The Geometrical Structure and Physics of Coronal Mass       Ejections
{'Code': '06020203', 'Directorate': {'Abbreviation': 'GEO', 'LongName': 'Directorate For Geosciences'}, 'Division': {'Abbreviation': 'AGS', 'LongName': 'Div Atmospheric & Geospace Sciences'}}
{'SignBlockName': 'Sherry O. Farwell', 'PO_EMAI': None, 'PO_PHON': None}
Solar disturbances produce major effects on the corona, the                solar wind, the interplanetary medium, and the Earth along with                 its magnetosphere.  New techniques have been developed for                      studying plasma disturbances in the inner heliosphere.  This                    grant will continue an investigation of the physics of these                    disturbances, using data from the HELIOS zodiacal-light                         photometers and a variety of other coronal instruments.  These                  zodiacal-light photometers (data coverage from 1974 to 1986)                    provide the first stereoscopic information about the heliospheric               shapes of these disturbances.  The basic research effort includes               modeling techniques to interpret and match the observational                    data.  The HELIOS imaging combined with other observations                      provides a unique opportunity to determine coronal mass-ejection                velocities, streamer material velocities, 3-dimensional                         structures, and total masses in the interplanetary medium.  This                can be done with fewer assumptions and to greater accuracies                    than heretofore possible.  Beside mass ejections, solar                         disturbances which reach the interplanetary medium also include                 coronal streamers, shocks measured in situ and co-rotating                      interface regions.  It has been possible to view these features                 with the zodiacal-light photometers on board the HELIOS                         spacecraft and this study will relate near-surface solar                        structures and the heliospheric current sheet.
[{'FirstName': 'Hugh', 'LastName': 'Hudson', 'PI_MID_INIT': 'S', 'PI_SUFX_NAME': None, 'PI_FULL_NAME': 'Hugh S Hudson', 'EmailAddress': None, 'NSF_ID': '000260154', 'StartDate': '08/15/1988', 'EndDate': None, 'RoleCode': 'Co-Principal Investigator'}, {'FirstName': 'Bernard', 'LastName': 'Jackson', 'PI_MID_INIT': 'V', 'PI_SUFX_NAME': None, 'PI_FULL_NAME': 'Bernard V Jackson', 'EmailAddress': 'bvjackson@ucsd.edu', 'NSF_ID': '000314554', 'StartDate': '08/15/1988', 'EndDate': None, 'RoleCode': 'Principal Investigator'}]
{'Name': 'University of California-San Diego', 'CityName': 'LA JOLLA', 'ZipCode': '920930021', 'PhoneNumber': '8585344896', 'StreetAddress': '9500 GILMAN DR', 'StreetAddress2': None, 'CountryName': 'United States', 'StateName': 'California', 'StateCode': 'CA', 'CONGRESSDISTRICT': '50', 'CONGRESS_DISTRICT_ORG': 'CA50', 'ORG_UEI_NUM': 'UYTTZT6G9DT1', 'ORG_LGL_BUS_NAME': 'UNIVERSITY OF CALIFORNIA, SAN DIEGO', 'ORG_PRNT_UEI_NUM': None}
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[{'Code': '1523', 'Text': 'SOLAR-TERRESTRIAL'}, {'Code': '5750', 'Text': 'MAGNETOSPHERIC PHYSICS'}]
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