论文标题
SS433中分子云的物理特性；分子云与SS433射流的相互作用的证据
Physical properties of the molecular cloud, N4, in SS433; Evidence for an interaction of molecular cloud with the jet from SS433
论文作者
论文摘要
我们对分子云N4进行了观察和分析，该N4位于SS433的〜40 pc，与无线电外壳相同的视线，在12CO（j = 1-0），12co（j = 3-2），13co（j = 3-2），13co（j = 3-2）和大态oh oh emissions.n4中具有强大的整体级别，即12co（jemented Interted Interated Interated Interted Interated Interted Interted Antiment of 12co），J = j = j = J = j = j = j = -j = j = J = j = j = j = j = J = j = j = j.东方和西部边缘。 N4的主体还具有〜0.16 km s^-1 20“^-1。从系统性速度向〜49 km s^-1的速度向速度偏离3 km s^-1的速度，仅在N4的西北部仅检测到49 km s^-1。 13CO（J = 3-2）通过Radex代码进行的排放量为10^3 cm^-3，T_K范围〜20 K至〜56K。估计N4的质量为〜7300 mo。 N4中的热压力往往与银河平面中的分子云相似，这些值高于银河系平面中典型的分子云的值。 N4与先前的研究相比，由于当前的伽马射线观测值的敏感性低，因此很难检测到宇宙射线质子的辐射，这是由于观察值和天线束稀释的敏感性低。
We conducted observations and analyses of the molecular cloud, N4, which is located at ~40 pc from SS433 and the same line of sight as that of the radio shell, in 12CO(J=1-0), 12CO(J=3-2), 13CO(J=3-2), and grand-state OH emissions.N4 has a strong gradient of the integrated intensity of 12CO(J=1-0, 3-2) emission at the northern, eastern and western edges. The main body of N4 also has a velocity gradient of ~0.16 km s^-1 20"^-1. A velocity shift by up to 3 km s^-1 from the systemic velocity at ~49 km s^-1 is detected at only the northwestern part of N4. The volume density of the molecular hydrogen gas and the kinematic temperature are estimated at eight local peaks of 12CO(J=1-0) and 13CO(J=3-2) emissions by the RADEX code. The calculated n(H2) is an order of 10^3 cm^-3, and T_k ranges ~20 K to ~56 K. The mass of N4 is estimated to be ~7300 Mo. The thermal and turbulent pressures in N4 are estimated to be ~10^5 K cm^-3 and ~10^7 K cm^-3, respectively. The relation of the thermal and turbulent pressures in N4 tends to be similar to that of the molecular clouds in the Galactic plane. However, these values are higher than those in the typical molecular clouds in the Galactic plane. Several pieces of circumstantial evidence representing the physical properties of N4 and comparison with the data of infrared and X-ray radiation suggest that N4 is interacting with a jet from SS433. However, no gamma-ray radiation is detected toward N4. Compared to the previous study, it is hard to detect the gamma-ray radiation by cosmic-ray proton origin due to the low sensitivity of the current gamma-ray observatories. Any OH emission was not detected toward N4 due to the low sensitivity of the observation and antenna beam dilution.
