Controlling Influence of Magnetic Field on Solar Wind Outflow: An Investigation Using Current Sheet Source Surface Model

Poduval, B.

doi:10.3847/2041-8205/827/1/l6

Cited by 20 publications

(16 citation statements)

References 23 publications

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“…We used the CSSS model (Zhao & Hoeksema 1995;Poduval & Zhao 2014;Poduval 2016;Jackson et al 2019) of the corona in magnetostatic equilibrium (Bogdan & Low 1986). The analytical solutions (Bogdan & Low 1986) incorporate volume and sheet currents effectively (see Zhao & Hoeksema 1995 and the references therein) by dividing the corona into three regions separated by two concentric spherical surfaces: the inner surface, the cusp surface (associated with the cusps of helmet streamers) placed at around 2.5 R s , and the outer source surface (Figure1 in Zhao & Hoeksema 1995) placed at ∼15R s .…”

Section: Appendix B Csss Modelmentioning

confidence: 99%

Seed Population Preconditioning and Acceleration Observed by the Parker Solar Probe

Schwadron

Bale

Bonnell

et al. 2020

ApJS

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A series of solar energetic particle (SEP) events was observed by the Integrated Science Investigation of the Sun (ISeIS) on the Parker Solar Probe (PSP) during the period from 2019 April 18 through 24. The PSP spacecraft was located near 0.48 au from the Sun on Parker spiral field lines that projected out to 1 au within ∼25°of the near-Earth spacecraft. These SEP events, though small compared to historically large SEP events, were among the largest observed thus far in the PSP mission and provide critical information about the space environment inside 1 au during SEP events. During this period, the Sun released multiple coronal mass ejections (CMEs). One of these CMEs observed was initiated on 2019 April 20 at 01:25 UTC, and the interplanetary CME (ICME) propagated out and passed over the PSP spacecraft. Observations by the Electromagnetic Fields Investigation show that the magnetic field structure was mostly radial throughout the passage of the compression region and the plasma that followed, indicating that PSP did not directly observe a flux rope internal to the ICME, consistent with the location of PSP on the ICME flank. Analysis using relativistic electrons observed near Earth by the Electron, Proton and Alpha Monitor on the Advanced Composition Explorer demonstrates the presence of electron seed populations (40-300 keV) during the events observed. The energy spectrum of the ISeIS-observed proton seed population below 1 MeV is close to the limit of possible stationary-state plasma distributions out of equilibrium. ISeISobservations reveal the enhancement of seed populations during the passage of the ICME, which likely indicates a key part of the preacceleration process that occurs close to the Sun.

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Section: Appendix B Csss Modelmentioning

confidence: 99%

Seed Population Preconditioning and Acceleration Observed by the Parker Solar Probe

Schwadron

Bale

Bonnell

et al. 2020

ApJS

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“…These values from the 3‐D model also provide the output of solar wind speed and density at Earth. As the IPS observations do not provide information on the magnetic field for the reconstruction method of the solar wind, the magnetic field in the model is obtained from an extrapolation of the photospheric magnetic field using the CSSS model (Poduval, 2016; Poduval & Zhao, 2014; Zhao & Hoeksema, 1995), which is then advected with the stream in the model (Dunn et al, 2005). In this study, we use output from the UCSD CAT model, which was run by UCSD to provide solar wind forecasts up to 5 days ahead.…”

Section: Methodsmentioning

confidence: 99%

“…A number of simulation methods for reconstructing the coronal magnetic field (that can also be used in ENLIL) from observations have been developed in recent years. The methods use some form of simplification and parameterization, most notably the Potential Field Source Surface (PFSS) method (Altschuler & Newirk, 1969; Nikolic, 2017; Schatten et al, 1969), the magnetofrictional (MF) method (van Ballegooijen et al, 2000; Yang et al, 1986; Yeates et al, 2008), and the Current Sheet Source Surface (CSSS) method (Poduval & Zhao, 2014; Poduval, 2016; Zhao & Hoeksema, 1995). For the outer corona (beyond a source surface of, for example, r > 2.5 R ⊙ where the magnetic field is assumed to be fully radial; see also Nikolic, 2017), the Schatten Current Sheet (SCS) method (Schatten, 1972) is commonly employed.…”

Section: Introductionmentioning

confidence: 99%

Impact of Inner Heliospheric Boundary Conditions on Solar Wind Predictions at Earth

Gonzi

Weinzierl

Bocquet³

et al. 2021

Space Weather

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Predictions of the physical parameters of the solar wind at Earth are at the core of operational space weather forecasts. Such predictions typically use line‐of‐sight observations of the photospheric magnetic field to drive a heliospheric model. The models Wang‐Sheeley‐Arge (WSA) and ENLIL for the transport in the heliosphere are commonly used for these respective tasks. Here we analyze the impact of replacing the potential field coronal boundary conditions from WSA with two alternative approaches. The first approach uses a more realistic nonpotential rather than potential approach, based on the Durham Magneto Frictional Code (DUMFRIC) model. In the second approach the ENLIL inner boundary conditions are based on Inter Planetary Scintillation observations (IPS). We compare predicted solar wind speed, plasma density, and magnetic field magnitude with observations from the WIND spacecraft for two 6‐month intervals in 2014 and 2016. Results show that all models tested produce fairly similar output when compared to the observed time series. This is not only reflected in fairly low correlation coefficients (<0.3) but also large biases. For example, for solar wind speed some models have average biases of more than 150 km/s. On a positive note, the choice of coronal magnetic field model has a clear influence on the model results when compared to the other models in this study. Simulations driven by IPS data have a high success rate with regard to detection of the high speed solar wind. Our results also indicate that model forecasts do not degrade for longer forecast times.

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“…We used the CSSS model (Zhao & Hoeksema 1995;Poduval & Zhao 2014;Poduval 2016;Jackson et al 2019) of the corona in magnetostatic equilibrium (Bogdan & Low 1986). The analytical solutions (Bogdan & Low 1986) incorporate volume and sheet currents effectively (see Zhao & Hoeksema 1995 and the references therein) by dividing the corona into three regions separated by two concentric spherical surfaces: the inner surface, the cusp surface (associated with the cusps of helmet streamers) placed at around 2.5 R s , and the outer source surface The CSSS model extrapolates the observed photospheric magnetic field to obtain the coronal magnetic field.…”

Section: Appendix B Csss Modelmentioning

confidence: 99%

Seed Population Pre-Conditioning and Acceleration Observed by Parker Solar Probe

Schwadron¹,

Bale²,

Bonnell³

et al. 2020

Preprint

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<p>A series of solar energetic particle (SEP) events were observed at Parker Solar Probe (PSP) by the Integrated Science Investigation of the Sun (IS&#9737;IS) during the period from April 18, 2019 through April 24, 2019. The PSP spacecraft was located near 0.48 au from the Sun on Parker spiral field lines that projected out to 1 au within &#8764;25<strong>&#176;</strong> of near Earth spacecraft. These SEP events, though small compared to historically large SEP events, were amongst the largest observed thus far in the PSP mission and provide critical information about the space environment inside 1 au during SEP events. During this period the Sun released multiple coronal mass ejections (CMEs). One of these CMEs observed was initiated on April 20, 2019 at 01:25 UTC, and the interplanetary CME (ICME) propagated out and passed over the PSP spacecraft. Observations by the Electromagnetic Fields Investigation (FIELDS) show that the magnetic field structure was mostly radial throughout the passage of the compression region and the plasma that followed, indicating that PSP did not directly observe a flux rope internal to the ICME, consistent with the location of PSP on the flank of the ICME. Analysis using relativistic electrons observed near Earth by the Electron, Proton and Alpha Monitor (EPAM) on the Advanced Composition Explorer (ACE) demonstrates the presence of flare-accelerated seed populations during the events observed. The energy spectrum of the IS&#9737;IS observed seed population below 1 MeV is consistent with the superposition of acceleration processes near the limit of plasma stability. IS&#9737;IS observations reveal the compression and acceleration of seed populations during the passage of the ICME, which is likely a key part of the pre-acceleration process that occurs close to the Sun and pre-conditions the energetic particle acceleration process.</p>

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Controlling Influence of Magnetic Field on Solar Wind Outflow: An Investigation Using Current Sheet Source Surface Model

Cited by 20 publications

References 23 publications

Seed Population Preconditioning and Acceleration Observed by the Parker Solar Probe

Seed Population Preconditioning and Acceleration Observed by the Parker Solar Probe

Impact of Inner Heliospheric Boundary Conditions on Solar Wind Predictions at Earth

Seed Population Pre-Conditioning and Acceleration Observed by Parker Solar Probe

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