ar X iv : a st ro - p h / 01 03 16 4 v 1 1 2 M ar 2 00 1 1 ON THE SOLAR ROTATION RATE IN THE UPPER CONVECTION ZONE

ar X iv : a st ro - p h / 07 03 71 1 v 1 2 8 M ar 2 00 7 Solar Interior – Radial Structure , Rotation , Solar Activity Cycle

Some basic properties of the solar convection zone are considered and the use of helioseismology as an observational tool to determine its depth and internal angular velocity is discussed. Aspects of solar magnetism are described and explained in the framework of dynamo theory. The main focus is on mean field theories for the Sun's magnetic field and its differential rotation.

ar X iv : a st ro - p h / 01 03 25 4 v 1 1 6 M ar 2 00 1 Construction of the Variability → Luminosity Estimator

ar X iv : a st ro - p h / 03 12 21 2 v 1 8 D ec 2 00 3 The Sun ’ s Preferred Longitudes and the Coupling of Magnetic Dynamo Modes

Observations show that solar activity is distributed non-axisymmetrically, concentrating at “preferred longitudes”. This indicates the important role of non-axisymmetric magnetic fields in the origin of solar activity. We investigate the generation of the non-axisymmetric fields and their coupling with axisymmetric solar magnetic field. Our kinematic generation (dynamo) model operating in a sph...

ar X iv : a st ro - p h / 01 03 44 4 v 1 2 7 M ar 2 00 1 From Centimeter to Millimeter Wavelengths : A High Angular Resolution Study of 3 C 273

We monitored 3C 273 with VLBI at 15–86 GHz since 1990. We discuss component trajectories, opacity effects, a rotating jet, and outburst-ejection relations from Gamma-ray to radio bands.

ar X iv : a st ro - p h / 02 05 14 1 v 1 9 M ay 2 00 2 To appear in ApJ What Causes P - mode Asymmetry Reversal ?

The solar acoustic p-mode line profiles are asymmetric. Velocity spectra have more power on the low-frequency sides, whereas intensity profiles show the opposite sense of asymmetry. Numerical simulations of the upper convection zone have resonant p-modes with the same asymmetries and asymmetry reversal as the observed modes. The temperature and velocity power spectra at optical depth τ cont = 1...