Near-Sun Switchback Boundaries: Dissipation with Solar Distance

Evolution of Near-Sun Solar Wind Turbulence

This paper presents a preliminary analysis of the turbulence spectrum of the solar wind in the near-Sun region R < 50R⊙, obtained from interplanetary scintillation measurements with the Ooty Radio Telescope at 327 MHz. The results clearly show that the scintillation is dominated by density irregularities of size about 100 − 500 km. The scintillation at the small-scale side of the spectrum, alth...

Understanding Coronal Heating and Solar Wind Acceleration: Case for in Situ Near-sun Measurements

[1] The solar wind has been measured directly from 0.3 AU outward, and the Sun’s atmosphere has been imaged from the photosphere out through the corona. These observations have significantly advanced our understanding of the influence of the Sun’s varying magnetic field on the structure and dynamics of the corona and the solar wind. However, how the corona is heated and accelerated to produce t...

Neutrinos from the Sun: Experimental results confronted with solar models.

Tidal Dissipation in Rotating Solar-type Stars

We calculate the excitation and dissipation of low-frequency tidal oscillations in uniformly rotating solar-type stars. For tidal frequencies smaller than twice the spin frequency, inertial waves are excited in the convective envelope and are dissipated by turbulent viscosity. Enhanced dissipation occurs over the entire frequency range rather than in a series of very narrow resonant peaks, and ...

The sun and heliosphere at solar maximum.

Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitu...