Space Weather is a new field of science that studies the space environment driven by the interaction between the Sun and the Earth. Space Weather can adversely affect humans and human technology, including astronauts, satellites (systems and orbits), communications and navigation, electric power grids, and pipelines.  This course begins with an overview of the space weather systems involving the Sun, Heliosphere, Magnetosphere and Ionosphere. Physical processes in the solar atmosphere are the ultimate drivers of space weather. We will present the basic structure of the Sun, the solar magnetic field and configuration, the physical bases of flares and coronal mass ejections, and particle acceleration mechanisms. The various forms of particle and field outflow are traced throughout interplanetary space.  Evolution of solar disturbances through the solar system the configuration of the solar magnetic field in the heloiosphere, and the consequences for acceleration of particles are covered. The interaction of the solar wind with the nearby interstellar medium is covered as well. Together, the Sun and heliosphere form the boundary conditions for establishing the physical state of the near-Earth space system, including the upper atmosphere.

        The outermost magnetized region surrounding the Earth is the magnetosphere. The solar wind causes the Earth’s dipole-like field to be distorted and elongated. The outermost field lines are highly variable, depending on the conditions of the solar wind. The physical processes that govern the magnetosphere’s behavior and its interaction with the atmosphere will be covered. These include electric fields and particle acceleration that can produce geomagnetic storms. The ground state of the upper atmosphere is established primarily by solar radiation. The fundamental equations of state that dictate atmospheric equilibrium and the creation of the ionosphere will be presented. Basic processes include neutral gas dynamics, ionospheric motions, and photochemical processes. Some aspects of non-thermal radiation transport and spectroscopy will be covered as background material for understanding remote sensing of the near-Earth space environment, a new tool for understanding space weather on a global-scale.

• Overview of Space Weather Systems (Sun, Heliosphere, Magnetosphere, Ionosphere)
• Solar interior and helioseismology
• Solar Magnetic field and magnetic reconnection
  
• Structure of Solar Atmosphere: Photosphere, Chromosphere, Transition Region and Corona
• Solar Activity: Flares, Coronal Mass Ejecitons and Solar Energetic Particles
• Solar Wind Formation and Acceleration, Heliospheric Structure
• CMEs and energetic particles in the heliosphere, interplanetary shocks
  
• Solar Wind Interacation with Magnetized and Non-Magnetized Planets
• Solar Wind Interaction with the Nearby Interstellar Medium
• Magnetospheric Structure; Bow shock scattering; Charged particle orbits
  
• Dawn-dusk electric feild; gyrokinetic codes; magnetic tail and current sheet
  
• MHD codes and boundary conditions; pararrel E-fields & precipitation; satellite diagnostics
  
• Interaction of Solar Radiation with the Upper Atmosphere
• Geomagnetic Storms, Airglow, Photoioniztation and Photochemistry
• Ionospheric Structure; Electrodynamics
• Space Weather Effects on Technological Systems
  

Homework      

Projects:

Exams: one midterm and final

Grades:          

Text Book (required):                

Supplement Reference Books (reserved at Johnson Center Library):

“Physics of the Solar Corona”, Markus J. Aschwanden, 2004

 “Solar and Steller Magnetic Activity”, Carolus J. Schrijver and Cornelis Zwann, 1999

“Solar Activity and Earth's Climate”, R.E. Benestad, 2002

“An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres”, May-Britt Kallenrode, 2004

 “Theory of Planetary Atmosphere”, Joseph W. Chamberlain, Donald M. Hunten

     “Physics & Chemistry of the Upper Atmosphere”, M.H. Rees

     "Physics of space plasma: An Introduction", George K. Parks