Long-term behavior of active longitudes for solar X-ray flares

Details Long-term behavior of active longitudes for solar X-ray flares Long-term behavior of active longitudes for solar X-ray flares

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...471..711z&link_type=abstract

Astronomy and Astrophysics, Volume 471, Issue 2, August IV 2007, pp.711-716

Astronomy and Astrophysics

Astrophysics

11

Sun: Activity, Sun: Flares, Sun: Magnetic Fields

Scientific paper

Context: Recently, it was found that two persistent active longitudes of sunspots separated by about 180° existed on the sun by considering a dynamic reference frame inferred from the differential rotation law. The same phenomenon was found in the longitudinal distribution of powerful X-ray flares. Aims: To study the statistical characteristics of active longitudes of solar activities, we analyzed the data sets of optical flares associated with all the solar X-ray flares ≥ C class observed by GOES during the period of 1975 to 2005, of sunspots collected at the Royal Greenwich Observatory, the US Air Force, and NOAA for the same period as X-ray flares. Methods: The differential rotation law on the Sun is simply described as Ω = Ω0 - {B}sin2ϕ , where Ω is the angular velocity at a given latitude ϕ, while Ω0 is the equatorial angular velocity and B describes the differential rotation rate. Both Ω0 and B are the parameters that need to be determined from observations. Results: The authors found that there are two active longitudes separated by 180^circ for X-ray flares of any class, which have existed for tens of years, that X-ray flares occur more often near the two active longitudes than sunspots do, and that the non-axisymmetry of the longitudinal distribution of X-ray flares increases with the X-ray flare class. Conclusions: Stronger solar activities occur more preferentially at certain longitudes.

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