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

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hstx.reptr....b&link_type=abstract

Annual Report, 12 Jul. 1994 - 11 Jul. 1995 Hughes STX, Inc., Lanham, MD.

Computer Science

Extreme Ultraviolet Radiation, Magnetic Field Configurations, Magnetic Signatures, Solar Corona, Solar Magnetic Field, Solar Wind, Spectroscopic Analysis, Bremsstrahlung, Calibrating, Microwave Emission, Photosphere, Solar Instruments, Spectrographs, Sun, Ultraviolet Telescopes, Very Large Array (Vla)

Scientific paper

The purposes of this investigation are to use existing, calibrated, coaligned sets of coordinated multiwaveband observations of the Sun to determine the coronal magnetic field strength and structure, and interpret the collective observations in terms of a self-consistent model of the coronal plasma and magnetic field. This information is vital to understanding processes such as coronal heating, solar wind acceleration, pre-flare energy storage, and active region evolution. Understanding these processes is the central theme of Max '91, the NASA-supported series of solar observing campaigns under which the observations acquired for this work were obtained. The observations came from NASA/GSFC's Solar EUV Rocket Telescope and Spectrograph (SERTS), the Very Large Array (VLA), and magnetographs. The technique of calculating the coronal magnetic field is to establish the contributions to the microwave emission from the two main emission mechanisms: thermal bremsstrahlung and thermal gyroemission. This is done by using the EUV emission to determine values of the coronal plasma quantities needed to calculate the thermal bremsstrahlung contribution to the microwave emission. Once the microwave emission mechanism(s) are determined, the coronal magnetic field can be calculated. A comparison of the coronal magnetic field derived from the coordinated multiwaveband observations with extrapolations from photospheric magnetograms will provide insight into the nature of the coronal magnetic field.

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