INTRO TO SPACE PHYS
INTRO TO SPACE PHYS ESS 471
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This 2 page Class Notes was uploaded by Miss Jeanette Keebler on Wednesday September 9, 2015. The Class Notes belongs to ESS 471 at University of Washington taught by Robert Holzworth in Fall. Since its upload, it has received 20 views. For similar materials see /class/192640/ess-471-university-of-washington in Earth And Space Sciences at University of Washington.
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Date Created: 09/09/15
Some Key Concepts in Solar Terrestrial Physics What is the solar power source fusion pp CNO cycles How do we know this neutrinos and fit to Standard Solar Model Summarize the Standard Solar Model Hydrostatic equilibrium and other assumptions gives 4 ordinary di erential equations and 4 unknowns Why does energy transport by convection dominate in the Convection Zone plasma becomes opaque to photons because atoms begin to form as T drops Describe the Solar Spectrum black body spectrum at 6000 0K dominates What physical phenomenon allows us to study Solar Seismology from Doppler shift can study photosphere motions result in Sound waves and Buoyancy oscillations Standing Waves What are some of the main features of the Photosphere sunspots granules and supergranules T N 6 000 0K What is the Frozen in Condition for magnetic elds and plasma plasma moves with magnetic field What is a plasma 39ionized gas Discuss the concepts of temperature density and basic response time of plasma describe plasma frequency and Debye Length plasmas shield E fields from net charged regions What is the real length of the sunspot cycle about 22 years Is the 39solar constant really constant no the Luminosity is NOT constant Since the Corona is above the photosphere it must be cooler right no it is HOT T N 1 06 K CME coronal Mass Ejections What is the source for the Solar Wind main source coronal holes Supersonic super Alfvenic What is the so called Garden hose angle for Interplanetary magnetic eld about 450 at Earth depends on speed of solar wind and rotation rate of sun What is the Heliosphere extent of the solar wind which extends to the Interstellar medium What is the Bow Shock 39Solar Wind Earth systems interaction first Bow Shock Describe the basic motion of charged particles Guiding Center Motion Drift Equations Describe the upstream region of the Earth s Bow Shock upstream region unique in shock physics Tincrease B increase Density increase velocity decrease at shock Describe some important Magnetosphere interactions Most solar wind plasma re ects o earth39s B field and flows around Chapman Ferraro current What does the Reconnection theory tell us puts whole magnetosphere in motion magnetospheric convection B field has to diffuse out of plasma MHD breakdown particle accelerationheating Give some Evidence for quot 39 particles in polar ionosphere 39 E and solar wind Describe the Magnetotail 39 hundreds of Re earth radii in length Reconnection in tail closes cycle and injects heated plasma into inner magnetosphere What is the motion of a Trapped energetic particle in dipole B eld 39 Gyration Bounce and Drift Describe the Radiation Belts What is the Ring current 39 2nd largest energy reservoir in magnetosphere what is largest What are the main properties of the Plasmasphere 39 high density low energy Corotation Discuss the importance of Field aligned currents 39 e g Auroras Coupled system How do the Magnetotail and ionosphere interact 39 substorms cross tail current interruption putting it all together Alfven shielding current systems coldhot plasma drifts Ionosphere D E and F regions Currents in Eregion can be dissipation less
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