A Near-half-century Simulation of the Solar Corona

TY - JOUR

T1 - A Near-half-century Simulation of the Solar Corona

AU - Aslanyan, Valentin

AU - Meyer, Karen

AU - Scott, Roger B.

AU - Yeates, Anthony

N1 - Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

PY - 2024/1/20

Y1 - 2024/1/20

N2 - We present an overview of results from a magnetofrictional model of the entire solar corona over a period of 47 yr. The simulation self-consistently reproduces decades of solar phenomena, varying in duration between rapid eruptions and the long-term solar cycles, from an input of observed active regions emerging at the photosphere. We have developed a geometric approach to use magnetic helicity to identify and localize the frequent eruptions that occur in the simulation. This method allows us to match our results to extreme-ultraviolet observations of transient events. We have analyzed the evolving magnetic topology by computing the squashing factor and segmenting the corona into discrete magnetic domains bounded by the Separatrix-Web. The simulations show a more dynamic structure to the Separatrix-Web than is predicted by potential field models, which may explain solar wind observations.

AB - We present an overview of results from a magnetofrictional model of the entire solar corona over a period of 47 yr. The simulation self-consistently reproduces decades of solar phenomena, varying in duration between rapid eruptions and the long-term solar cycles, from an input of observed active regions emerging at the photosphere. We have developed a geometric approach to use magnetic helicity to identify and localize the frequent eruptions that occur in the simulation. This method allows us to match our results to extreme-ultraviolet observations of transient events. We have analyzed the evolving magnetic topology by computing the squashing factor and segmenting the corona into discrete magnetic domains bounded by the Separatrix-Web. The simulations show a more dynamic structure to the Separatrix-Web than is predicted by potential field models, which may explain solar wind observations.

KW - Solar physics

KW - Solar corona

KW - Solar prominences

KW - Solar coronal mass ejections

KW - Solar cycle

U2 - 10.3847/2041-8213/ad1934

DO - 10.3847/2041-8213/ad1934

M3 - Article

SN - 2041-8205

VL - 961

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L3

ER -