Geospace systems

围绕和通过地球磁层的能量流动受到一系列过程的调节。大多数基本关系被广泛理解，但日地空间科学仍然是一个相对年轻的领域，有许多悬而未决的问题。空间物理研究将增加我们对复杂的日地相互作用的理解，这些相互作用可能对空间和地面技术产生重大影响。未来的进展将涉及世界各地的数千名科学家和工程师，他们将把观测、理论和建模结合在一起，在广泛的空间和时间尺度上研究日地系统。*我的研究集中在两个领域：磁层对太阳风强迫的响应和对磁层结构和动力学的质子极光遥感。*太阳风和地球磁层之间的耦合极其复杂。一般来说，磁层的响应不仅取决于太阳风等离子体参数，而且还取决于磁层的当前状态和最近的时间历史。我的研究利用了太阳风动压和地球静止轨道磁场之间的一个相对简单的关系。这种联系是众所周知的，并在许多事件研究中得到了检验。然而，我最近开发了新的分析方法来证明这种效应可以在数千个时间间隔内被检测到。太阳风强迫和磁层响应之间的时间延迟将取决于卫星位置、太阳风参数和磁层条件。到达时间离散最小值对应于最优模型参数，并且使用非常大的数据集使我能够确定对其他量的依赖关系，例如磁场配置。这为研究许多不同的过程提供了一种创新的方法，包括太阳风的取向、传播和磁层的不对称性。磁层中的能量和散射过程产生了几种不同类型的粒子降水进入高层大气。质子极光(或氢极光)是极光椭圆形赤道方向边缘高能质子沉淀的著名标志。发光强度相对较低，因此需要比明亮的电子极光更灵敏的仪器。作为我在这个领域研究的一部分，我在加拿大北部运营着一个子午线扫描测光仪网络。来自该系统的数据用于确定质子极光的位置和亮度。这将提供有关磁层结构和动力学的独特信息来源。**

Energy flow around and through the Earth's magnetosphere is mediated by a wide range of processes. Most of the basic relationships are broadly understood, but solar terrestrial space science is still a relatively young field with many open questions. Space physics research will increase our understanding of complex sun-Earth interactions that can have significant effects on space- and ground-based technology. Future progress will involve thousands of scientists and engineers around the world bringing together observations, theory, and modeling to study the solar terrestrial system over a wide range of spatial and temporal scales.******My research focuses on two areas: magnetospheric response to solar wind forcing and proton auroral remote sensing of magnetospheric structure and dynamics.******Coupling between the solar wind and the Earth's magnetosphere is extremely complicated. In general, magnetospheric response depends not only on solar wind plasma parameters, but also on the present state and recent time history of the magnetosphere. My research takes advantage of a relatively simple relationship between solar wind dynamic pressure and magnetic field at geostationary orbit. This connection is well-known and has been examined in numerous event studies. However, I have recently developed new analysis methods to demonstrate that this effect can be detected in many thousands of intervals. The time delay between solar wind forcing and magnetospheric response will depend on satellite location, solar wind parameters, and magnetospheric conditions. Arrival time dispersion minima correspond to optimal model parameters, and using a very large data set allows me to determine dependence on other quantities such as magnetic field configuration. This provides an innovative approach to study many different processes including solar wind orientation, propagation, and magnetospheric asymmetry.******Energization and scattering processes in the magnetosphere produce several different types of particle precipitation into the upper atmosphere. The proton aurora (or hydrogen aurora) is a well-known signature of energetic proton precipitation at the equatorward edge of the auroral oval. The luminous intensity is relatively low, so more sensitive instruments are required than for bright electron aurora. As part of my research in this area I operate a network of meridian scanning photometers in northern Canada. Data from this system are used to determine proton auroral location and brightness. This will provide a unique source of information about magnetospheric structure and dynamics.**