Speaker
Elena Benevolenskaya
(Pulkovo Astronomical Observatory, Saint Petersburg)
Description
The current solar cycle 24 attracts an attention of researchers to study the nature
of the solar activity at the different levels of the Sun from the interior to the
solar corona. The Solar Dynamics Observatory (SDO) provides us multi-waves data from
the Extreme Ultraviolet to the visible light and magnetic field measurements. Here,
it is presented the synoptic structure of the solar cycle 24 using the line-of sight
component of the magnetic field (HMI/SDO), EUV emission in lines: 171A, 193A and
304A (AIA/SDO) from May 2010, 20 to January 2013, 25 (CR2097--CR2032). This
structure detects the extremely strong north-south asymmetry in the emerging magnetic
flux and as a result the delay in the polar magnetic field reversals. This delay
occurs due to impulses of the magnetic flux with negative in Northern hemisphere and
with positive polarity Southern hemispheres at the beginning of the solar cycle. The
coronal patterns follow the magnetic activity and display the activity waves in the
mid-latitude. In the high-latitude the EUV emission of the line of Fe IX,X (171A)
clearly shows the high-latitude wave in the south, and the less pronounced activity
wave in the north.
Primary author
Elena Benevolenskaya
(Pulkovo Astronomical Observatory, Saint Petersburg)
