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A STRUCTURE FOR QUASARS

机译：拟态的结构

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This paper proposes a simple, empirically derived, unifying structure for the inner regions of quasars. This structure is constructed to explain the broad absorption line regions (BALRs) and the narrow " associated" ultraviolet and X-ray "ionized" absorbers (NALs) and is also found to explain the broad emission line regions (BELRs) and several scattering features, including a substantial fraction of the broad X-ray Fe-K emission line and the biconical extended narrow emission line region (ENLR) struc- tures seen on large kiloparsec scales in Seyfert images. The model proposes that a funnel-shaped thin shell outflow creates all of these features. The wind arises vertically from a narrow range of radii on a disk at BELR velocities. Radiation force then acceler- ates the flow radially, so that it bends outward to a cone angle of ~60 deg. and has a divergence angle of ~6 deg. , to give a covering factor of ~ l0%. When the central continuum is viewed from the side, through this wind, narrow high-ionization "associated" ultraviolet absorption lines and the X-ray "ionized absorbers" are seen, as in many low-luminosity active galactic nuclei (AGNs). When viewed end-on, the full range of velocities is seen in absorption with a large total column density, giving rise to the broad absorption line systems seen in a minority of quasars, the BAL QSOs. The wind is both warm (~ 10~6 K) and highly ionized. This warm highly ionized medium (WHlM) has a density of ~ 10~9 cm~-3, putting it in pressure equilibrium with the BELR clouds; the BELR is then a cool phase embedded in the overall outflow, avoiding cloud destruction through shear. The wind has the correct ionization parameter and filling factor for this. The high- and low-ionization zones of the BELR correspond to the cylindrical and conical regions of the wind, since the former is exposed to the full continuum while the latter receives only the continuum filtered by the former. The warm wind is significantly Thomson thick along the radial flow direction, producing the polarized optical continuum found in BALs, but is only partially ionized, creating a broad fluorescent 6.4 keV Fe-K emission line and greater than 10 keV Compton hump. The conical shell outflow can produce a biconical matter-bounded NELR. Luminosity-dependent changes in the structure, reducing the cylindrical part of the fiow or increasing the mean angle to the disk axis and decreasing the wind opening angle, may explain the UV and X-ray Baldwin effects and the greater prevalence of obscuration in low-luminosity AGNs.
机译：本文为类星体的内部区域提出了一个简单的，根据经验推导的统一结构。此结构构造用于解释宽吸收线区域（BALR）和狭窄的“相关”紫外和X射线“电离”吸收剂（NALs），还可以发现其解释宽发射线区域（BELR）和一些散射特征包括大部分的X射线Fe-K发射线和在塞弗图像中在大千帕尺度上看到的双锥扩展的窄发射线区域（ENLR）结构。该模型建议漏斗形的薄壳流出物产生所有这些特征。风以BELR速度从磁盘上的狭窄半径范围垂直产生。辐射力然后沿径向加速流动，使其向外弯曲成锥角〜60度。且发散角约为〜6度。给出约10％的覆盖率。当从侧面看中央连续体时，通过这种风，可以看到狭窄的高电离“相关”紫外线吸收线和X射线“电离吸收体”，就像许多低发光活性银河核（AGNs）一样。从尾部观察时，可以看到吸收整个速度范围，并且总柱密度大，从而在少数类星体BAL QSO中看到了较宽的吸收线系统。风既温暖（〜10〜6 K）又高度离子化。这种温暖的高电离介质（WH1M）的密度约为10〜9 cm〜-3，使其与BELR云处于压力平衡状态。那么，BELR就是一个冷态，嵌入到整个流出物中，避免了由于剪切作用而造成的云团破坏。为此，风具有正确的电离参数和填充因子。 BELR的高电离区和低电离区对应于风的圆柱区域和圆锥区域，因为前者暴露于完整的连续体，而后者仅接收由前者过滤的连续体。沿径向流动方向，暖风的厚度明显为Thomson厚，产生了在BAL中发现的偏振光学连续体，但仅被部分电离，从而产生了宽泛的6.4 keV Fe-K荧光发射线和大于10 keV的康普顿峰。圆锥形外壳流出可产生双圆锥形边界NELR。结构中与光度有关的变化，减少了流的圆柱部分或增加了与圆盘轴的平均角度并减小了风的张开角度，这可以解释紫外线和X射线鲍德温效应以及低空下的遮盖率较高的原因。发光度AGN。

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