Abstract
Strong flares and coronal mass ejections (CMEs), launched from -sunspots, are the most catastrophic energy-releasing events in the solar system. The formations of -sunspots and relevant polarity inversion lines (PILs) are crucial for the understanding of flare eruptions and CMEs. In this work, the kink-stable, spot-spot-type -sunspots induced by flux emergence are simulated, under different subphotospheric initial conditions of magnetic field strength, radius, twist, and depth. The time evolution of various plasma variables of the -sunspots are simulated and compared with the observation data, including magnetic bipolar structures, relevant PILs, and temperature. The simulation results show that magnetic polarities display switchbacks at a certain stage and then split into numerous fragments. The simulated fragmentation phenomenon in some -sunspots may provide leads for future observations in the field.
Highlights
Plasma features in solar corona are commonly observed with X-ray and EUV instruments [1,2]
Large-scale magnetic flux emergence from the convection zone creates δ-sunspots and sheared polarity inversion lines (PILs), which are crucial for the understanding of flare eruptions and coronal mass ejections (CMEs) [3,4,16]
Kink-stable, spot-spot-type δ-sunspots induced by flux emergence are simulated, under different subphotospheric initial conditions of magnetic field strength, radius, twist, and depth
Summary
Plasma features in solar corona are commonly observed with X-ray and EUV instruments [1,2]. In [12], the emergence of a magnetic flux tube from the convection zone to the solar atmosphere was simulated by using a 3D MHD model. In [15], emerging magnetic flux tubes with different initial magnetic field strengths, radii, twists, and lengths were simulated by using a 3D MHD model to investigate the effects of these parameters. Large-scale magnetic flux emergence from the convection zone creates δ-sunspots and sheared PILs, which are crucial for the understanding of flare eruptions and CMEs [3,4,16]. Kink-stable, spot-spot-type δ-sunspots induced by flux emergence are simulated, under different subphotospheric initial conditions of magnetic field strength, radius, twist, and depth. The time evolution of δ-sunspots is presented in Section 4, and some conclusions are drawn Section 5
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
