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I prove our turbulence transport models admit a conservation representation that resembles the well known WKB transport equation for Alfvén wave energy density after introducing appropriate definitions of the “pressure” associated with the turbulent fluctuations.
I prove our turbulence transport models admit a conservation representation that resembles the well known WKB transport equation for Alfvén wave energy density after introducing appropriate definitions of the “pressure” associated with the turbulent fluctuations.
Wang, B-B., et al. "On the Conservation of Turbulence Energy in Turbulence Transport Models." The Astrophysical Journal 928.2 (2022): 176.
The self-generated turbulent magnetic field is much stronger than both the large-scale magnetic field and the preexisting turbulent magnetic field at the shock of supernova remenants. The resulting CR diffusion coefficient (as shown in the Left panel) is substantially suppressed and is more than three orders smaller near the shock than it is far upstream.
The self-generated turbulent magnetic field is much stronger than both the large-scale magnetic field and the preexisting turbulent magnetic field at the shock of supernova remenants. The resulting CR diffusion coefficient (as shown in the Left panel) is substantially suppressed and is more than three orders smaller near the shock than it is far upstream.
Wang, B-B., et al. "Turbulent Cosmic Ray–Mediated Shocks in the Hot Ionized Interstellar Medium." The Astrophysical Journal 932.1 (2022): 65.
First time to illustate that the adiabatic heating can significantly increase the energy of PUIs in the heliosheath on the way to the heliopause. The resulting spectrum of energetic neutral atoms are different from that when the adiabatic heating is ignored (compare the long-dash-dot line and dashed line in the left panel).
First time to illustate that the adiabatic heating can significantly increase the energy of PUIs in the heliosheath on the way to the heliopause. The resulting spectrum of energetic neutral atoms are different from that when the adiabatic heating is ignored (compare the long-dash-dot line and dashed line in the left panel).
Wang, Bingbing, et al. "Relating energetic ion spectra to energetic neutral atoms." The Astrophysical Journal 944.2 (2023): 198.
Investigate the temporal and spatial variation in the strength of low-frequency turbulence driven by PUIs from 1998 to 2020. The driving rate is stronger during periods of high solar activity and at lower latitudes in the outer heliosphere. The driving rates for parallel and anti-parallel propagating (relative to the background magnetic field) slab turbulence have different spatial and latitude dependences.
Investigate the temporal and spatial variation in the strength of low-frequency turbulence driven by PUIs from 1998 to 2020. The driving rate is stronger during periods of high solar activity and at lower latitudes in the outer heliosphere. The driving rates for parallel and anti-parallel propagating (relative to the background magnetic field) slab turbulence have different spatial and latitude dependences.
Wang, Bingbing, et al. "The temporal and latitudinal dependence of turbulence driven by pickup ions (PUIs) in the outer heliosphere." Frontiers in Astronomy and Space Sciences 10: 1298577.
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