Construction of Hybrid Model for Astrophysical Jets

考虑到气体、辐射和磁压力，我们构建了一个从一个几何上很薄的圆盘发出的稳定射流模型。我们发现射流通常有多个临界（跨音速）点，因为沿流线的重力和辐射力不是单调的。因此，射流通过鞍型临界点加速到超音速。我们还得到了射流终端速度的近似经验公式。2004年，我们研究了超临界吸积盘的轴向喷流，那里的质量吸积率远远超过爱丁顿吸积率。喷射气体受到中心物体的重力、来自圆盘的辐射通量以及圆盘强辐射场的辐射阻力的影响。我们计算了轴上射流的平衡速度和终点速度。我们还发现了终端速度和磁盘亮度之间的一个有用的表达式。fy2005我们在完全特殊相对论的处理下，仔细地研究了来自一个发光盘的相对论辐射流。假设流动是垂直的，忽略重力、气体压力和粘性加热。用数值方法求解了圆盘内从流底（圆盘“内部”）到流顶的辐射驱动流。对于给定的光深和流底处适当的初始条件（即流的起始点），得到流中的负载质量作为流顶边界条件的特征值。此外，还得到了流速和沿流辐射场随光深的变化规律。

FY2003We constructed a steady jet model emanating from a geometrically thin disk, taking into account the gas, radiation, and magnetic pressures. We have found that the jet flow generally have multiple critical (transonic) points, since the gravitational and radiative forces along the streamline do not monotonic.As a result, the jet flow is accelerated by passing through the saddle type critical point to be supersonic.We also obtained an approximate empirical formula for the terminal speed of jet flows.FY2004We examined on-axis jets of supercritical accretion disks, where the mass-accretion rate highly exceeds the Eddington accretion rate. The jet gas suffers from the gravity of the central object, the radiative flux from the disk, and the radiation drag force of the intense radiation fields of the disk.We have calculated the equilibrium speed as well as the terminal one for on-axis jets.We also found a useful expression between the terminal speed and the disk luminosity.FY2005We carefully examined the relativistic radiative flow from a luminous disk under a fully special relativistic treatment. The flow is assumed to be vertical, and the gravity, the gas pressure, and the viscous heating are ignored. The radiatively-driven flow in a luminous disk is numerically solved, from the flow base (disk "inside") to the flow top. For a given optical depth and appropriate initial conditions at the flow base, where the flow starts, a loaded mass in the flow is obtained as an eigenvalue of the boundary condition at the flow top. Moreover, the flow velocity and radiation fields along the flow are obtained as a function of the optical depth.