Some features of the evolution of the magnetic complex of activity including AO NOAA 11944 and NOAA 11946, during its passage across the solar disk

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Abstract

The evolution of properties of the magnetic activity complex (MAC) during its passage across the solar disk on (03–12).01.2014 was analyzed. This MAC comprises two active regions (ARs) magnetically coupled by the equator, that are located in different solar hemispheres: AR NOAA 11944 in the Southern Hemisphere and NOAA 11946 in the Northern Hemisphere. Time dependences of total unsigned magnetic fluxes of all spots, including pores, and specifically for each polarity were plotted for each AR. The variation of total unsigned magnetic flux F(t) for all MAC sunspots was examined with respect to the variation of total area of the corresponding sunspots S(t). In all cases, the magnetic flux increases non-monotonically, reaches its maximum, and decreases afterwards. We found differences in the pattern of changes in F(t) and S(t) during the period 10.01–12.01, which are related to the characteristics of radiation bursts in the hard X-ray range and solar flares in soft X-ray range. No halo-type coronal mass ejections were detected in the MAC during the entire observation period, and relatively few limb CMEs were detected when the MAC was close to limbs.

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About the authors

Yu. S. Zagainova

Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation of the Russian Academy of Sciences (IZMIRAN)

Author for correspondence.
Email: yuliazag@izmiran.ru
Russian Federation, Troitsk, Moscow

V. N. Obridko

Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation of the Russian Academy of Sciences (IZMIRAN)

Email: yuliazag@izmiran.ru
Russian Federation, Troitsk, Moscow

V. G. Fainshtein

Institute of Solar–Terrestrial Physics, SB of RAS

Email: yuliazag@izmiran.ru
Russian Federation, Irkutsk

G. V. Rudenko

Institute of Solar–Terrestrial Physics, SB of RAS

Email: yuliazag@izmiran.ru
Russian Federation, Irkutsk

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2. Fig. 1. Images of the solar disk from the SCA when it is located near the central meridian for three moments in time. Below the equator in the southern hemisphere of the Sun is AO NOAA 11944, above is AO 11946. The white areas correspond to the positive polarity of the radial magnetic field, the dark areas correspond to the negative polarity of the radial magnetic field. The curved black lines are the calculated magnetic field lines.

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3. Fig. 2. Changes over time in the total unsigned magnetic flux F(t) from the umbra of all solar spots (filled black squares) and the area S(t) of the umbra of all solar spots (circles) in the period 03–11.01.2014. Shaded areas of the graphs are those where, due to projection effects, the error in determining the values of the studied parameters of the sunspot umbra is large.

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4. Fig. 3. Time variation of the unsigned magnetic flux in the umbra of sunspots of each polarity for each AO in the MCA. The upper graph is constructed for AO 11946, the lower graph – for AO 11944. The vertical lines mark the moments of solar flares in the hard X-ray range. Circles and black filled squares refer to head spots, circles and unfilled squares – to trailing spots.

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