MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling

Keebler, Timothy B; Tóth, G.; Zieger, B.; Opher, M.

doi:10.3847/1538-4365/ac67eb

Cited by 5 publications

(8 citation statements)

References 42 publications

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“…As a crude estimation, B y and B z can be scaled as 1/r, while the proton density and Bx can be scaled as 1/r 2 . For a more accurate description, a model (e.g., MSWIM2D by Keebler et al 2022) is needed to propagate the solar wind from 1 to 1.3 au. As this study focuses on the cometary magnetospheric response to an extreme CME, it is not critical to scale the solar wind observations to the exact same heliocentric distance.…”

Section: Methodsmentioning

confidence: 99%

Interaction between a Coronal Mass Ejection and Comet 67P/Churyumov–Gerasimenko

Huang,

Tóth,

Gombosi

et al. 2024

ApJ

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The interaction between a coronal mass ejection (CME) and a comet has been observed several times by in situ observations from the Rosetta Plasma Consortium, which is designed to investigate the cometary magnetosphere of comet 67P/Churyumov–Gerasimenko (CG). Goetz et al. reported a magnetic field of up to 300 nT measured in the inner coma, which is among the largest interplanetary magnetic fields observed in the solar system. They suggested the large magnetic field observations in the inner coma come from magnetic field pileup regions, which are generated by the interaction between a CME and/or corotating interaction region and the cometary magnetosphere. However, the detailed interaction between a CME and the cometary magnetosphere of comet CG in the inner coma has not been investigated by numerical simulations yet. In this paper, we will use a numerical model to simulate the interaction between comet CG and a Halloween class CME and investigate its magnetospheric response to the CME. We find that the plasma structures change significantly during the CME event, and the maximum value of the magnetic field strength is more than 500 nT close to the nucleus. Virtual satellites at similar distances as Rosetta show that the magnetic field strength can be as large as 250 nT, which is slightly less than what Goetz et al. reported.

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Section: Methodsmentioning

confidence: 99%

Interaction between a Coronal Mass Ejection and Comet 67P/Churyumov–Gerasimenko

Huang,

Tóth,

Gombosi

et al. 2024

ApJ

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“…ACR intensities did not change at the TS, but slowly increased as the spacecraft moved deeper into the HS (Decker et al, 2010). Hypotheses for the ACR acceleration mechanism and location are: 1) in the flanks of the TS (Cummings et al, 2008); 2) in "hot spots" along a turbulent TS (McComas & Schwadron, 2006;Kota, 2010); 3) by reconnection (Guo et al, 2010;Opher et al, 2011;Keebler et al, 2022); 4) by turbulence processes (Zank et al, 2015); 5) by second-order Fermi acceleration; and 5) by turbulence generated by multi-ion magnetosonic waves (Dialynas et al, 2020). Knowledge Gap: We need to understand where and how ACRs are accelerated.…”

Section: Rt43 Acceleration Of Anomalous Cosmic Rays (Acrs)mentioning

confidence: 96%

“…Interplanetary shocks observed by NH will be simulated using PIC simulations (Swisdak, Drake) (Drake et al, 2010) and multi-ion fluid simulations (Zieger, Keebler) (Zieger et al, 2015;2020). Turbulence parameters will be constrained by Voyager (Fraternale et al, 2019) (Richardson, Szabo) and NH (Keebler et al, 2022) data (Elliott, Hill). Outcome: SHIELD will predict the PUI spectra upstream of the TS for input into global MHD models and production of ENA maps.…”

Section: Rt21 Pui Evolution In the Supersonic Solar Windmentioning

confidence: 99%

Solar wind with Hydrogen Ion charge Exchange and Large-Scale Dynamics (SHIELD) DRIVE Science Center

Opher,

Richardson,

Zank

et al. 2023

Front. Astron. Space Sci.

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Most stars generate winds and move through the interstellar medium that surrounds them. This movement creates a cocoon formed by the deflection of these winds that envelops and protects the stars. We call these “cocoons” astrospheres. The Sun has its own cocoon, the heliosphere. The heliosphere is an immense shield that protects the Solar System from harsh, galactic radiation. The radiation that enters the heliosphere affects life on Earth as well as human space exploration. Galactic cosmic rays are the dominant source of radiation and principal hazard affecting space missions within our Solar System. Current global heliosphere models do not successfully predict the radiation environment at all locations or under different solar conditions. To understand the heliosphere’s shielding properties, we need to understand its structure and large-scale dynamics. A fortunate confluence of missions has provided the scientific community with a treasury of heliospheric data. However, fundamental features remain unknown. The vision of the Solar wind with Hydrogen Ion charge Exchange and Large-Scale Dynamics (SHIELD) DRIVE Science Center is to understand the nature and structure of the heliosphere. Through four integrated research thrusts leading to the global model, SHIELD will: 1) determine the global nature of the heliosphere; 2) determine how pickup ions evolve from “cradle to grave” and affect heliospheric processes; 3) establish how the heliosphere interacts with and influences the Local Interstellar Medium (LISM); and 4) establish how cosmic rays are filtered by and transported through the heliosphere. The key deliverable is a comprehensive, self-consistent, global model of the heliosphere that explains data from all relevant in situ and remote observations and predicts the radiation environment. SHIELD will develop a “digital twin” of the heliosphere capable of: (a) predicting how changing solar and LISM conditions affect life on Earth, (b) understanding the radiation environment to support long-duration space travel, and (c) contributing toward finding life elsewhere in the Galaxy. SHIELD also will train the next-generation of heliophysicists, a diverse community fluent in team science and skilled working in highly transdisciplinary collaborative environments.

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“…Interplanetary shocks observed by NH will be simulated using PIC simulations (Swisdak, Drake) (Drake et al, 2010) and multi-ion fluid simulations (Zieger, Keebler) (Zieger et al, 2015;. Turbulence parameters will be constrained by Voyager (Fraternale et al, 2019) (Richardson, Szabo) and NH (Keebler et al, 2022) data (Elliott, Hill). Outcome: SHIELD will predict the PUI spectra upstream of the TS for input into global MHD models and production of ENA maps.…”

Section: Rt21 Pui Evolution In the Supersonic Solar Windmentioning

confidence: 99%

Reviews in astronomy and space sciences

2024

Frontiers Research Topics

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MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling

Cited by 5 publications

References 42 publications

Interaction between a Coronal Mass Ejection and Comet 67P/Churyumov–Gerasimenko

Interaction between a Coronal Mass Ejection and Comet 67P/Churyumov–Gerasimenko

Solar wind with Hydrogen Ion charge Exchange and Large-Scale Dynamics (SHIELD) DRIVE Science Center

Reviews in astronomy and space sciences

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