Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona

Szente, J.; Landi, E.; van der Holst, B.

doi:10.3847/1538-4365/ad0232

Cited by 3 publications

(3 citation statements)

References 31 publications

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“…and van der Holst et al (2014) described the physics within AWSoM in great detail, while van der Holst et al (2022) discussed the recent improvement of the Alfvén wave turbulence cascade. AWSoM results have shown reasonable agreement with in situ and remote observations under different solar wind conditions(Jin et al 2012;Oran et al 2013;Sachdeva et al 2019;Sachdeva et al 2021;Szente et al 2022;Huang et al 2023;Szente et al 2023;Shi et al 2024) and were widely used in the community(Jian et al 2016;Lloveras et al 2020;Henadhira Arachchige et al 2022).…”

supporting

confidence: 57%

Adjusting the Potential Field Source Surface Height Based on Magnetohydrodynamic Simulations

Huang,

Tóth,

Huang

et al. 2024

ApJL

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A potential field solution is widely used to extrapolate the coronal magnetic field above the Sun’s surface to a certain height. This model applies the current-free approximation and assumes that the magnetic field is entirely radial beyond the source surface height, which is defined as the radial distance from the center of the Sun. Even though the source surface is commonly specified at 2.5 R s (solar radii), previous studies have suggested that this value is not optimal in all cases. In this study, we propose a novel approach to specify the source surface height by comparing the areas of the open magnetic field regions from the potential field solution with predictions made by a magnetohydrodynamic model, in our case the Alfvén Wave Solar atmosphere Model. We find that the adjusted source surface height is significantly less than 2.5 R s near solar minimum and slightly larger than 2.5 R s near solar maximum. We also report that the adjusted source surface height can provide a better open flux agreement with the observations near the solar minimum, while the comparison near the solar maximum is slightly worse.

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supporting

confidence: 57%

Adjusting the Potential Field Source Surface Height Based on Magnetohydrodynamic Simulations

Huang,

Tóth,

Huang

et al. 2024

ApJL

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“…Multiple modules can be coupled with AWSoM to gain more insight into the underlying physics of the system. For example, spectroscopic images can be made with the SPECTRUM module (Szente et al 2019;Shi et al 2022) and the charge states' composition through the heliosphere can be modeled using the nonequilibrium ionization charge state calculations (Szente et al 2022(Szente et al , 2023.…”

Section: Awsom Modelmentioning

confidence: 99%

Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics

Wraback,

Hoffmann,

Manchester

et al. 2024

ApJ

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We used the stream-aligned magnetohydrodynamics (SA-MHD) model to simulate Carrington rotation 2210, which contains Parker Solar Probe’s (PSP) first perihelion at 36.5 R ⊙ on 2018 November 6, to provide context to the in situ PSP observations by FIELDS and SWEAP. The SA-MHD model aligns the magnetic field with the velocity vector at each point, thereby allowing for clear connectivity between the spacecraft and the source regions on the Sun, without unphysical magnetic field structures. During this Carrington rotation, two stream interaction regions (SIRs) form, due to the deep solar minimum. We include the energy partitioning of the parallel and perpendicular ions and the isotropic electrons to investigate the temperature anisotropy through the compression regions to better understand the wave energy amplification and proton thermal energy partitioning in a global context. Overall, we found good agreement in all in situ plasma parameters between the SA-MHD results and the observations at PSP, STEREO-A, and Earth, including at PSP’s perihelion and through the compression region of the SIRs. In the typical solar wind, the parallel proton temperature is preferentially heated, except in the SIR, where there is an enhancement in the perpendicular proton temperature. This is further showcased in the ion cyclotron relaxation time, which shows a distinct decrease through the SIR compression regions. This work demonstrates the success of the Alfvén wave turbulence theory for predicting interplanetary magnetic turbulence levels, while self-consistently reproducing solar wind speeds, densities, and overall temperatures, including at small heliocentric distances and through SIR compression regions.

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“…It is open-source on GitHub 1 and can also be accessed via the runs-on-request service provided by the Community Coordinated Modeling Center. AWSoM has been extensively validated with in situ and remote observations under different solar wind conditions (Jin et al 2012;Oran et al 2013;Sachdeva et al 2021;Szente et al 2022Szente et al , 2023Huang et al 2023), as well as at different heliocentric distances including Parker Solar Probe locations (van der Holst et al 2019(van der Holst et al , 2022.…”

Section: Introductionmentioning

confidence: 99%

Solar Wind Driven from GONG Magnetograms in the Last Solar Cycle

Huang,

Tóth,

Sachdeva

et al. 2024

ApJ

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In a previous study, Huang et al. used the Alfvén Wave Solar atmosphere Model, one of the widely used solar wind models in the community, driven by ADAPT-GONG magnetograms to simulate the solar wind in the last solar cycle and found that the optimal Poynting flux parameter can be estimated from either the open field area or the average unsigned radial component of the magnetic field in the open field regions. It was also found that the average energy deposition rate (Poynting flux) in the open field regions is approximately constant. In the current study, we expand the previous work by using GONG magnetograms to simulate the solar wind for the same Carrington rotations and determine if the results are similar to the ones obtained with ADAPT-GONG magnetograms. Our results indicate that similar correlations can be obtained from the GONG maps. Moreover, we report that ADAPT-GONG magnetograms can consistently provide better comparisons with 1 au solar wind observations than GONG magnetograms, based on the best simulations selected by the minimum of the average curve distance for the solar wind speed and density.

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Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona

Cited by 3 publications

References 31 publications

Adjusting the Potential Field Source Surface Height Based on Magnetohydrodynamic Simulations

Adjusting the Potential Field Source Surface Height Based on Magnetohydrodynamic Simulations

Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics

Solar Wind Driven from GONG Magnetograms in the Last Solar Cycle

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