A Model for the Sources of the Slow Solar Wind

Antiochos, S. K.; Mikić, Z.; Titov, V. S.; Lionello, R.; Linker, J. A.

doi:10.1088/0004-637x/731/2/112

Cited by 278 publications

(338 citation statements)

References 64 publications

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“…This is in some ways similar to the S-web model 62 proposed to explain the high latitudes at which the slow solar wind is observed. In this model, a complex web of QSLs (resulting from deformations of the coronal hole boundary) surround the heliospheric neutral sheet and are proposed as likely sites for reconnection.…”

Section: Discussionsupporting

confidence: 82%

Dynamic topology and flux rope evolution during non-linear tearing of 3D null point current sheets

Wyper

Pontin

2014

Physics of Plasmas

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Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. In this work, the dynamic magnetic field within a tearing-unstable three-dimensional current sheet about a magnetic null point is described in detail. We focus on the evolution of the magnetic null points and flux ropes that are formed during the tearing process. Generally, we find that both magnetic structures are created prolifically within the layer and are non-trivially related. We examine how nulls are created and annihilated during bifurcation processes, and describe how they evolve within the current layer. The type of null bifurcation first observed is associated with the formation of pairs of flux ropes within the current layer. We also find that new nulls form within these flux ropes, both following internal reconnection and as adjacent flux ropes interact. The flux ropes exhibit a complex evolution, driven by a combination of ideal kinking and their interaction with the outflow jets from the main layer. The finite size of the unstable layer also allows us to consider the wider effects of flux rope generation. We find that the unstable current layer acts as a source of torsional magnetohydrodynamic waves and dynamic braiding of magnetic fields. The implications of these results to several areas of heliophysics are discussed. V C 2014 AIP Publishing LLC.

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Section: Discussionsupporting

confidence: 82%

Dynamic topology and flux rope evolution during non-linear tearing of 3D null point current sheets

Wyper

Pontin

2014

Physics of Plasmas

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“…The CoMP observations we have presented demonstrate how discrepancies between observations and the empirically-predicted solar wind speed could at least partially arise from an underestimate of magnetic expansion and null-point height by the PFSS model due to intrinsic limitations of photospheric extrapolations. It is also possible that reconnections at the open-closed magnetic boundary rather than flux-tube expansion is the dominant physical process controlling the solar wind speed associated with pseudostreamers, as has been argued in other models (e.g., Antiochos et al (2011);Del Zanna et al (2011)). These models too require accurate determination of coronal magnetic topology, in particular magnetic null point location.…”

Section: Discussionmentioning

confidence: 85%

Magnetic Nulls and Super-radial Expansion in the Solar Corona

Gibson

Dalmasse

Rachmeler

et al. 2017

ApJL

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Magnetic fields in the sun's outer atmosphere -the corona -control both solar-wind acceleration and the dynamics of solar eruptions. We present the first clear observational evidence of coronal magnetic nulls in off-limb linearly polarized observations of pseudostreamers, taken by the Coronal Multichannel Polarimeter (CoMP) telescope. These nulls represent regions where magnetic reconnection is likely to act as a catalyst for solar activity. CoMP linearpolarization observations also provide an independent, coronal proxy for magnetic expansion into the solar wind, a quantity often used to parameterize and predict the solar wind speed at Earth. We introduce a new method for explicitly calculating expansion factors from CoMP coronal linear-polarization observations, which does not require photospheric extrapolations. We conclude that linearly-polarized light is a powerful new diagnostic of critical coronal magnetic topologies and the expanding magnetic flux tubes that channel the solar wind.

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“…Einaudi et al 2001;Lapenta and Knoll, 2005;Antiochos et al 2011) or may be composed of two components, one transient and one resulting from a continual wind flow heated and accelerated for instance by wave-particle interactions at highly expanded flux tubes (e.g. ).…”

Section: Discussionmentioning

confidence: 99%

Observational Evidence for the Associated Formation of Blobs and Raining Inflows in the Solar Corona

Sanchez-Diaz

Rouillard

Davies

et al. 2017

ApJL

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The origin of the slow solar wind is still a topic of much debate. The continual emergence of small transient structures from helmet streamers is thought to constitute one of the main sources of the slow wind. Determining the height at which these transients are released is an important factor in determining the conditions under which the slow solar wind forms. To this end, we have carried out a multipoint analysis of small transient structures released from a north-south tilted helmet streamer into the slow solar wind over a broad range of position angles during Carrington Rotation 2137. Combining the remote-sensing observations taken by the Solar-TErrestrial RElations Observatory (STEREO) mission with coronagraphic observations from the Solar and Heliospheric Observatory (SoHO) spacecraft, we show that the release of such small transient structures (often called blobs), which subsequently move away from the Sun, is associated with the concomitant formation of transient structures collapsing back towards the Sun; the latter have been referred to by previous authors as 'raining inflows'. This is the first direct association between outflowing blobs and raining inflows, which locates the formation of blobs above the helmet streamers and gives strong support that the blobs are released by magnetic reconnection.

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A Model for the Sources of the Slow Solar Wind

Cited by 278 publications

References 64 publications

Dynamic topology and flux rope evolution during non-linear tearing of 3D null point current sheets

Dynamic topology and flux rope evolution during non-linear tearing of 3D null point current sheets

Magnetic Nulls and Super-radial Expansion in the Solar Corona

Observational Evidence for the Associated Formation of Blobs and Raining Inflows in the Solar Corona

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