论文标题
$σ_{\ rmhβ} $ - 基于无量纲的积聚率及其与agn的电晕的联系
The $σ_{\rm Hβ}$-based dimensionless accretion rate and its connection with the corona for AGN
论文作者
论文摘要
关于$ \ rmhβ$以半限度为单位的全宽度（$ \ rm fwhm_ {hβ} $），广泛的$ \ rmhβ$线分散（$σ_{\ rmhβ} $）首选为单个速度tracer，以计算单个ep-epblack supermass supermass supermass supermass supermass supermass supermass supermass supermass supermass supermass supermass supermass bh。 \ cite {yu2020b}。 For a compiled sample of 311 broad-line active galactic nuclei (AGN) with measured hard X-ray photon index ($z<0.7$), $σ_{\rm Hβ}$ and the optical Fe II relative strength ($R_{\rm Fe}$) are measured from their optical spectra, which are used to calculate $σ_{\rm Hβ}$-based virial $ m _ {\ rm bh} $和无量化的积聚率（$ \ dot {\ mathscr {m}} $）。关于$ \ rm fwhm _ {\ rmhβ} $ $ \ dot {\ mathscr {m}} $平均要小于0.51 dex。发现存在Eddington比率（$ l _ {\ rm bol}/l _ {\ rm edd} $）与$ \ dot {\ nathscr {m}} $，即\ dot {\ mathscr {m}}}^{0.56 \ pm 0.01} $。这种非线性关系来自增值效率$η$，对于具有较高$ \ dot {\ Mathscr {m}} $的AGN而言，它较小。我们发现在电晕$ f _ {\ rm x} $中与$ \ dot {\ Mathscr {\ Mathscr {m}} $和\ mbh，$ f _ {\ rm x} \ propto \ dot propto \ dot {\ mathscr {\ mathscr {\ pm pm pm pm pm pm pm， m _ {\ rm bh}^{ - 0.54 \ pm 0.06} $。 $ -0.57 \ pm 0.05 $的扁平坡度有利于积聚盘的剪切应力张量与气体压力和总压的几何平均值成正比。我们发现$γ$与$ \ dot {\ mathscr {m}} $和$ f _ {\ rm x} $，$γ\ propto \ dot {\ Mathscr {\ Mathscr {m}}^{ - 0.21 { - 0.21 { - 0.21} f pm pm pm pm pm rmMMMM，我们发现了$γ$的牢固双变量关系0.04} $。硬X射线频谱随着$ f _ {\ rm x} $的增加而变得更柔和，尽管散布很大。
With respect to the $\rm Hβ$ full width at half-maximum ($\rm FWHM_{Hβ}$), the broad $\rm Hβ$ line dispersion ($σ_{\rm Hβ}$) was preferred as a velocity tracer to calculate the single-epoch supermassive black hole mass ($M_{\rm BH}$) suggested by \cite{Yu2020b}. For a compiled sample of 311 broad-line active galactic nuclei (AGN) with measured hard X-ray photon index ($z<0.7$), $σ_{\rm Hβ}$ and the optical Fe II relative strength ($R_{\rm Fe}$) are measured from their optical spectra, which are used to calculate $σ_{\rm Hβ}$-based virial $M_{\rm BH}$ and dimensionless accretion rate ($\dot{\mathscr{M}}$). With respect to $\rm FWHM_{\rm Hβ}$, it is found that the mean value of $σ_{\rm Hβ}$-based $M_{\rm BH}$ is on average larger by 0.26 dex, and the mean value of $σ_{\rm Hβ}$-based $\dot{\mathscr{M}}$ is on average smaller by 0.51 dex. It is found that there exists a non-linear relationship between the Eddington ratio ($L_{\rm Bol}/L_{\rm Edd}$) and $\dot{\mathscr{M}}$, i.e., $L_{\rm Bol}/L_{\rm Edd} \propto \dot{\mathscr{M}}^{0.56\pm 0.01}$. This non-linear relationship comes from the accretion efficiency $η$, which is smaller for AGN with higher $\dot{\mathscr{M}}$. We find a strong bivariate correlation of the fraction of energy released in the corona $F_{\rm X}$ with $\dot{\mathscr{M}}$ and \mbh, $F_{\rm X} \propto \dot{\mathscr{M}}^{-0.57\pm 0.05} M_{\rm BH}^{-0.54\pm 0.06}$. The flat slope of $-0.57\pm 0.05$ favours the shear stress tensor of the accretion disk being proportional to the geometric mean of gas pressure and total pressure. We find a strong bivariate relation of $Γ$ with $\dot{\mathscr{M}}$ and $F_{\rm X}$, $Γ\propto \dot{\mathscr{M}}^{-0.21\pm 0.02}F_{\rm X}^{0.02\pm 0.04}$. The hard X-ray spectrum becomes softer with increasing of $F_{\rm X}$, although the scatter is large.
