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

TL;DR

This study analyzes how solar granulation scales change over the solar cycle using high-resolution data from SDO/HMI and Hinode/SOT, revealing cyclical variations linked to solar activity.

Contribution

It provides the first detailed measurement of solar granulation property variations over a cycle, combining space-based observations from SDO and Hinode.

Findings

Granule density varies by about 2% over the cycle.

Granule mean area decreases at solar maximum.

Granulation changes lag behind sunspot activity by about one year.

Abstract

The Sun is the only star where the superficial turbulent convection can be observed at very high spatial resolution. The Solar Dynamics Observatory (SDO) has continuously observed the full Sun from space with multi-wavelength filters since July 2010. In particular, the Helioseismic and Magnetic Imager (HMI) instrument takes high-cadence frames (45 seconds) of continuum intensity in which solar granulation is visible. We aimed to follow the evolution of the solar granules over an activity cycle and look for changes in their spatial properties. We investigated the density of granules and their mean area derived directly from the segmentation of deconvolved images from SDO/HMI. To perform the segmentation, we define granules as convex elements of images. We measured an approximately 2% variation in the density and the mean area of granules over the cycle, the density of granules being greater at solar maximum with a smaller granule mean area. The maximum density appears to be delayed by about one year compared to classical activity indicators, such as the sunspot number. We complemented this study with high-spatial-resolution observations obtained with Hinode/SOTBFI (Solar Optical Telescope Broadband Filter Imager), which are consistent with our results. The observed variations in solar granulation at the disc centre reveal a direct insight into the change in the physical properties that occur in the upper convective zone during a solar cycle. These variations can be due to interactions between convection and magnetic fields, either at the global scale or, locally, at the granulation scale.