Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics
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 magneti...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad21fd |
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| author | E. M. Wraback A. P. Hoffmann W. B. Manchester IV I. V. Sokolov B. van der Holst D. Carpenter |
| author_facet | E. M. Wraback A. P. Hoffmann W. B. Manchester IV I. V. Sokolov B. van der Holst D. Carpenter |
| author_sort | E. M. Wraback |
| collection | DOAJ |
| description | 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. |
| first_indexed | 2024-03-07T23:29:28Z |
| format | Article |
| id | doaj.art-3c68b4af6b8a4640bd99b1b177c3503d |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-07T23:29:28Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-3c68b4af6b8a4640bd99b1b177c3503d2024-02-20T16:42:38ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01962218210.3847/1538-4357/ad21fdSimulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned MagnetohydrodynamicsE. M. Wraback0https://orcid.org/0009-0007-6235-4057A. P. Hoffmann1https://orcid.org/0000-0003-2477-2761W. B. Manchester IV2https://orcid.org/0000-0003-0472-9408I. V. Sokolov3https://orcid.org/0000-0002-6118-0469B. van der Holst4https://orcid.org/0000-0001-5260-3944D. Carpenter5https://orcid.org/0000-0002-0301-1341Climate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAClimate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAClimate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAClimate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAClimate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAClimate and Space Sciences and Engineering, University of Michigan , Ann Arbor, MI 48109, USAWe 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.https://doi.org/10.3847/1538-4357/ad21fdSolar coronaHydrodynamical simulationsSolar wind |
| spellingShingle | E. M. Wraback A. P. Hoffmann W. B. Manchester IV I. V. Sokolov B. van der Holst D. Carpenter Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics The Astrophysical Journal Solar corona Hydrodynamical simulations Solar wind |
| title | Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics |
| title_full | Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics |
| title_fullStr | Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics |
| title_full_unstemmed | Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics |
| title_short | Simulating Compressive Stream Interaction Regions during Parker Solar Probe’s First Perihelion Using Stream-aligned Magnetohydrodynamics |
| title_sort | simulating compressive stream interaction regions during parker solar probe s first perihelion using stream aligned magnetohydrodynamics |
| topic | Solar corona Hydrodynamical simulations Solar wind |
| url | https://doi.org/10.3847/1538-4357/ad21fd |
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