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.
Contributed by Chris Hanson. Posted on June 27, 2022
High-frequency inertial waves were detected inside the Sun, propagating retrograde relative to the solar rotation with a phase speed faster than equatorial Rossby waves. How these waves are generated is discussed but remains unclear.
Contributed by Samarth G. Kashyap. Posted on September 29, 2021
A new method, which is to characterize the multiscale convective spectrum of the Sun using high-resolution line-of-sight Dopplergram images from HMI, is developed, enabling the authors to estimate the spectrum to the finest observable scales.
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.
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.
Contributed by Gopal Hazra. Posted on December 19, 2017
The Sun’s meridional flow varies with the solar cycle, and this is possibly caused by the back-reaction of the dynamo-generated magnetic field on the meridional flow due to the Lorentz force.
Contributed by Ben Greer. Posted on June 29, 2015
Ring-diagram analysis reveals that the convective flow speed inside the Sun is consistent with most numerical simulations of global convection.
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.
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.
Contributed by Michal Švanda. Posted on September 24, 2014
Flow system in an average supergranule is compared to the moat flow around axisymmetric sunspots. Both phenomena are very similar, only the outflow in the moat is distorted due to the proper motion of the sunspot with respect to the local frame of rest and moat is a purely downflow region.