Tag Archives: convection

189. Spatial Scales and Time Variation of Solar Subsurface Convection

Contributed by Alexander Getling. Posted on October 31, 2022

Spectral analysis of the spatial structure of solar subphotospheric convection is carried out for subsurface flow maps. It is found that the horizontal flow scales increase rapidly with depth, from supergranulation to giant-cell values. The total power of the convective flows is found to be anticorrelated with the sunspot number variation over the solar activity cycle in shallow subsurface layers and positively correlated at larger depths.

161. Changes in granulation scales over the solar cycle seen with SDO/HMI and Hinode/SOT

Contributed by J. Ballot. Posted on August 29, 2021

An analysis of granule sizes over a few years of HMI observations shows that, even in quite regions, the granular size shows an anti-correlation with the solar magnetic activity with a time delay of about 300 days. The granular size decreases by about 2% during the activity maximum relative to the minimum.

91. On The Origin of the Double-Cell Meridional Circulation in the Solar Convection Zone

Contributed by Valery Pipin. Posted on March 19, 2018

It is demonstrated that when taking into account of the radial inhomogeneity of the Coriolis number, the solar-like differential rotation and the double-cell meridional circulation can both be reproduced by the mean-field model.

38. Subsurface Structure of Pores and Sunspots

Contributed by Robert Stein. Posted on May 12, 2015

Numerical simulation of sunspots indicate that different subsurface structures are possible. They may be deep coherent flux tubes or twisted spaghetti or shallow structures. It may well be that all the models proposed for sunspot structures are correct for some spot somewhere.

31. The Photospheric Size-Flux Distribution and its Relationship with the Small-Scale and Global Components of the Solar Dynamo

Contributed by Andrés Muñoz Jaramillo. Posted on October 31, 2014

Taking advantage of 11 different databases, we use statistical analysis to probe the nature of photospheric magnetic structures. We find evidence of two separate mechanisms at play, and propose that they are directly connected to the global and small-scale components of the solar dynamo.