本文關(guān)鍵詞： Mrk421 數(shù)據(jù)處理 光變 光變周期 雙黑洞　出處：《山東大學(xué)》2013年碩士論文　論文類型：學(xué)位論文

【摘要】：自20世紀60年代類星體(Quasi-Stellar Objects, QSOs)和blazar天體等活動星系核(Active Galactic Nuclei, AGNs)發(fā)現(xiàn)以來,AGN的研究一直是天體物理學(xué)中最活躍的研究領(lǐng)域之一。AGN的研究,在能量產(chǎn)生、輻射機制和宇宙學(xué)等基本問題上占有重要地位。Blazar天體是AGN中最活躍的子類,具有大幅、快速光變等特征。觀測和研究blazar天體的光變是獲得該類天體有關(guān)特性的一種重要的手段。Mrk421是目前已知的最近的blazar天體之一,由于其同步輻射峰頻高于0.1keV,它被歸類為高峰頻blazar (High Frequency Peaked Blazar. HBL)天體。研究Mrk421的光變特性對(?)blazar等AGN天體的研究及物理模型的建立都具有重要意義。 山東大學(xué)威海天文臺1.0米望遠鏡自2009年起便對Mrk421進行了較為細致的觀測。由于數(shù)據(jù)量大,作者以NASA天文包為基礎(chǔ)編寫了時序測光數(shù)據(jù)的1DL自動處理程序,使得數(shù)據(jù)處理過程自動化程度大大提高,處理的效率得到很大提升。測試表明,該IDL程序的測光結(jié)果與IRAF的測光結(jié)果一致。 作者對山東大學(xué)威海天文臺1.0米望遠鏡Mrk421的R和V波段的觀測數(shù)據(jù)進行了處理,在40個觀測夜中,有39個觀測夜至少有一個波段觀測數(shù)據(jù)點超過了5個。作者使用C檢驗和F檢驗對這39個觀測夜的數(shù)據(jù)進行了微光變的分析,未探測到微光變。前人的觀測認為HBL天體與低峰頻blazar (Low Frequency Peaked Blazar, LBL)天體相比,有著更少的光變,作者的結(jié)果支持這種觀點。HBL天體中有著比LBL天體更強的磁場(Romeroet a1.,1999)可能是該現(xiàn)象產(chǎn)生的原因。 作者從文獻中搜集了Mrk421B和V波段的歷史數(shù)據(jù),并匯集了美國變星觀測者協(xié)會(AAVSO)數(shù)據(jù)庫及美國Arizona大學(xué)Steward天文臺對Mrk421的觀測數(shù)據(jù),與山東大學(xué)威海天文臺觀測的V波段的數(shù)據(jù)一起,得到了Mrk421的長期光變曲線。作者使用離散相關(guān)函數(shù)和結(jié)構(gòu)函數(shù)兩種方法對Mrk421的光變曲線進行了周期分析,結(jié)果顯示Mrk421很可能存在一個1.37年的光變周期。這可能暗示著Mrk421-中心存在密近的雙黑洞系統(tǒng),其中主黑洞質(zhì)量為1.66×108M。,次黑洞質(zhì)量為6.96×104M。 作者分析Mrk421的色指數(shù)變化,包括準同時性的V-R色指數(shù)和長期的B-V色指數(shù)。分析發(fā)現(xiàn)在Mrk421處于低態(tài)的情況下,Mrk421表現(xiàn)出“變暗變紅”的現(xiàn)象,這一現(xiàn)象的產(chǎn)生可能是由宿主星系熱輻射的貢獻在目標較暗時所占更大的比重導(dǎo)致的。
[Abstract]:Since the discovery of Quasi-Stellar objects (QSOs) and active Galactic Nuclei (AGNs) in 1960s, the study of AGNs has been one of the most active research fields in astrophysics. The Blazar object is the most active subclass in AGN, and has a large size. The observation and study of the photovariation of blazar objects is an important means of obtaining the properties of these objects. Mrk421 is one of the most recent known blazar objects. Because its peak frequency of synchrotron radiation is higher than 0.1 Kev, it is classified as blazar High Frequency Peaked Blazar.HBL. The study of AGN objects such as blazar and the establishment of physical models are of great significance. The 1.0-meter telescope of Weihai Observatory of Shandong University has made a detailed observation of Mrk421 since 2009. Due to the large amount of data, the author has compiled a 1DL automatic processing program for time series photometric data based on the NASA astronomical package. The automation degree of the data processing process is greatly improved and the processing efficiency is greatly improved. The test results show that the photometric results of the IDL program are consistent with those of the IRAF program. The authors have processed the R and V band observations of the 1.0-meter telescope at Weihai Observatory, Shandong University, in 40 observation nights. In 39 observation nights, at least one band observation data point is more than 5. The authors used C test and F test to analyze the data of these 39 observation nights. No low light change was detected. Previous observations have shown that HBL objects have less light variability than low peak frequency blazar low Frequency Peaked Blazar objects. The author's results support this view. The fact that there is a stronger magnetic field in HBL objects than in LBL objects may be the cause of this phenomenon. The author collected the historical data of Mrk421B and V band from the literature, and compiled the AAVSO database of the American Association of variable Star observers and the Mrk421 observation data of the Steward Observatory of Arizona University in the United States. Along with the data of V band observed by Weihai Observatory of Shandong University, the long term optical variation curve of Mrk421 is obtained. The authors use discrete correlation function and structure function to analyze the optical variation curve of Mrk421 periodically. The results show that there is probably a 1.37 year optical variation period in Mrk421, which may imply that there exists a close double black hole system in the center of Mr k421- in which the mass of the main black hole is 1.66 脳 108M.and the mass of the secondary black hole is 6.96 脳 104m. The authors analyzed the changes of Mrk421's color index, including the quasi-simultaneous V-R color index and the long-term B-V color index. It was found that Mr k 421 showed the phenomenon of "turning dark and red" when Mrk421 was in a low state. This phenomenon may be caused by the contribution of thermal radiation from host galaxies to a larger proportion when the target is dark.
【學(xué)位授予單位】：山東大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2013
【分類號】：P141

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相關(guān)碩士學(xué)位論文 前1條

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本文編號：1529753