Anticorrelation of X-ray bright points with sunspot number, 1970-1978

Details Anticorrelation of X-ray bright points with sunspot number, 1970-1978 Anticorrelation of X-ray bright points with sunspot number, 1970-1978

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229l.145g&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 229, May 1, 1979, p. L145-L150.

Astronomy and Astrophysics

Astrophysics

45

Solar Activity, Solar Corona, Sunspots, X Ray Spectra, Magnetic Signatures, Skylab Program, Solar Cycles, Solar Magnetic Field, Solar Oscillations, X Ray Imagery

Scientific paper

Soft X-ray observations of the solar corona over the period 1970-1978 show that the number of small short-lived bipolar magnetic features (X-ray bright points) varies inversely with the sunspot index. During the entire period from 1973 to 1978 most of the magnetic flux emerging at the solar surface appeared in the form of bright points. In 1970, near the peak of solar cycle 20, the contributions from bright points and from active regions appear to be approximately equal. These observations strongly support an earlier suggestion that the solar cycle may be characterized as an oscillator in wave-number space with relatively little variation in the average total rate of flux emergence.

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