We have analyzed the full set of Solar and Heliospheric Observatory (SOHO) Michelson Doppler Imager (MDI) fand p-mode oscillation frequencies from 1996 to date in a search for evidence of solar radius evolution during the rising phase of the current activity cycle. Just as Antia et al. in 2000, we Ðnd that a signiÐcant fraction of the f-mode frequency changes scale with frequency and that if th...

We propose that the coronal magnetic field, linking concentrations on the photosphere through an interwoven web of flux, embodies a scale-free network. It arises from a self-organized critical dynamics including flux emergence, the diffusion and merging of magnetic concentrations, as well as avalanches of reconnecting flux tubes. Magnetic concentrations such as fragments, pores and sunspots, ar...

We present a comprehensive model of the global properties of Alfvén waves in the solar atmosphere and the fast solar wind. Linear non-WKB wave transport equations are solved from the photosphere to a distance past the orbit of the Earth, and for wave periods ranging from 3 s to 3 days. We derive a radially varying power spectrum of kinetic and magnetic energy fluctuations for waves propagating ...

The Earth-Sun Lagrangian point 4 is a meta-stable location at 1 AU from the Sun, 60° ahead of Earth's orbit. It has an uninterrupted view solar photosphere centered on W60, nominal magnetic field connection to Sun. Such mission its own would serve as remote sensing observatory that oversee entire radiation hemisphere with significant relevance for protecting Moon and Mars explorers exposure. In...

The 3 seismic sources S1, S2 and S3 detected from MDI dopplergrams using the time-distance diagram technique are presented with the locations, areas and vertical and horizontal velocities of the visible wave displacements. Within the datacube of 120 Mm the horizontal velocities and the wave propagation times slightly vary from source to source. The momenta and start times measured from the TD d...

Small-scale fluctuations of magnetic field and velocity may be responsible for the Stokes asymmetries observed in all photospheric magnetic structures (the MISMA hypothesis). We support the hypothesis showing that atmospheres with optically-thin micro-structure reproduce the polarization of Fe I λ6301.5 Å and Fe I λ6302.5 Å observed in a sunspot. Ten thousand spectra were fitted by model MISMAs...

Alfvén waves have proven to be important in a range of physical systems due their ability transport non-thermal energy over long distances magnetized plasma. This property is specific interest solar physics, where the extreme heating atmosphere Sun remains unexplained. In an inhomogeneous plasma such as flux tube atmosphere, they manifest incompressible torsional perturbations. However, despite...

The magnetic field in the interplanetary medium is formed by action of sources on photosphere Sun and currents expanding atmosphere solar wind. In turn, high-speed plasma flow changes configuration lines. problem determining parameters near thus a three-dimensional interaction We present analytical expressions for calculating total vector B→(r, θ, ϕ) (in spherical coordinates) radially wind fin...