Some properties of latitude-time evolution of local and background solar magnetic fields

Latitudinal Distribution of Photospheric Magnetic Fields of Different Magnitudes

“…Another study (Deng et al, 2013) showed that polar faculae lead the sunspot number by 52 months. Polar facular measurements are in excellent agreement with polar magnetic flux estimates and allow studying the evolution of the polar magnetic field (Muñoz-Jaramillo et al, 2012). A strong correlation between the heliospheric magnetic field (HMF) and the polar flux at solar minimum was found, whereas during periods of activity the HMF showed a good correlation with the square root of the sunspot area.…”

“…The width of the sunspot zone and its connection to the solar cycle was studied in Ivanov, Miletskii, and Nagovitsyn (2011), and Miletsky, Ivanov, and Nagovitsyn (2015). The active latitude bands are narrow at minimum, expand to a greatest width at the time of maximum, and then narrow again during the declining phase of the cycle.…”

Latitudinal Profiles of the Photospheric Magnetic Field in Solar Cycles 19–21

“…The strong difference of variations of a total magnetic flux at low and high latitudes is revealed. The analysis of development of latitudinal distributions for magnetic fields with different strengths in solar cycles 12-23 has shown, that the width of a sunspot zone is intimately connected with the total magnetic flux of sunspots (Miletsky, Ivanov, Nagovitsyn, 2015).…”

“…It was shown by Li, Yun, Gu (2001), that the latitude migration-velocity of sunspot groups is maximal at the beginning of a solar cycle, decreasing later in process of solar cycle development. The width of the sunspot zone and its connection to the solar cycle was studied in (Ivanov, Miletskii, Nagovitsyn, 2011;Miletsky, Ivanov, Nagovitsyn, 2015).…”