A Model for the Coupled Eruption of a Pseudostreamer and Helmet Streamer

Wyper, P. F.; Antiochos, S. K.; DeVore, C. R.; Lynch, B. J.; Karpen, J. T.; Kumar, Pankaj

doi:10.3847/1538-4357/abd9ca

Cited by 26 publications

(26 citation statements)

References 62 publications

(83 reference statements)

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“…One possibility for the jet bifurcation is that the jet material simultaneously entered open and closed magnetic field line after the initial null-point reconnection. We notice that a similar jet dynamic process was reported in the recent simulation work from Wyper et al (2021). By projecting the global extrapolated field lines from PFSS model onto STEREO-A EUVI 304 Å image (see Figure 4 (d)), we can found that there are indeed two different system of magnetic field lines, i.e., the green open and the white closed lines.…”

Section: Qfp Wave Train and Cmesupporting

confidence: 81%

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

Duan,

Shen,

Zhou

et al. 2022

Preprint

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Using imaging and radio multi-wavelength observations, we studied the origin of two homologous accelerated electron beams and a quasi-periodic fast-propagating (QFP) wave train associated with a solar jet on 2012 July 14. The jet occurred in a small-scale fan-spine magnetic system embedding in a large-scale pseudostreamer, which associated with a GOES C1.4 flare, a jet-like coronal mass ejection (CME), a type II radio burst, and a type III radio burst. During the initial stage, a QFP wave train and a fast moving on-disk radio source were detected in succession ahead of the jet along the outer spine of the fan-spine system. When the jet reached a height of about 1.3 solar radii, it underwent a bifurcation into two branches. Based on our analysis results, all the observed phenomena in association with the jet can be explained by using a fanspine magnetic system. We propose that both the type III radio burst and the on-disk fast moving radio source were caused by the same physical process, i.e., the energetic electrons accelerated by the magnetic reconnection at the null point, and they were along the open field lines of the pseudostreamer and the closed outer spine of the fanspine structure, respectively. Due to the bifurcation of the jet body, the lower branch along the closed outer spine of the fan-spine structure fell back to the solar surface, while the upper branch along the open field lines of the pseudostreamer caused the jet-like CME in the outer corona.

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Section: Qfp Wave Train and Cmesupporting

confidence: 81%

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

Duan,

Shen,

Zhou

et al. 2022

Preprint

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“…We consider a magnetic geometry in which a coronal hole is isolated at midlatitudes, bounded from the north by a pseudostreamer (see Titov et al 2011 for a complete discussion) and from the south by a portion of the global helmet streamer. To achieve this, a set of magnetic dipoles has been placed so as to create a region of parasitic polarity (see Wyper et al 2021 for further details). The initial magnetic field was computed using a PFSS model and the plasma was initialized with the spherically symmetric, radial, isothermal Parker solar wind solution (Parker 1958).…”

Section: Magnetic Field Geometry and Boundary Conditionsmentioning

confidence: 99%

The Dynamic Coupling of Streamers and Pseudostreamers to the Heliosphere

Aslanyan

Pontin

Higginson

et al. 2022

ApJ

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The slow solar wind is generally believed to result from the interaction of open and closed coronal magnetic flux at streamers and pseudostreamers. We use three-dimensional magnetohydrodynamic simulations to determine the detailed structure and dynamics of open-closed interactions that are driven by photospheric convective flows. The photospheric magnetic field model includes a global dipole giving rise to a streamer together with a large parasitic polarity region giving rise to a pseudostreamer that separates a satellite coronal hole from the main polar hole. Our numerical domain extends out to 30R ⊙ and includes an isothermal solar wind, so that the coupling between the corona and heliosphere can be calculated rigorously. This system is driven by imposing a large set of quasi-random surface flows that capture the driving of coronal flux in the vicinity of streamer and pseudostreamer boundaries by the supergranular motions. We describe the resulting structures and dynamics. Interchange reconnection dominates the evolution at both streamer and pseudostreamer boundaries, but the details of the resulting structures are clearly different from one another. Additionally, we calculate in situ signatures of the reconnection and determine the dynamic mapping from the inner heliosphere back to the Sun for a test spacecraft orbit. We discuss the implications of our results for interpreting observations from inner heliospheric missions, such as Parker Solar Probe and Solar Orbiter, and for space weather modeling of the slow solar wind.

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“…We consider a magnetic geometry in which a coronal hole is isolated at mid latitudes, bounded from the north by a pseudostreamer (see Titov et al (2011) for a complete discussion) and from the south by a portion of the global helmet streamer. To achieve this, a set of magnetic dipoles has been placed so as to create a region of parasitic polarity (see Wyper et al (2021) for further details). The initial magnetic field was computed using a PFSS model and the plasma was initialized with the spherically symmetric, radial, isothermal Parker solar wind solution (Parker 1958).…”

Section: Magnetic Field Geometry and Boundary Conditionsmentioning

confidence: 99%

“…Due to the very weak field in the vicinity of the eastern null, different numbers of nulls are found in that region at different times during the simulations due to small-scale fluctuations (that lead to either a null bifurcation or the emergence of a null through the photosphere). For an in-depth discussion of the topology of our relaxed state see Wyper et al (2021). We evaluate and visualize the magnetic geometry using the squashing factor Q (Titov et al 2002), typically displayed on a plane of constant radius (but always calculated between the solar surface and the outer boundary at R = 30R ).…”

Section: Magnetic Field Geometry and Boundary Conditionsmentioning

confidence: 99%

The Dynamic Coupling of Streamers and Pseudostreamers to the Heliosphere

Aslanyan,

Pontin,

Higginson

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

The slow solar wind is generally believed to result from the interaction of open and closed coronal magnetic flux at streamers and pseudostreamers. We use 3-dimensional magnetohydrodynamic simulations to determine the detailed structure and dynamics of open-closed interactions that are driven by photospheric convective flows. The photospheric magnetic field model includes a global dipole giving rise to a streamer together with a large parasitic polarity region giving rise to a pseudostreamer that separates a satellite coronal hole from the main polar hole. Our numerical domain extends out to 30 solar radii and includes an isothermal solar wind, so that the coupling between the corona and heliosphere can be calculated rigorously. This system is driven by imposing a large set of quasi-random surface flows that capture the driving of coronal flux in the vicinity of streamer and pseudostreamer boundaries by the supergranular motions. We describe the resulting structures and dynamics. Interchange reconnection dominates the evolution at both streamer and pseudostreamer boundaries, but the details of the resulting structures are clearly different from one another. Additionally, we calculate in situ signatures of the reconnection and determine the dynamic mapping from the inner heliosphere back to the Sun for a test spacecraft orbit. We discuss the implications of our results for interpreting observations from inner heliospheric missions, such as Parker Solar Probe and Solar Orbiter, and for space weather modeling of the slow solar wind.

show abstract

A Model for the Coupled Eruption of a Pseudostreamer and Helmet Streamer

Cited by 26 publications

References 62 publications

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

The Dynamic Coupling of Streamers and Pseudostreamers to the Heliosphere

The Dynamic Coupling of Streamers and Pseudostreamers to the Heliosphere

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