The sun, the closest star to us, is not as quiet as it seems, and a wide variety of solar activity takes place every hour and every moment. These phenomena are formed by the accumulation and release of energy and are related to solar magnetic fields.
Magnetic helicalness can quantitatively characterize the solar magnetic field’s topology properties and non-potential state. Studying the deposition and transport of the magnetic helix can help understand the energy transfer process, from production in the interior of solar energy to deposit in the corona.
A research team from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC) calculated the accumulated magnetic helicity through the photosphere (Hemp) and the instantaneous relative magnetic helicity in the corona (Hmc) using the helicity flux integration method and finite volume. Method respectively.
This work has been published in The Astrophysical Journal.
The researchers found that the consistency of Hmc and Hemp partially depends on the resolution of the magnetograms and their computational methods.
Coronal magnetic fields are derived from photospheric magnetic fields with the help of the nonlinear force-free field (NLFFF) model. This study evaluates the value of the NLFFF model and provides a reference for future comparison investigations of different magnetic helicity.
“The work is owed to excellent data from the Solar Magnetic Field Telescope, which was independently developed by Chinese scientists and has been operating steadily for nearly 40 years,” said Wang Quan, NAOC, first author of the study.
NAOC’s Dr. “Our research will help better understand future observations from the Full-disk MagnetoGraph, the first Chinese space magnetograph to be the main payload on the ASO-S scientific satellite,” said Yang Shangbin. Study.
Chief Scientist of the Huairou Solar Observing Station (HSOS), Prof. “In the future, we will extend this method to the disintegration of the spiral during solar flares,” said Zhang Mei.
HSOS is one of NAOC’s key stations. It was founded by academician AI Guoxiang in 1984 and is located on an island near the north shore of the Huairou Reservoir. The primary scientific purpose of the station is to measure and study solar magnetic and velocity fields at various heights of the solar atmosphere.