Astronomy and Astrophysics – Astronomy
Scientist
Astronomy and Astrophysics
Astronomy
Scientist
High Altitude Observatory, Boulder, Colo.
Boston College, Chestnut Hill, MA
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099, USA
Jet Propulsion Lab., California Institute of Technology
Jet Propulsion Laboratory, Pasadena, CA, US
MS 169-506, JPL, Pasadena, CA, USA;
California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
Jet Propulsion Laboratory, California Institute of Technology, Pasadena
JPL, Pasadena, CA
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
Boston College, Chestnut Hill, Mass.
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
Jet Propulsion Laboratory, M / S 169-506 4800 Oak Grove Drive, Pasadena, CA 91109, USA
Jet Propulsion Laboratory, M / 8 169-506 4800 Oak Grove Dr., Pasadena, CA 91109, USA
Jet Propulsion Laboratory, California Institute of Technology
Boston Coll., Chestnut Hill, MA.
Jet Propulsion Laboratory, Pasadena, CA, USA
AFGL
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
Jet Propulsion Laboratory, Pasadena, California
Jet Propulsion Laboratory, Pasadena, CA 91101, USA
Helio research, 5212, Maryland Avenue, La Crescenta, USA
Jet Propulsion Lab., California Institute of Technology, Pasadena.
National Aeronautics and Space Administration. Lyndon B. Johnson Space Center, Houston, TX.
Jet Propulsion Laboratory, California Institute of Technology, 91109, Pasadena, CA, USA
California State Universit
A High-Speed Erupting-Prominence CME: A Bridge Between Types
A new model for the calculation and prediction of solar proton fluences
A new proton fluence model for E greater than 10 MeV
An estimate of the maximum speed of the solar wind, 1938-1989
Auroral changes during the eighteenth and nineteenth centuries and their implications for the solar wind and the long-term variation of sunspot activity
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