AGN中央黑洞质量及辐射研究
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摘要
本文主要对射电强类星体中央黑洞质量与射电性质之间的关系，射电喷流和吸积盘之间相互作用，发射线性质等方面进行了一些研究．
类星体的辐射能量来自于中央黑洞吸积过程的能量释放，在此图像中，黑洞质量是一个非常重要的物理量．射电强类星体的重要特征之一是存在射电喷流，类星体的喷流可能是由核心的转动黑洞提供能量，或者是由吸积盘的磁场加速而产生．近两年来的一些研究工作表明，黑洞质量与射电活动性似乎存在密切联系．由于这些研究工作中，射电强类星体的数目较少，为了更好地对黑洞质量与射电辐射特性之间的关系进行研究，我们对86个射电强类星体进行了研究．我们利用宽H_β的线宽和光学连续谱光度，估算了中央黑洞质量，发现绝大部分类星体黑洞质量大于10~8M_⊙，但有部分的类星体黑洞质量较小，〈10~8M_⊙，最近的一个研究工作也证实了这个结果．射电光度有一随中央黑洞质量增长的趋势，中央黑洞质量与射电噪度之间有一很强的反相关关系，在一定程度上说明喷流形成与黑洞质量之间有较密切的联系．许多类星体光学／紫外连续谱存在一个大蓝包，一般认为大蓝包来自于吸积盘的热辐射，由吸积盘的物理状态所决定．因此，观测到的类星体连续谱反映了吸积盘的性质．最近的数值模拟表明，喷流可能在非常靠近黑洞的吸积盘内区加速形成．一些研究工作说明吸积盘和喷流之间很可能有相互作用，吸积盘上的外流风可以显著地改变吸积盘内区的温度分布．我们对一个射电低频选类星体样本研究了射电光学光度比与蓝／紫外连续谱谱指数之间的关系，发现，两者之间有很强的反相关关系，这说明蓝／紫外连续谱谱形与射电吸积功率比之间可能存在密切的联系．我们的结果说明喷流与吸积盘之间的相互作用很可能会影响吸积盘的结构和辐射谱．活动星系核光学光谱上的主要特征是有很强的发射线，宽发射线云团的动力学直接反映了活动星系核内部引力场或辐射场特性，分析各类谱线的强度和轮廓是深入了解活动星系核的有效途径．EGRET活动星系核的γ射线辐射机制可能是高能电子对软光子的逆康普顿过程．宽发射线辐射可能是软光子来源之一．但目前，还没有发现γ射线辐射与发射线强度之间的关系．对缺少发射线资料的EGRET活动星系核进行光谱观测，扩大宽发射线数据样本有利于进一步研究γ射线辐射机制．对于类星体，可以利用单次光谱观测，测量宽发射线宽度，结合光学连续光度，就可以对中央黑洞质量进行估算．我们对10个EGRET活动星系核和13个射电强类星体进行了光谱观测，主要对2个EGRET源和6个类星体测量了宽Hβ，MgⅡ，[OⅢ]λ5007发射线流量，等值宽度和宽度．对于6个类星体中的5个源，结合文献中给出的每个源的宽Hβ线宽度，我们发现宽Hβ线宽度是变化的，剩下的1个源，文献中没有这个源的宽Hβ线资料，我们给出了我们的测量值．我们对这8个源的中央黑洞质量进行了估算，发现所有源的中央黑洞质量都〉3×10~8M_⊙．
In this thesis, we present the studies of the relationships between the central black holemasses and radio properties, the interactions between the radio jets and accretion disc,and the properties of emission lines for radio-loud quasars.
The energy released from the accretion process upon central black holes is believed topower the quasars. In such scenario, the black hole mass is one of the most importantphysical quantity. The radio-loud quasars are characteristic of powerful radio jets, and thejets are probably powered by the rotating black hole, or accelerated by the magnetic field ofthe accretion disc. Several recent researches discovered the relationships between the blackhole masses and radio activities. But, the number of radio-loud quasars included in thesework is relatively small, we performed a study for a sample of 86 radio-loud quasars forfurther understanding the relationships between the black hole masses and radio activities.The central black-hole masses of radio-loud quasars are estimated by using the data of Hβline-width and the optical continuum luminosity. We found the vast majority of the quasarsin this sample have black-hole masses higher than 10~8M_⊙, while a few quasars may containrelatively smaller black-holes〈10~8M_⊙. Our results are confirmed by a recent researchon PHFS. There are a tendency of the radio luminosity increasing with the central blackhole mass. We found a significant anti-correlation between radio-loudness and the centralblack-hole mass. It might imply that the jet formation is related with the black-hole mass.
Many quasars show a big blue bump in the optical/UV continuum, which is usuallythought to origin from the thermal emission from the accretion disc. The optical/UVcontinuum is determined by the physical conditions of the accretion disc. So, the observedcontinuum of quasars could reflect the properties of accretion disc. Recent numericalsimulations indicate the jets probably accelerated from the inner region of accretion discnear the black hole. Some studies show the interactions between the jets and accretiondiscs may be important, and the outflows from the accretion disc could significantly alterthe temperature distribution in the inner region of the accretion disc. We studied therelationships between the ratio of radio to optical luminosities and the continuum spectralindex in blue/UV bands for a low-frequency radio selected quasar sample, and found asignificant anti-correlation. It might indicate that the continuum shape in blue/UV bandsis related to the ratio of jet to accretion power. The results may imply that the spectra and structure of accretion discs are probably affected by the interactions between jets anddiscs.
Strong emission-lines are the main characteristic of the optical spectra of AGN. Thedynamics of the broad emission line cloud directly reflect the inner gravitational field or theemission properties of AGN, and one of the effective means to understand AGN could bethrough analysing the strength and profile of various types of emission-lines. The inverse-compton process of soft photons upon high-energy electrons is probably responsible for theγ-ray emission. One possible origin of soft photon is from the emission of the broad-lineclouds. However, there is no obvious evidence on the relationships ofγ-ray emission and thestrength of emission-lines at present. The optical spectral observations for EGRET AGNslack of emission line data are useful for the further research onγ-ray radiation mechanism.For quasars, the central black hole masses could be estimated using the optical continuumluminostiy and the boad emission line width from the single spectra. We performed thespectral observations on ten EGRET AGNs and thirteen radio-loud quasars. Using 2.16mtelescope in the Xinglong station of NAO, we have measured the flux, equivalent widthand FWHM of broad H/β, MgⅡ, [OⅢ]λ5007 for two EGRET AGNs and six quasars. Forfive of six radio-loud quasars, combining the results of literature and ours, we found theFWHM of broad Hβline is varying. For the rest one, we found no broad Hβemission linedata available in the literature, and we present our measurements on this source. Finally,we estimated the central black hole masses for all eight sources, and found all the blackhole masses are higher than 3×10~8M_⊙.
类星体的辐射能量来自于中央黑洞吸积过程的能量释放，在此图像中，黑洞质量是一个非常重要的物理量．射电强类星体的重要特征之一是存在射电喷流，类星体的喷流可能是由核心的转动黑洞提供能量，或者是由吸积盘的磁场加速而产生．近两年来的一些研究工作表明，黑洞质量与射电活动性似乎存在密切联系．由于这些研究工作中，射电强类星体的数目较少，为了更好地对黑洞质量与射电辐射特性之间的关系进行研究，我们对86个射电强类星体进行了研究．我们利用宽H_β的线宽和光学连续谱光度，估算了中央黑洞质量，发现绝大部分类星体黑洞质量大于10~8M_⊙，但有部分的类星体黑洞质量较小，〈10~8M_⊙，最近的一个研究工作也证实了这个结果．射电光度有一随中央黑洞质量增长的趋势，中央黑洞质量与射电噪度之间有一很强的反相关关系，在一定程度上说明喷流形成与黑洞质量之间有较密切的联系．许多类星体光学／紫外连续谱存在一个大蓝包，一般认为大蓝包来自于吸积盘的热辐射，由吸积盘的物理状态所决定．因此，观测到的类星体连续谱反映了吸积盘的性质．最近的数值模拟表明，喷流可能在非常靠近黑洞的吸积盘内区加速形成．一些研究工作说明吸积盘和喷流之间很可能有相互作用，吸积盘上的外流风可以显著地改变吸积盘内区的温度分布．我们对一个射电低频选类星体样本研究了射电光学光度比与蓝／紫外连续谱谱指数之间的关系，发现，两者之间有很强的反相关关系，这说明蓝／紫外连续谱谱形与射电吸积功率比之间可能存在密切的联系．我们的结果说明喷流与吸积盘之间的相互作用很可能会影响吸积盘的结构和辐射谱．活动星系核光学光谱上的主要特征是有很强的发射线，宽发射线云团的动力学直接反映了活动星系核内部引力场或辐射场特性，分析各类谱线的强度和轮廓是深入了解活动星系核的有效途径．EGRET活动星系核的γ射线辐射机制可能是高能电子对软光子的逆康普顿过程．宽发射线辐射可能是软光子来源之一．但目前，还没有发现γ射线辐射与发射线强度之间的关系．对缺少发射线资料的EGRET活动星系核进行光谱观测，扩大宽发射线数据样本有利于进一步研究γ射线辐射机制．对于类星体，可以利用单次光谱观测，测量宽发射线宽度，结合光学连续光度，就可以对中央黑洞质量进行估算．我们对10个EGRET活动星系核和13个射电强类星体进行了光谱观测，主要对2个EGRET源和6个类星体测量了宽Hβ，MgⅡ，[OⅢ]λ5007发射线流量，等值宽度和宽度．对于6个类星体中的5个源，结合文献中给出的每个源的宽Hβ线宽度，我们发现宽Hβ线宽度是变化的，剩下的1个源，文献中没有这个源的宽Hβ线资料，我们给出了我们的测量值．我们对这8个源的中央黑洞质量进行了估算，发现所有源的中央黑洞质量都〉3×10~8M_⊙．
In this thesis, we present the studies of the relationships between the central black holemasses and radio properties, the interactions between the radio jets and accretion disc,and the properties of emission lines for radio-loud quasars.
The energy released from the accretion process upon central black holes is believed topower the quasars. In such scenario, the black hole mass is one of the most importantphysical quantity. The radio-loud quasars are characteristic of powerful radio jets, and thejets are probably powered by the rotating black hole, or accelerated by the magnetic field ofthe accretion disc. Several recent researches discovered the relationships between the blackhole masses and radio activities. But, the number of radio-loud quasars included in thesework is relatively small, we performed a study for a sample of 86 radio-loud quasars forfurther understanding the relationships between the black hole masses and radio activities.The central black-hole masses of radio-loud quasars are estimated by using the data of Hβline-width and the optical continuum luminosity. We found the vast majority of the quasarsin this sample have black-hole masses higher than 10~8M_⊙, while a few quasars may containrelatively smaller black-holes〈10~8M_⊙. Our results are confirmed by a recent researchon PHFS. There are a tendency of the radio luminosity increasing with the central blackhole mass. We found a significant anti-correlation between radio-loudness and the centralblack-hole mass. It might imply that the jet formation is related with the black-hole mass.
Many quasars show a big blue bump in the optical/UV continuum, which is usuallythought to origin from the thermal emission from the accretion disc. The optical/UVcontinuum is determined by the physical conditions of the accretion disc. So, the observedcontinuum of quasars could reflect the properties of accretion disc. Recent numericalsimulations indicate the jets probably accelerated from the inner region of accretion discnear the black hole. Some studies show the interactions between the jets and accretiondiscs may be important, and the outflows from the accretion disc could significantly alterthe temperature distribution in the inner region of the accretion disc. We studied therelationships between the ratio of radio to optical luminosities and the continuum spectralindex in blue/UV bands for a low-frequency radio selected quasar sample, and found asignificant anti-correlation. It might indicate that the continuum shape in blue/UV bandsis related to the ratio of jet to accretion power. The results may imply that the spectra and structure of accretion discs are probably affected by the interactions between jets anddiscs.
Strong emission-lines are the main characteristic of the optical spectra of AGN. Thedynamics of the broad emission line cloud directly reflect the inner gravitational field or theemission properties of AGN, and one of the effective means to understand AGN could bethrough analysing the strength and profile of various types of emission-lines. The inverse-compton process of soft photons upon high-energy electrons is probably responsible for theγ-ray emission. One possible origin of soft photon is from the emission of the broad-lineclouds. However, there is no obvious evidence on the relationships ofγ-ray emission and thestrength of emission-lines at present. The optical spectral observations for EGRET AGNslack of emission line data are useful for the further research onγ-ray radiation mechanism.For quasars, the central black hole masses could be estimated using the optical continuumluminostiy and the boad emission line width from the single spectra. We performed thespectral observations on ten EGRET AGNs and thirteen radio-loud quasars. Using 2.16mtelescope in the Xinglong station of NAO, we have measured the flux, equivalent widthand FWHM of broad H/β, MgⅡ, [OⅢ]λ5007 for two EGRET AGNs and six quasars. Forfive of six radio-loud quasars, combining the results of literature and ours, we found theFWHM of broad Hβline is varying. For the rest one, we found no broad Hβemission linedata available in the literature, and we present our measurements on this source. Finally,we estimated the central black hole masses for all eight sources, and found all the blackhole masses are higher than 3×10~8M_⊙.
引文
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