A coronal hole and its identification as the source of a high velocity solar wind stream

Krieger, A. S.; Timothy, A. F.; Roelof, E. C.

doi:10.1007/bf00150828

Cited by 725 publications

(409 citation statements)

References 23 publications

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“…It was discovered during the 1970s from Skylab data that high-speed solar wind streams originate from large coronal holes (Krieger et al, 1973;Nolte et al, 1976;Zirker, 1977). Wang and Sheeley Jr (1990) investigated the empirical relationship between solar wind speed patterns and the magnetic field structure at the solar wind source location.…”

Section: Relationship Between Coronal Hole Structure and Solar Wind Smentioning

confidence: 99%

Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

100

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This review describes observations of the polar magnetic fields, models for the cyclical formation and decay of these fields, and evidence of their great influence in the solar atmosphere. The polar field distribution dominates the global structure of the corona over most of the solar cycle, supplies the bulk of the interplanetary magnetic field via the polar coronal holes, and is believed to provide the seed for the creation of the activity cycle that follows. A broad observational knowledge and theoretical understanding of the polar fields is therefore an essential step towards a global view of solar and heliospheric magnetic fields. Analyses of both high-resolution and long-term synoptic observations of the polar fields are summarized. Models of global flux transport are reviewed, from the initial phenomenological and kinematic models of Babcock and Leighton to present-day attempts to produce time-dependent maps of the surface magnetic field and to explain polar field variations, including the weakness of the cycle 23 polar fields. The relevance of the polar fields to solar physics extends far beyond the surface layers from which the magnetic field measurements usually derive. As well as discussing the polar fields' role in the interior as seed fields for new solar cycles, the review follows their influence outward to the corona and heliosphere. The global coronal magnetic structure is determined by the surface magnetic flux distribution, and is dominated on large scales by the polar fields. We discuss the observed effects of the polar fields on the coronal hole structure, and the solar wind and ejections that travel through the atmosphere. The review concludes by identifying gaps in our knowledge, and by pointing out possible future sources of improved observational information and theoretical understanding of these fields. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: Relationship Between Coronal Hole Structure and Solar Wind Smentioning

confidence: 99%

Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

100

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“…Krieger et al 1973). The only significant features are low-contrast, largely radial structures within the coronal holes known as polar plumes.…”

Section: ) Driven By Micro-streams Of Several Tens Of Km S -•mentioning

confidence: 99%

Evidence of a solar origin for pressure balance structures in the high‐latitude solar wind

Reisenfeld

McComas

Steinberg

1999

Geophysical Research Letters

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“…The class of storms driven by corotating interaction regions (CIRs) originating at coronal holes on the Sun [Krieger et al, 1973;Tsurutani et al, 2006] is especially interesting because while they are generally weaker storms, they often result in more efficient coupling into the Earth's magnetosphere [Turner et al, 2006].…”

Section: Introductionmentioning

confidence: 99%

Evolution of CIR storm on 22 July 2009

et al. 2012

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[1] Global images of ion intensities are deconvolved from TWINS ENA images during the main and recovery phase of a CIR storm on 22 July 2009. The global spatial ion images taken at different times, along with solar wind data, geomagnetic activity indices, geosynchronous orbit observations, and in situ measurements from the THEMIS mission provide a picture of the evolution of the ring current during both the main phase and early recovery phase of the storm. Major features of the evolution are consistent with expectations based upon time dependent geomagnetic indices, e.g., SYM/H and ASY/H, and geosynchronous orbit detection of dipolarizations from GOES 11 and 12. Direct comparisons are made with in situ THEMIS ESA and SST spectral measurements. The peak energy of the ion spectrum in the ring current is seen to decrease in the recovery phase. The time evolution of the ion energy spectra over the range from 2.5 to 97.5 keV at the spatial peaks of the ring current in the inner magnetosphere obtained from ENA images is presented for the first time.

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A coronal hole and its identification as the source of a high velocity solar wind stream

Cited by 725 publications

References 23 publications

Solar Magnetism in the Polar Regions

Solar Magnetism in the Polar Regions

Evidence of a solar origin for pressure balance structures in the high‐latitude solar wind

Evolution of CIR storm on 22 July 2009

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