Waves and oscillations have been observed in the Sun's atmosphere for over half a century.
While such phenomena have readily been observed across the entire electromagnetic …

The brightness of the Sun varies on all timescales on which it has been observed, and there
is increasing evidence that this has an influence on climate. The amplitudes of such …

A wealth of new experimental and theoretical results has been obtained in solar physics
since the first edition of this textbook appeared in 1989. Thus all nine chapters have been …

ABSTRACT A three-dimensional magnetohydrodynamic (MHD) model for the propagation
and dissipation of Alfvén waves in a coronal loop is developed. The model includes the …

Numerical simulations provide information on solar convection not available by direct
observation. We present results of simulations of near surface solar convection with realistic …

As we resolve ever smaller structures in the solar atmosphere, it has become clear that
magnetism is an important component of those small structures. Small-scale magnetism …

We present the first center-to-limb G-band images synthesized from high-resolution
simulations of solar magnetoconvection. Toward the limb the simulations show" hilly" …

In solving the solar coronal heating problem, it is crucial to comprehend the mechanisms by
which energy is conveyed from the photosphere to the corona. Recently, magnetic …

We propose a novel one-dimensional model that includes both shock and turbulence
heating and qualify how these processes contribute to heating the corona and driving the …

Using realistic ab initio simulations of radiative magnetoconvection, we show that the bright
structures in images taken in the" G band," a spectral band dominated by lines of the CH …