Plasma Properties and Magnetic Field Structure of the Solar Corona, Based on Coordinated Max 1991 Observations from SERTS, the VLA, and Magnetographs

Details Plasma Properties and Magnetic Field Structure of the Solar Corona, Based on Coordinated Max 1991 Observations from SERTS, the VLA, and Magnetographs Plasma Properties and Magnetic Field Structure of the Solar Corona, Based on Coordinated Max 1991 Observations from SERTS, the VLA, and Magnetographs

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hstx.rept.....b&link_type=abstract

Technical Report, Hughes STX, Inc. Lanham, MD United States

Astronomy and Astrophysics

Astronomy

Solar Corona, Magnetic Field Configurations, Plasma Temperature, Plasma Density, Solar Magnetic Field, Ultraviolet Astronomy, Ultraviolet Spectra, Microwave Emission, Satellite Observation, Very Large Array (Vla), Magnetic Signatures, Spectrographs, Spectroheliographs, Extreme Ultraviolet Radiation, Satellite Instruments, Emission Spectra, Line Spectra, Ultraviolet Telescopes, Bremsstrahlung, Thermal Emission, Solar Radiation

Scientific paper

The purposes of this investigation are to determine the plasma properties and magnetic field structure of the solar corona using coordinated observations obtained with NASA/GSFC's Solar EUV Rocket Telescope and Spectrograph (SERTS), the Very Large Array (VLA), and magnetographs. The observations were obtained under the auspices of NASA's Max '91 program. The methods of achieving the stated purposes are to use SERTS spectra and spectroheliograms to determine coronal plasma properties such as temperature, density, and emission measure. These properties are subsequently used to calculate the intensity of the thermal bremsstrahlung microwave emission from the coronal plasma (the minimum microwave intensity expected from the emitting plasma). This, in turn, can be used to establish which emission mechanism(s) contribute to the observed microwave emission. Because both mechanisms that may contribute to quiescent active region microwave emission (thermal bremsstrahlung and thermal gyroemission) depend upon the coronal magnetic field in known ways, this information can ultimately be used to derive the coronal magnetic field. Ideally, three-dimensional models of the coronal plasma and magnetic field which are consistent with all of the EUV spectra and spectroheliograms, as well as with the intensity and polarization maps at all of the microwave observing frequencies, can be derived. For completeness, the coronal magnetic field derived from the coordinated multiwaveband observations must be compared with extrapolations from photospheric magnetograms.

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