恒星潮汐撕裂事件的红外回响和活动星系核的X-射线辐射
发布时间：2018-07-27 10:43
【摘要】：随着多波段测光和光谱重复巡天的开展,天体爆发事件的发现和研究也越来越多,揭示出很多有趣的天体物理现象和性质。超大质量黑洞潮汐撕裂恒星事件(简称潮汐撕裂事件或TDE)属于非常有趣也是发生概率很小的事件。我们基于WISE的数据在五个TDE中发现了它们的红外回响信号,极大的丰富了对此类事件及其中心黑洞周围介质的研究和理解,打开了一个发现TDE候选体和研究休眠黑洞周围环境的新窗口。此外,我们还利用XMM-Newton空间望远镜的数据对近邻活动星系核的X-射线辐射特性开展了研究。本文将分别简要综述这两个方面的研究背景,然后详细介绍我们的具体工作,最后对我们在这两个方面工作进行总结和展望。潮汐撕裂事件的红外回响：我们利用WISE和NEOWISE-R近期释放的数据,在TDE ASASSN-141i中发现了明显的红外光变信号。ASASSN-141i是在最近十余年里发现的距离我们最近的TDE之一,其在紫外、光学、X-射线和射电多个波段都有很好研究。与TDE爆发前的中红外波段的亮度相比,我们发现在TDE被光学波段探测到36天后(或潮汐撕裂光度达到峰值后110天),这个源在W1、W2波段分别变亮了0.12、0.16星等。与之对应的黑体温度估计为～2100 K,比通常的尘埃升华温度稍高,表明其所处的位置在尘埃升华半径附近。如果认为这个红外波段增强信号来自于黑洞周围的尘埃,利用加热和辐射平衡,我们得到TDE的热光度在1043-1045 erg s-1之间(其范围主要由尘埃颗粒大小的不确定性引起的),与其它波段观测得到的峰值光度相当。该研究首次在观测上证实TDE的中心黑洞附近尘埃的红外回响信号的存在。除了ASASSN-141i之外,我们还对已知的四个暂现强冕线TDE候选体的红外回响进行了研究。这四个TDE的闪耀发生后均探测到持续的中红外辐射的大幅衰减,持续时间可以达到闪耀发生14年之后。在这些源的光学冕线闪耀发生3-5年后,即WISE卫星首次探测到这些源时,其中红外波段再辐射的光度在0.4-2 x 1043 erg s-1之间,尘埃温度在570到800 K之间。其光度和尘埃温度都随时间下降。这些中红外辐射衰减信号可以解释为潮汐撕裂闪耀的红外回响。利用加热和辐射平衡,我们得到的热光度在1-30 x 1044 erg s-1之间,距中心黑洞几个pc距离处的热尘埃质量为0.05-1.3Mo。我们的研究结果表明：在气体丰富的环境中,中红外回响信号是TDE的一个普遍信号。活动星系核的X-射线辐射：我们分析了一个红化的窄线Seyfert 1型亮星系Was 61的X-射线光谱及其时变特征。XMM-Newton寸该天体曝光90 ks,获得了高信噪比的X射线光谱和光变曲线。其能谱表现出多个特征,包括电离吸收、软X-射线过剩、和FeKα发射线。根据能谱拟合,其幂律连续谱谱型在流量变化时基本保持不变。其中的吸收物质被轻度的电离,柱密度为3×1021cm,并在XMM-Newton的观测时间内保持不变。如果这个源的光学红化也是由同样的物质引起的,这些物质应该在窄线区外侧,其尘气比与银河系的类似。有趣的是,我们探测到与连续谱流量变化相伴随的Fe K发射线的变化。在其流量较低的前40 ks内,观测到能量在16.7 keV的宽Fe Kα发射线,并且该宽Fe Kα发射线特征在之后的光谱中消失。在后20 ks的曝光时间里,光子计数率比低流量阶段高35%,观测到线心能量为(?)6.4 keV,宽度为～0.1 keV的窄Fe Kα发射线,并且窄Fe Kα发射线在两天后的观测中依然存在。我们认为上述变化与X-射线发射冕区的几何结构和动力学变化有关。另外,软X-射线超的温度和流量与硬X-射线幂律成分的流量之间存在弱相关性。我们认为一个内区光学厚的热康普顿化吸积盘模型比电离反射模型可能更适合解释软超成分。此外,作为主要合作者,本人还参与了对一个红移为6.3的极亮类星体的Chandra的探索性观测研究。这个源的X-射线辐射非常明亮,我们估计X-射线与光学波段之间的指数为αo、=-1.22-0.05+0.07,表明与其他具有同等光学紫外亮度的类星体相比,该类星体具有较强的X-射线辐射。从这次探测得到的X-射线特征来看,这个极亮类星体中心的黑洞很可能正处在super-Eddington吸积阶段。
[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.
【学位授予单位】：中国科学技术大学
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P152;P145.8;P172.2
本文编号：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.
【学位授予单位】：中国科学技术大学
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P152;P145.8;P172.2
【相似文献】
相关期刊论文 前1条
1 王亚迅;邵明珠;罗诗裕;宋爱民;;相干的参数X-射线辐射及弯晶的退道效应[J];半导体光电;2009年02期
相关博士学位论文 前1条
1 窦立明;恒星潮汐撕裂事件的红外回响和活动星系核的X-射线辐射[D];中国科学技术大学;2016年
，本文编号：2147564
本文链接：https://www.wllwen.com/shoufeilunwen/jckxbs/2147564.html
