论文标题
带有冲击正常角度$θ_{b_n} $在时空中演变的太阳能粒子加速度在球形冲击下加速
Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle $θ_{B_n}$ Evolving in Space and Time
论文作者
论文摘要
我们提出了一个2D运动学模型，以研究由冠状质量喷射驱动的休克的太阳能颗粒（SEP）的加速度。震动被认为是从太阳中心抵消的来源的球形。这导致了磁场和冲击正常方向之间角度的空间和时间演变（$θ_{bn} $），因为它通过Parker螺旋磁场从下电晕到1 AU传播。我们发现，由于$θ_{bn} $的演变，高能SEP强度沿冲击前线有很大变化。通常，与东侧面和冲击鼻子相比，冲击的西侧优先加速颗粒到高能。这可以从加速度的速度来理解，而加速度在西侧较高。由于局部加速和运输效应，在我们的模型中复制了双重幂律能谱。这些结果将有助于更好地理解SEP加速的演变，并为多飞机运动物（尤其是靠近太阳的人，例如Parker Solar Probe和Solar Orbiter）观察到的大型SEP事件提供新的见解。
We present a 2D kinematic model to study the acceleration of solar energetic particles (SEPs) at a shock driven by a coronal mass ejection. The shock is assumed to be spherical about an origin that is offset from the center of the Sun. This leads to a spatial and temporal evolution of the angle between the magnetic field and shock normal direction ($θ_{Bn}$) as it propagates through the Parker spiral magnetic field from the lower corona to 1 AU. We find that the high-energy SEP intensity varies significantly along the shock front due to the evolution of $θ_{Bn}$. Generally, the west flank of the shock preferentially accelerates particles to high energies compared to the east flank and shock nose. This can be understood in terms of the rate of acceleration, which is higher at the west flank. Double power-law energy spectra are reproduced in our model as a consequence of the local acceleration and transport effects. These results will help better understand the evolution of SEP acceleration and provide new insights into large SEP events observed by multi-spacecraft, especially those close to the Sun, such as Parker Solar Probe and Solar Orbiter.
