Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22

Details Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22 Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992cait.rept.....m&link_type=abstract

Annual Technical Report, 1 Oct. 1990 - 30 Sep. 1991 California Inst. of Tech., Pasadena. Solar Astronomy Group.

Astronomy and Astrophysics

Astronomy

Magnetic Fields, Magnetic Flux, Photosphere, Solar Activity Effects, Solar Cycles, Solar Magnetic Field, Solar Radiation, Velocity Distribution, Brightness, Light (Visible Radiation), Sunspots

Scientific paper

One key accomplishment from the research during FY 1991 was the finding by K. Harvey and P. Foukal that the photospheric network is the third significant component that accounts for observed variations in the total solar irradiance (the first previously recognized component is the temporary decreases due to sunspots and the second is variation due to plage brightness). Other key accomplishments were the K. Harvey results from studying magnetic flux over the solar cycle: (1) increases in the total magnetic flux by a factor of 4 to 5 from solar minimum to solar maximum with the variation from active regions flux (greater than 25 Gauss) by more than a factor of 20 from cycle minimum to maximum while the variation from quiet sun fields (less than 25 Gauss) was no more than a factor of 2; (2) interpretation of (1) as meaning that more than 70 percent of the magnetic flux in active regions disappears without dispersing; (3) slower decreases of weak fields in phase with the decrease in strong fields; and (4) irregular pulses of new flux which appear to be primarily associated with active region complexes.

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