S1期

3 馬宇劏,李惕碚;X和γ天文譜線觀測(cè)結(jié)果的可靠性[J];Chinese Journal of Astronomy and Astrophysics;1984年01期

4 ;Gamma-Ray Bursts in the Swift Era[J];Chinese Journal of Astronomy and Astrophysics;2007年01期

5 ;Swift/BAT Observations of X-Ray Flashes[J];Chinese Journal of Astronomy and Astrophysics;2008年03期

6 ;A GRB Follow-up System at the Xinglong Observatory and Detection of the High-Redshift GRB 060927[J];Chinese Journal of Astronomy and Astrophysics;2008年06期

7 Edward L.Chupp;James M.Ryan;;High energy neutron and pion-decay gamma-ray emissions from solar flares[J];Research in Astronomy and Astrophysics;2009年01期

8 ;Comparison between Swift and pre-Swift gamma-ray bursts[J];Research in Astronomy and Astrophysics;2009年06期

9 Chetana Jain;Biswajit Paul;Anjan Dutta;;Orbital X-ray modulation study of three supergiant HMXBs[J];Research in Astronomy and Astrophysics;2009年12期

10 ;Not enough evidence to support the correlation between gamma-ray bursts and foreground galaxy clusters in the Swift Era[J];Research in Astronomy and Astrophysics;2010年06期

相關(guān)博士學(xué)位論文 前7條

1 操小鳳;X射線雙星快速光變研究與伽瑪暴的光度和紅移統(tǒng)計(jì)[D];華中師范大學(xué);2012年

2 賈蘭偉;伽馬暴脈沖光變曲線與能譜的關(guān)系[D];中國(guó)科學(xué)院研究生院（云南天文臺(tái)）;2008年

3 張富文;伽瑪暴脈沖時(shí)變特征及其對(duì)能量的依賴[D];中國(guó)科學(xué)院研究生院（云南天文臺(tái)）;2008年

4 沈宗俊;直接解調(diào)方法的研究與應(yīng)用[D];清華大學(xué);2007年

5 俞云偉;Swift時(shí)代伽瑪射線暴及其余輝的多波段研究[D];華中師范大學(xué);2009年

6 呂靜;伽瑪暴火球輻射光度與初始洛倫茲因子相關(guān)性及物理意義[D];華中科技大學(xué);2013年

7 侯書進(jìn);伽瑪射線暴的中心引擎及能譜的研究[D];廈門大學(xué);2014年

相關(guān)碩士學(xué)位論文 前1條

1 馮思軼;Fermi時(shí)代伽瑪射線暴相關(guān)研究[D];南京大學(xué);2011年

，

本文編號(hào)：1411246