Japan Geoscience Union Meeting 2018

Presentation information

[EE] Oral

P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM12] Space Weather, Space Climate, and VarSITI

Thu. May 24, 2018 1:45 PM - 3:15 PM 303 (3F International Conference Hall, Makuhari Messe)

convener:Ryuho Kataoka(National Institute of Polar Research), Antti A Pulkkinen (NASA Goddard Space Flight Center), Kanya Kusano(名古屋大学宇宙地球環境研究所, 共同), Kazuo Shiokawa(Institute for Space-Earth Environmental Research, Nagoya University), Chairperson:Shiokawa Kazuo(Nagoya University)

2:45 PM - 3:00 PM

[PEM12-23] A self-consistent model of the coronal heating and solar wind acceleration including compressible and incompressible heating processes

*Munehito Shoda1, Takaaki Yokoyama1, Takeru Suzuki2 (1.School of Science, University of Tokyo, 2.School of Arts & Sciences, University of Tokyo)

Keywords:Coronal heating, Solar wind acceleration, Alfvén wave turbulence, Parametric decay instability

We propose a novel one-dimensional model that includes both shock and turbulence heating and qualify how these processes contribute to heating the corona and driving the solar wind. Compressible MHD simulations allow us to automatically consider shock formation and dissipation, while turbulent dissipation is modeled via a one-point closure based on Alfvén wave turbulence. Numerical simulations were conducted with different photospheric perpendicular correlation lengths, which is a critical parameter of Alfvén wave turbulence, and different root-mean-square photospheric transverse-wave amplitudes. For the various correlation length, we obtain a low-temperature chromosphere, high-temperature corona, and supersonic solar wind. Our analysis shows that turbulence heating is always dominant when the correlation length is smaller than 1 Mm. This result does not mean that we can ignore the compressibility because the analysis indicates that the compressible waves and their associated density fluctuations enhance the Alfvén wave reflection and therefore the turbulence heating. The density fluctuation and the cross helicity are strongly affected by the correlation length, while the coronal temperature and mass loss rate depend weakly on it.