恒星潮汐撕裂事件的紅外回響和活動(dòng)星系核的X-射線輻射
發(fā)布時(shí)間：2018-07-27 10:43
【摘要】：隨著多波段測(cè)光和光譜重復(fù)巡天的開展,天體爆發(fā)事件的發(fā)現(xiàn)和研究也越來越多,揭示出很多有趣的天體物理現(xiàn)象和性質(zhì)。超大質(zhì)量黑洞潮汐撕裂恒星事件(簡(jiǎn)稱潮汐撕裂事件或TDE)屬于非常有趣也是發(fā)生概率很小的事件。我們基于WISE的數(shù)據(jù)在五個(gè)TDE中發(fā)現(xiàn)了它們的紅外回響信號(hào),極大的豐富了對(duì)此類事件及其中心黑洞周圍介質(zhì)的研究和理解,打開了一個(gè)發(fā)現(xiàn)TDE候選體和研究休眠黑洞周圍環(huán)境的新窗口。此外,我們還利用XMM-Newton空間望遠(yuǎn)鏡的數(shù)據(jù)對(duì)近鄰活動(dòng)星系核的X-射線輻射特性開展了研究。本文將分別簡(jiǎn)要綜述這兩個(gè)方面的研究背景,然后詳細(xì)介紹我們的具體工作,最后對(duì)我們?cè)谶@兩個(gè)方面工作進(jìn)行總結(jié)和展望。潮汐撕裂事件的紅外回響：我們利用WISE和NEOWISE-R近期釋放的數(shù)據(jù),在TDE ASASSN-141i中發(fā)現(xiàn)了明顯的紅外光變信號(hào)。ASASSN-141i是在最近十余年里發(fā)現(xiàn)的距離我們最近的TDE之一,其在紫外、光學(xué)、X-射線和射電多個(gè)波段都有很好研究。與TDE爆發(fā)前的中紅外波段的亮度相比,我們發(fā)現(xiàn)在TDE被光學(xué)波段探測(cè)到36天后(或潮汐撕裂光度達(dá)到峰值后110天),這個(gè)源在W1、W2波段分別變亮了0.12、0.16星等。與之對(duì)應(yīng)的黑體溫度估計(jì)為～2100 K,比通常的塵埃升華溫度稍高,表明其所處的位置在塵埃升華半徑附近。如果認(rèn)為這個(gè)紅外波段增強(qiáng)信號(hào)來自于黑洞周圍的塵埃,利用加熱和輻射平衡,我們得到TDE的熱光度在1043-1045 erg s-1之間(其范圍主要由塵埃顆粒大小的不確定性引起的),與其它波段觀測(cè)得到的峰值光度相當(dāng)。該研究首次在觀測(cè)上證實(shí)TDE的中心黑洞附近塵埃的紅外回響信號(hào)的存在。除了ASASSN-141i之外,我們還對(duì)已知的四個(gè)暫現(xiàn)強(qiáng)冕線TDE候選體的紅外回響進(jìn)行了研究。這四個(gè)TDE的閃耀發(fā)生后均探測(cè)到持續(xù)的中紅外輻射的大幅衰減,持續(xù)時(shí)間可以達(dá)到閃耀發(fā)生14年之后。在這些源的光學(xué)冕線閃耀發(fā)生3-5年后,即WISE衛(wèi)星首次探測(cè)到這些源時(shí),其中紅外波段再輻射的光度在0.4-2 x 1043 erg s-1之間,塵埃溫度在570到800 K之間。其光度和塵埃溫度都隨時(shí)間下降。這些中紅外輻射衰減信號(hào)可以解釋為潮汐撕裂閃耀的紅外回響。利用加熱和輻射平衡,我們得到的熱光度在1-30 x 1044 erg s-1之間,距中心黑洞幾個(gè)pc距離處的熱塵埃質(zhì)量為0.05-1.3Mo。我們的研究結(jié)果表明：在氣體豐富的環(huán)境中,中紅外回響信號(hào)是TDE的一個(gè)普遍信號(hào)�；顒�(dòng)星系核的X-射線輻射：我們分析了一個(gè)紅化的窄線Seyfert 1型亮星系Was 61的X-射線光譜及其時(shí)變特征。XMM-Newton寸該天體曝光90 ks,獲得了高信噪比的X射線光譜和光變曲線。其能譜表現(xiàn)出多個(gè)特征,包括電離吸收、軟X-射線過剩、和FeKα發(fā)射線。根據(jù)能譜擬合,其冪律連續(xù)譜譜型在流量變化時(shí)基本保持不變。其中的吸收物質(zhì)被輕度的電離,柱密度為3×1021cm,并在XMM-Newton的觀測(cè)時(shí)間內(nèi)保持不變。如果這個(gè)源的光學(xué)紅化也是由同樣的物質(zhì)引起的,這些物質(zhì)應(yīng)該在窄線區(qū)外側(cè),其塵氣比與銀河系的類似。有趣的是,我們探測(cè)到與連續(xù)譜流量變化相伴隨的Fe K發(fā)射線的變化。在其流量較低的前40 ks內(nèi),觀測(cè)到能量在16.7 keV的寬Fe Kα發(fā)射線,并且該寬Fe Kα發(fā)射線特征在之后的光譜中消失。在后20 ks的曝光時(shí)間里,光子計(jì)數(shù)率比低流量階段高35%,觀測(cè)到線心能量為(?)6.4 keV,寬度為～0.1 keV的窄Fe Kα發(fā)射線,并且窄Fe Kα發(fā)射線在兩天后的觀測(cè)中依然存在。我們認(rèn)為上述變化與X-射線發(fā)射冕區(qū)的幾何結(jié)構(gòu)和動(dòng)力學(xué)變化有關(guān)。另外,軟X-射線超的溫度和流量與硬X-射線冪律成分的流量之間存在弱相關(guān)性。我們認(rèn)為一個(gè)內(nèi)區(qū)光學(xué)厚的熱康普頓化吸積盤模型比電離反射模型可能更適合解釋軟超成分。此外,作為主要合作者,本人還參與了對(duì)一個(gè)紅移為6.3的極亮類星體的Chandra的探索性觀測(cè)研究。這個(gè)源的X-射線輻射非常明亮,我們估計(jì)X-射線與光學(xué)波段之間的指數(shù)為αo、=-1.22-0.05+0.07,表明與其他具有同等光學(xué)紫外亮度的類星體相比,該類星體具有較強(qiáng)的X-射線輻射。從這次探測(cè)得到的X-射線特征來看,這個(gè)極亮類星體中心的黑洞很可能正處在super-Eddington吸積階段。
[Abstract]:With the development of multi band photometry and spectral duplication, the discovery and research of celestial bursts are becoming more and more, and many interesting astrophysical phenomena and properties are revealed. The event of stellar torn stars in supermassive black holes (the tidal rip or TDE) is very interesting and very small. We are based on WISE The data of the five TDE found their infrared echoes, which greatly enriched the study and understanding of the media around the black hole and its central black hole, and opened a new window to discover the TDE candidate and study the surrounding environment of the dormant black hole. In addition, we also use the data of the XMM-Newton space telescope for nearby active galaxies. The characteristics of the nuclear X- ray radiation are studied. This paper will briefly review the research background of these two aspects, and then introduce our specific work in detail. Finally, we summarize and look forward to our work on these two aspects. The infrared echo of the tidal rip events: we use the data released by WISE and NEOWISE-R in the near future, in TDE ASASS N-141i found an obvious infrared light change signal.ASASSN-141i is one of our nearest TDE in the last decade, which has been well studied in ultraviolet, optical, X- and radio bands. Compared with the brightness of the middle infrared band before the TDE burst, we now detect 36 days (or tides) in the optical band of TDE. The tear luminosity reaches 110 days after peak value), the source at the W1, W2 band brightens 0.12,0.16 stars respectively. The corresponding blackbody temperature is estimated to be 2100 K, which is slightly higher than the usual dust sublimation temperature, indicating that its location is near the dust sublimation radius. If the red outer band enhancement signal is derived from the dust around the black hole, Using the heating and radiation balance, we get the thermal light of TDE between 1043-1045 ERG S-1 (its range is mainly caused by the uncertainty of the size of the dust particles), which is equivalent to the peak luminosity observed in other bands. This study was the first time to observe the existence of the infrared echo signal near the dust of the central black hole of the TDE. Except ASASSN In addition to -141i, we also studied the infrared reverberation of the four known coronal line TDE candidates. The four TDE blazes detected a significant attenuation of continuous medium infrared radiation, which lasted 14 years after the blazed. After 3-5 years in the optical coronal lines of these sources, the WISE satellite was first explored. When these sources were measured, the infrared radiance luminosity was between 0.4-2 x 1043 ERG s-1, and the dust temperature was between 570 and 800 K. The luminosity and dust temperature decreased with time. These infrared radiation attenuation signals can be interpreted as the infrared reverberation of the tidal rip blazed. Using the heating and radiation balance, we get the thermal light of 1 -30 x 1044 ERG s-1, the mass of hot dust at several PC distances from the central black hole is 0.05-1.3Mo.. Our results show that in a gas rich environment, the mid infrared reverberation signal is a universal signal for TDE. The X- ray radiation of the active galactic nucleus: We analyzed the X- of a reddish narrow line Seyfert 1 bright galaxy Was 61. The ray spectrum and its time-varying characteristic.XMM-Newton inch of the celestial body is exposed to 90 KS, and the high signal to noise ratio X ray spectra and light curves are obtained. The energy spectrum shows many characteristics, including ionization absorption, soft X- ray surplus, and FeK alpha hair rays. According to the energy spectrum, the power law continuous spectral pattern is basically unchanged when the flow changes. The substance is slightly ionized and the column density is 3 * 1021cm and remains unchanged during the observation time of XMM-Newton. If the optical redness of the source is also caused by the same substance, these substances should be outside the narrow line area, and the dust gas is similar to that of the Milky way. It is interesting that we detect the Fe K associated with the continuous spectral flow change. In the first 40 KS of the lower flow rate, the wide Fe K alpha emission line of energy at 16.7 keV was observed and the wide Fe K alpha hair ray characteristics disappeared in the subsequent spectrum. In the post 20 KS exposure time, the photon counting rate was 35% higher than the low flow stage, and the line core energy was (?) 6.4 keV and the width of the narrow Fe K alpha to 0.1 keV. The emission lines, and the narrow Fe K alpha emission lines still exist in two days. We think the above changes are related to the geometric structure and dynamics of the X- ray emission coronal region. In addition, there is a weak correlation between the temperature and flow of the soft X- ray and the flow of the power law component of the hard X- ray. The plton accretion disk model may be more suitable for interpreting the soft hyper components than the ionized reflection model. In addition, as a major collaborator, I also participated in the exploratory observational study of a Chandra of a red shift of 6.3 very bright quasars. The X- ray radiation of this source is very bright, and we estimate that the index between X- ray and optical band is alpha o, =-1 .22-0.05+0.07 shows that the quasar has a strong X- ray radiation compared to other quasars with the same optical ultraviolet luminance. From the X- ray characteristics obtained by this probe, the black hole at the center of the very bright quasar is likely to be in the super-Eddington accretion phase.
【學(xué)位授予單位】：中國(guó)科學(xué)技術(shù)大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2016
【分類號(hào)】：P152;P145.8;P172.2
本文編號(hào)：2147564
[Abstract]:With the development of multi band photometry and spectral duplication, the discovery and research of celestial bursts are becoming more and more, and many interesting astrophysical phenomena and properties are revealed. The event of stellar torn stars in supermassive black holes (the tidal rip or TDE) is very interesting and very small. We are based on WISE The data of the five TDE found their infrared echoes, which greatly enriched the study and understanding of the media around the black hole and its central black hole, and opened a new window to discover the TDE candidate and study the surrounding environment of the dormant black hole. In addition, we also use the data of the XMM-Newton space telescope for nearby active galaxies. The characteristics of the nuclear X- ray radiation are studied. This paper will briefly review the research background of these two aspects, and then introduce our specific work in detail. Finally, we summarize and look forward to our work on these two aspects. The infrared echo of the tidal rip events: we use the data released by WISE and NEOWISE-R in the near future, in TDE ASASS N-141i found an obvious infrared light change signal.ASASSN-141i is one of our nearest TDE in the last decade, which has been well studied in ultraviolet, optical, X- and radio bands. Compared with the brightness of the middle infrared band before the TDE burst, we now detect 36 days (or tides) in the optical band of TDE. The tear luminosity reaches 110 days after peak value), the source at the W1, W2 band brightens 0.12,0.16 stars respectively. The corresponding blackbody temperature is estimated to be 2100 K, which is slightly higher than the usual dust sublimation temperature, indicating that its location is near the dust sublimation radius. If the red outer band enhancement signal is derived from the dust around the black hole, Using the heating and radiation balance, we get the thermal light of TDE between 1043-1045 ERG S-1 (its range is mainly caused by the uncertainty of the size of the dust particles), which is equivalent to the peak luminosity observed in other bands. This study was the first time to observe the existence of the infrared echo signal near the dust of the central black hole of the TDE. Except ASASSN In addition to -141i, we also studied the infrared reverberation of the four known coronal line TDE candidates. The four TDE blazes detected a significant attenuation of continuous medium infrared radiation, which lasted 14 years after the blazed. After 3-5 years in the optical coronal lines of these sources, the WISE satellite was first explored. When these sources were measured, the infrared radiance luminosity was between 0.4-2 x 1043 ERG s-1, and the dust temperature was between 570 and 800 K. The luminosity and dust temperature decreased with time. These infrared radiation attenuation signals can be interpreted as the infrared reverberation of the tidal rip blazed. Using the heating and radiation balance, we get the thermal light of 1 -30 x 1044 ERG s-1, the mass of hot dust at several PC distances from the central black hole is 0.05-1.3Mo.. Our results show that in a gas rich environment, the mid infrared reverberation signal is a universal signal for TDE. The X- ray radiation of the active galactic nucleus: We analyzed the X- of a reddish narrow line Seyfert 1 bright galaxy Was 61. The ray spectrum and its time-varying characteristic.XMM-Newton inch of the celestial body is exposed to 90 KS, and the high signal to noise ratio X ray spectra and light curves are obtained. The energy spectrum shows many characteristics, including ionization absorption, soft X- ray surplus, and FeK alpha hair rays. According to the energy spectrum, the power law continuous spectral pattern is basically unchanged when the flow changes. The substance is slightly ionized and the column density is 3 * 1021cm and remains unchanged during the observation time of XMM-Newton. If the optical redness of the source is also caused by the same substance, these substances should be outside the narrow line area, and the dust gas is similar to that of the Milky way. It is interesting that we detect the Fe K associated with the continuous spectral flow change. In the first 40 KS of the lower flow rate, the wide Fe K alpha emission line of energy at 16.7 keV was observed and the wide Fe K alpha hair ray characteristics disappeared in the subsequent spectrum. In the post 20 KS exposure time, the photon counting rate was 35% higher than the low flow stage, and the line core energy was (?) 6.4 keV and the width of the narrow Fe K alpha to 0.1 keV. The emission lines, and the narrow Fe K alpha emission lines still exist in two days. We think the above changes are related to the geometric structure and dynamics of the X- ray emission coronal region. In addition, there is a weak correlation between the temperature and flow of the soft X- ray and the flow of the power law component of the hard X- ray. The plton accretion disk model may be more suitable for interpreting the soft hyper components than the ionized reflection model. In addition, as a major collaborator, I also participated in the exploratory observational study of a Chandra of a red shift of 6.3 very bright quasars. The X- ray radiation of this source is very bright, and we estimate that the index between X- ray and optical band is alpha o, =-1 .22-0.05+0.07 shows that the quasar has a strong X- ray radiation compared to other quasars with the same optical ultraviolet luminance. From the X- ray characteristics obtained by this probe, the black hole at the center of the very bright quasar is likely to be in the super-Eddington accretion phase.
【學(xué)位授予單位】：中國(guó)科學(xué)技術(shù)大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2016
【分類號(hào)】：P152;P145.8;P172.2
【相似文獻(xiàn)】
相關(guān)期刊論文 前1條
1 王亞迅;邵明珠;羅詩裕;宋愛民;;相干的參數(shù)X-射線輻射及彎晶的退道效應(yīng)[J];半導(dǎo)體光電;2009年02期
相關(guān)博士學(xué)位論文 前1條
1 竇立明;恒星潮汐撕裂事件的紅外回響和活動(dòng)星系核的X-射線輻射[D];中國(guó)科學(xué)技術(shù)大學(xué);2016年
，本文編號(hào)：2147564
本文鏈接：http://sikaile.net/shoufeilunwen/jckxbs/2147564.html
最近更新
教材專著
