Observations of solar wind from both large polar coronal holes (PCHs) during Ulysses' third
orbit showed that the fast solar wind was slightly slower, significantly less dense, cooler, and …

A major challenge for gravitational-wave (GW) detection in the μ Hz band is engineering a
test mass (TM) with sufficiently low acceleration noise. We propose a GW detection concept …

The last solar minimum, which extended into 2009, was especially deep and prolonged.
Since then, sunspot activity has gone through a very small peak while the heliospheric …

We examined plasma and magnetic field observations from all three Ulysses polar orbits of
the Sun to study the properties of the slow and fast solar wind and interplanetary coronal …

We explore new opportunities for solar physics that could be realized by future missions
providing sustained observations from vantage points away from the Sun-Earth line. These …

In an effort to understand the three-dimensional structure of the solar corona and inner
heliosphere during the Whole Heliosphere Interval (WHI), we have developed a global …

Observations from the recent Whole Heliosphere Interval (WHI) solar minimum campaign
are compared to last cycle's Whole Sun Month (WSM) to demonstrate that sunspot numbers …

We update two kinds of results obtained with the SWAN instrument on board SOHO. First,
we use H cell data recorded in 2001 and derive the H flow direction in the same way the …

The evolution of solar wind speed distribution during the period 1985–2008, which covers
two solar cycles (22 and 23), has been investigated using multistation interplanetary …

Quasi‐thermal noise spectroscopy is an efficient tool for measuring in situ macroscopic
plasma properties in space, using a passive wave receiver at the ports of an electric …