We present a statistical analysis of solar coronal mass ejections (CMEs) based on 23 years
of quasi-continuous observations with the LASCO coronagraph, thus covering two complete …

Context. It is well known that the polarity of the Sun's magnetic field reverses or flips around
the maximum of each 11 year solar cycle. This is commonly known as polar field reversal …

This study examines the variation of different energies linked with the Sun and the Earth's
magnetosphere-ionosphere systems for solar cycles (SCs) 22–24 for which the gradual …

We examine the temporal changes in both solar polar magnetic field (PMF) at latitudes≥
45° and heliospheric magnetic field (HMF) at 1 AU during solar cycles 21–24 with emphasis …

We report observations of a steady 20 year decline of solar photospheric fields at latitudes≥
45° starting from∼ 1995. This prolonged and continuing decline, combined with the fact that …

The ratio of the rms electron density fluctuations to the background density in the solar wind
(density modulation index, epsilon N≡ ΔN/N) is of vital importance for understanding …

Elongated magnetic polarities are observed during the emergence phase of bipolar active
regions (ARs). These extended features, called magnetic tongues, are interpreted as a …

Similar to the Sun, other stars shed mass and magnetic flux via ubiquitous quasi-steady
wind and episodic stellar coronal mass ejections (CMEs). We investigate the mass loss rate …

Three-dimensional electron density distributions in the solar corona are reconstructed for
100 Carrington rotations (CR 2054–2153) during 2007/03–2014/08 using the spherically …

We report on the amplitude of the density turbulence spectrum () and the density modulation
index (δN/N) in the solar wind between 10 and 45R⊙. We derive these quantities using a …