| Presentation Title: | Linking solar magneto-convection and interplanetary space in realistic MHD simulations |
| Author(s): | Haruhisa Iijima |
Abstract:
We will show recent advancements and related scientific topics of our comprehensive MHD simulations from the upper convection zone to the solar wind acceleration region. The supersonic plasma stream of solar wind is one of the steady backgrounds in interplanetary space. Although the small-scale dynamo and resultant MHD waves by the near-surface thermal convection have been believed to be a primary energetic origin of the solar wind, vast parameter space in the magnetic structure and the wave excitation/transport processes prevented us from understanding a quantitative picture of the Sun-to-Solar-Wind coupling. We have recently performed the first radiative MHD simulation that links solar near-surface magneto-convection and the formation and properties of resultant solar wind, using the numerical code RAMENS (Iijima et al., 2023, ApJL, 951, L47). This approach, which uses realistic simulation with minimum empirical parameters, is one of the possible ways to avoid the curse of dimensionality in modeling solar atmosphere. In this talk, we will present the latest findings on this topic, including the formation of solar coronal holes. We will also discuss a potential collaboration with the state-of-the-art and future instruments.