Development of Models of Electron Density in the            Magnetosphere from Ground and Satellite-Based Radio Data
{'Code': '06020203', 'Directorate': {'Abbreviation': 'GEO', 'LongName': 'Directorate For Geosciences'}, 'Division': {'Abbreviation': 'AGS', 'LongName': 'Div Atmospheric & Geospace Sciences'}}
{'SignBlockName': 'Kenneth H. Schatten', 'PO_EMAI': None, 'PO_PHON': None}
The purpose of this grant is for the development and                       interpretation of empirical models of electron density in the                   equatorial plane of the earth's magnetosphere.  When available,                 these models will provide a substantially improved basis for                    studies of magnetospheric convection, wave-particle interactions,               and plasma interchange between the magnetosphere and ionosphere.                The models would be based primarily upon a combination of results               from whistlers recorded be Stanford University at Antarctic                     stations and from the University of Iowa Plasma Wave Experiment                 Sweep Frequency Receiver on the ISEE-1 satellite.                                    Magnetospheric research has reached a point of increasing                  emphasis upon the development of theoretical and empirical models               of the plasma distribution and dynamics, an example of this                     emphasis being the October 1986 Huntsville Workshop on                          Magnetosphere-Ionosphere Plasma Models.  Among the magnetospheric               plasma parameters which one can model empirically, equatorial                   electron density neq now appears to be one of the most important                and most accessible.  This parameter is of scientific interest                  for many reasons.  It depends upon a number of fundamental                      physical processes that are difficult to observe, such as solar                 wind induced convection and relate substorm morphology and the                  interchange of ionization with the spatially and temporally                     variable ionosphere.  neq represents the equatorial propagation                 medium and hence the conditions on wave refractive index under                  which resonant wave particle interactions take place, including                 particle scattering from the radiation belts.  The equatorial                   plasma is also an important part of the medium through which ULF                waves must propagate in carrying energy form either the solar                   wind or the magnetopause regions where wave-particle interactions               may be modulated at ULF frequencies.
{'FirstName': 'Donald', 'LastName': 'Carpenter', 'PI_MID_INIT': 'L', 'PI_SUFX_NAME': None, 'PI_FULL_NAME': 'Donald L Carpenter', 'EmailAddress': None, 'NSF_ID': '000435227', 'StartDate': '02/01/1988', 'EndDate': None, 'RoleCode': 'Principal Investigator'}
{'Name': 'Stanford University', 'CityName': 'STANFORD', 'ZipCode': '943052004', 'PhoneNumber': '6507232300', 'StreetAddress': '450 JANE STANFORD WAY', 'StreetAddress2': None, 'CountryName': 'United States', 'StateName': 'California', 'StateCode': 'CA', 'CONGRESSDISTRICT': '16', 'CONGRESS_DISTRICT_ORG': 'CA16', 'ORG_UEI_NUM': 'HJD6G4D6TJY5', 'ORG_LGL_BUS_NAME': 'THE LELAND STANFORD JUNIOR UNIVERSITY', 'ORG_PRNT_UEI_NUM': None}
{'Name': None, 'CityName': None, 'StateCode': None, 'ZipCode': None, 'StreetAddress': None, 'CountryCode': None, 'CountryName': None, 'StateName': None, 'CountryFlag': None, 'CONGRESSDISTRICT': None, 'CONGRESS_DISTRICT_PERF': '""'}
[{'Code': '1523', 'Text': 'SOLAR-TERRESTRIAL'}, {'Code': '5750', 'Text': 'MAGNETOSPHERIC PHYSICS'}, {'Code': '9120', 'Text': 'CROSS-DIRECTORATE PROGRAMS'}]
{'url': 'https://www.nsf.gov/awardsearch/download?DownloadFileName=1987&All=true', 'xml': '8720411.xml'}