Ejection of magnetic fields from the sun - Acceleration of a solar wind containing diamagnetic plasmoids

Pneuman, G. W.

doi:10.1086/160691

Cited by 51 publications

(30 citation statements)

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“…There may be some similarity between these scenarios and older models of diamagnetic acceleration of the solar wind via buoyant plasmoids that may fill some 0fraction of the corona [e.g., Schlüter , 1957; Pneuman , 1986; Mullan , 1990]. The additional momentum deposited by this process is given approximately by an effective buoyancy‐driven pressure gradient where f d is the ratio of mass flux in the plasmoids to the total wind mass flux and w d is the most‐probable speed in the plasmoids [see also Pneuman , 1983; Yang and Schunk , 1989; Tamano , 1991]. Plasmoid inhomogeneities may arise from reconnection events [e.g., Yokoyama and Shibata , 1996] and expand to fill a large fraction of the volume of coronal holes [see also Feldman et al , 1997].…”

Section: Reconnection‐related Plasmoids (Plasma Blobs) In the Solar Amentioning

confidence: 99%

“…where f d is the ratio of mass flux in the plasmoids to the total wind mass flux and w d is the most-probable speed in the plasmoids [see also Pneuman, 1983;Yang and Schunk, 1989;Tamano, 1991]. Plasmoid inhomogeneities may arise from reconnection events [e.g., Yokoyama and Shibata, 1996] and expand to fill a large fraction of the volume of coronal holes [see also Feldman et al, 1997].…”

Section: Mass Flows Of Various Scales In the Solar Windmentioning

confidence: 99%

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Plasmoids in reconnecting current sheets: Solar and terrestrial contexts compared

2008

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Abstract. Magnetic reconnection plays a crucial role in violent energy conversion occurring in the environments of high electrical conductivity, such as the solar atmosphere, magnetosphere, and fusion devices. We focus on the morphological features of the process in two different environments, the solar atmosphere and the geomagnetic tail. In addition to indirect evidence that indicates reconnection in progress or having just taken place, such as auroral manifestations in the magnetosphere and the flare loop system in the solar atmosphere, more direct evidence of reconnection in the solar and terrestrial environments is being collected. Such evidence includes the reconnection inflow near the reconnecting current sheet, and the outflow along the sheet characterized by a sequence of plasmoids. Both turbulent and unsteady Petschek-type reconnection processes could account for the observations. We also discuss other relevant observational consequences of both mechanisms in these two settings. While on face value, these are two completely different physical environments, there emerge many commonalities, for example, an Alfvén speed of the same order of magnitude, a key parameter determining the reconnection rate. This comparative study is meant as a contribution to current efforts aimed at isolating similarities in processes occurring in very different contexts in the heliosphere, and even in the universe.

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Section: Reconnection‐related Plasmoids (Plasma Blobs) In the Solar Amentioning

confidence: 99%

Section: Mass Flows Of Various Scales In the Solar Windmentioning

confidence: 99%

Plasmoids in reconnecting current sheets: Solar and terrestrial contexts compared

2008

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“…These works discussed the evolution of an isolated plasmoid formed during magnetic reconnection. They calculated its motion in a radially diverging magnetic field and argued that the solar wind could be composed of a continuum of such plasmoids [Pneuman, 1983;Mullan, 1990].…”

Section: Modelmentioning

confidence: 99%

A model for accelerated density enhancements emerging from coronal streamers in Large‐Angle and Spectrometric Coronagraph observations

Schmidt¹,

Cargill²

2000

J. Geophys. Res.

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“…Although the nature of the formation and disappearance of quiescent filaments is still unclear, it may be safely suggested that their appearance and disap- ,,,,, , Tl,,,,,,,,i,,,,,r The reason behind this was an enhancement of the role played by unsteady state processes in the formation of high-speed solar wind streams. The plasma acceleration mechanism in this case is similar to the formation mechanism for coronal mass ejections and magnetic clouds [Pneuman, 1983]. Obviously, the most favorable conditions for this would be created in periods of global variations of coronal magnetic fields, with their overall attenuation [Kovalenko, 1988;Gosling, 1993].…”

Section: Phase Of Solar Activitymentioning

confidence: 67%

Heliospheric characteristics during fast global variations of solar magnetic fields

Жеребцов¹,

Kovalenko²,

Molodykh³

1997

J. Geophys. Res.

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Two periods of f•st (covering one or two solar rotations) global variations of solar magnetic fields have been found to exist in each 11-year cycle of solar activity. Solar activity that is determined from commonly employed indices (Wolf numbers, radio flux, etc.) changes little during these periods. These periods are characterized by both an enhancement of flaring activity, which accounts for the fast changes in current, and, accordingly, magnetic structures. One occurs during the rising phase of solar activity and is accompanied by an enhancement of large-scale magnetic fields •nd fast changes in global m•gnetic structure of the corona. In this case, "favorable conditions" are created for an effective acceleration of high-energy solar cosmic rays. The other occurs during the declining phase of solar •ctivity and is characterized by a structural simplification of large-scale magnetic fields and largely by the attenuation of magnetic fields in the corona. The observed significant increase in solar wind mass flux, •n enhancement of the interplanetary m•gnetic field, and anomalously strong geomagnetic disturbances are heliospheric m•nifestations of transient phenomena and processes in the solar corona associated with the dynamics of large-scale m•gnetic fields. This period is most conspicuous in long-term cosmic ray intensity variations, which are analogous to a Forbush decrease. These findings are explained by the commencement and cessation of •n active interaction between magnetic fields of the "old" cycle •nd emerging fields of the "new" cycle, which trigger transient, flare-related, coronal processes. 2137 2138 ZHEREBTSOV ET AL' FAST GLOBAL VARIATIONS OF SOLAR MAGNETIC FIELDS

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Ejection of magnetic fields from the sun - Acceleration of a solar wind containing diamagnetic plasmoids

Cited by 51 publications

References 0 publications

Plasmoids in reconnecting current sheets: Solar and terrestrial contexts compared

Plasmoids in reconnecting current sheets: Solar and terrestrial contexts compared

A model for accelerated density enhancements emerging from coronal streamers in Large‐Angle and Spectrometric Coronagraph observations

Heliospheric characteristics during fast global variations of solar magnetic fields

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