Origin of Streamer Material in the Outer Corona

Wang, Y.-M.; Sheeley, N. R.; Walters, Joshua R.; Brueckner, G. E.; Howard, R. A.; Michels, D. J.; Lamy, P. L.; Schwenn, R.; Simnett, G. M.

doi:10.1086/311321

Cited by 250 publications

(233 citation statements)

References 15 publications

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“…However, we note that the material within the heliospheric plasma sheet most likely originates from closed helmet-streamer loops, being tranferred to the open field region by interchange reconnection (Wang et al 1998;Crooker et al 2004). Our future objective is to extend the numerical code to two and three dimensions, while solving the full MHD equations with consistent dissipative terms.…”

Section: Discussionmentioning

confidence: 99%

Time-dependent hydrodynamical simulations of slow solar wind, coronal inflows, and polar plumes

Pinto¹,

Grappin²,

Wang³

et al. 2009

A&A

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Aims. We explore the effects of varying the areal expansion rate and coronal heating function on the solar wind flow. Methods. We use a one-dimensional, time-dependent hydrodynamical code. The computational domain extends from near the photosphere, where nonreflecting boundary conditions are applied, to 30 R , and includes a transition region where heat conduction and radiative losses dominate. Results. We confirm that the observed inverse relationship between asymptotic wind speed and expansion factor is obtained if the coronal heating rate is a function of the local magnetic field strength. We show that inflows can be generated by suddenly increasing the rate of flux-tube expansion and suggest that this process may be involved in the closing-down of flux at coronal hole boundaries. We also simulate the formation and decay of a polar plume, by including an additional, time-dependent heating source near the base of the flux tube.

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Section: Discussionmentioning

confidence: 99%

Time-dependent hydrodynamical simulations of slow solar wind, coronal inflows, and polar plumes

Pinto¹,

Grappin²,

Wang³

et al. 2009

A&A

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“…The slow solar wind also has different characteristic suprathermal electron anisotropies than the fast solar wind, including less intense heat flux electron beams (Pilipp et al 1987;Ogilvie et al 1999), and sometimes sunward directed anisotropies that indicate magnetic fields folded back toward the Sun (Kahler et al 1984) as well as heat flux dropouts (McComas et al 1989). One suggestion is that the slow wind at least in part consists of transient events from magnetic reconnection at the coronal hole boundaries or the cusps of streamers (e.g., Crooker and Intriligator 1996;Wang et al 1998). The bright blobs observed by SOHO-LASCO emanating from coronal streamers (Sheeley et al 1997) may be visible evidence of this process, but they have proven difficult to identify with in situ measurements.…”

Section: The Relationship Of the 3d Corona To Solar Wind Structurementioning

confidence: 99%

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

et al. 2007

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The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation.

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“…The purpose of this paper is to describe this technique and to show the principal results that we have obtained with it. Some preliminary results have been presented elsewhere [Wang et al, 1998;.…”

Section: Introductionmentioning

confidence: 99%

Continuous tracking of coronal outflows: Two kinds of coronal mass ejections

Sheeley¹,

Walters²,

Wang³

et al. 1999

J. Geophys. Res.

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The statistics improved during the 1980s as the SOLWIND (1979)(1980)(1981)(1982)(1983)(1984)(1985) and SMM (1980,(1984)(1985)(1986)(1987)(1988)(1989) However, there were relatively few systematic studies of acceleration. Despite its large 2.5-10 Rs field of view, the SOLWIND coronagraph had a low spatial resolution (-1.25 arc min) and revealed unambiguous accelerations for only a small number of particularly well observed events [Howard et 24,739

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Origin of Streamer Material in the Outer Corona

Cited by 250 publications

References 15 publications

Time-dependent hydrodynamical simulations of slow solar wind, coronal inflows, and polar plumes

Time-dependent hydrodynamical simulations of slow solar wind, coronal inflows, and polar plumes

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

Continuous tracking of coronal outflows: Two kinds of coronal mass ejections

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