The Magnetic Landscape of the Sun's Polar Region

Tsuneta, S.; Ichimoto, Kiyoshi; Katsukawa, Y.; Lites, B. W.; Matsuzaki, Keiichi; Nagata, Shinji; Suárez, D. Orozco; Shimizu, Toshifumi; Shimojo, Masataka; Shine, R. A.; Suematsu, Y.; Suzuki, Takeru; Tarbell, T. D.; Title, A. M.

doi:10.1086/592226

Cited by 190 publications

(181 citation statements)

References 43 publications

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“…As in the study by Tsuneta et al (2008), two distinct populations were found in the polar regions, large concentrations that varied with the solar cycle and determined the overall polarities of the polar fields, and smaller concentrations of mixed polarity that appeared to be cycle-invariant. Almost all large patches (> 10 17 Mx) had the same polarity at each pole while the population of smaller patches had approximately balanced flux.…”

Section: High-resolution Observations Of Polar Fieldssupporting

confidence: 52%

“…Using the Hinode Solar Optical Telescope (SOT) Spectro-polarimeter (SP), Tsuneta et al (2008) observed the south polar field on 2007 March 16 when the 0 tilt angle was around −7 ∘ and the south pole was visible on the solar disk from the ecliptic plane. Figure 1 shows a spatial map of the measured magnetic field strength.…”

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

“…Latitudinal lines for 85 ∘ , 80 ∘ , 75 ∘ , and 70 ∘ are shown as large circles, while the plus sign marks the south pole. Image reproduced with permission from Tsuneta et al (2008), copyright by AAS. with filling factor set to 1, and 10.0 G with 50% of stray light taken into account (Tsuneta et al, 2008).…”

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

“…Image reproduced with permission from Tsuneta et al (2008), copyright by AAS. with filling factor set to 1, and 10.0 G with 50% of stray light taken into account (Tsuneta et al, 2008). This estimate of average field strength is roughly consistent with the values derived from lower-resolution synoptic line-of-sight measurements that we will discuss in Section 2.7.…”

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

“…Regrettably, the MWO observations stopped in 2012, but the data series from NSO and WSO continue to the present day. Only since the launch of the Hinode spacecraft in late 2006 have detailed vector maps of the polar magnetic field distribution been possible (Tsuneta et al, 2008), under optimal observing conditions, viz. when the pole is tilted a little (about 7.25 ∘ ) towards us.…”

Section: Introductionmentioning

confidence: 99%

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Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

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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: High-resolution Observations Of Polar Fieldssupporting

confidence: 52%

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

Section: High-resolution Observations Of Polar Fieldsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Solar Magnetism in the Polar Regions

Petrie

2015

Living Rev. Sol. Phys.

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A 17 June 2011 polar jet and its presence in the background solar wind

Jackson

Yang

et al. 2016

JGR Space Physics

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High‐speed jet responses in the polar solar wind are enigmatic. Here we measure a jet response that emanates from the southern polar coronal hole on 17 June 2011 at the extreme speed of over 1200 km/s. This response was recorded from the Sun‐Earth line in Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) and Large Angle and Spectrometric Coronagraph/C2 and both Solar TErrestrial RElations Observatory Extreme Ultraviolet Imager and COR2 coronagraphs when the three spacecraft were situated ~90° from one another. These certify the coronal 3‐D location of the response that is associated with an existing solar plume structure and show its high speed to distances of over 14 RS. This jetting is associated with magnetic flux changes in the polar region as measured by the SDO/Helioseismic and Magnetic Imager instrumentation over a period of several hours. The fastest coronal response observed can be tracked to a time near the period of greatest flux changes and to the onset of the brightest flaring in AIA. This high‐speed response can be tracked directly as a small patch of outward moving brightness in coronal images as in Yu et al. (2014) where three slower events were followed from the perspective of Earth. This accumulated jet response has the largest mass and energy we have yet seen in 3‐D reconstructions from Solar Mass Ejection Imager observations, and its outward motion is certified for the first time using interplanetary scintillation observations. This jet response is surrounded by similar high‐speed patches, but these are smoothed out in Ulysses polar measurements, we speculate about how these dynamic activities relate to solar wind acceleration.

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MHD Wave Modes Resolved in Fine‐Scale Chromospheric Magnetic Structures

Verth¹,

Jess²

2016

Low‐Frequency Waves in Space Plasmas

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Within the last decade, due to significant improvements in the spatial and temporal resolution of chromospheric data, magnetohydrodynamic (MHD) wave studies in this fascinating region of the Sun's atmosphere have risen to the forefront of solar physics research. In this Chapter we begin by reviewing the challenges and debates that have manifested in relation to MHD wave mode identification in finescale chromospheric magnetic structures, including spicules, fibrils and mottles. Next we go on to discuss how the process of accurately identifying MHD wave modes also has a crucial role to play in estimating their wave energy flux. This is of cardinal importance for estimating what the possible contribution of MHD waves is to solar atmospheric heating. Finally, we detail how such advances in chromospheric MHD wave studies have also allowed us, for the first time, to implement cutting-edge magnetoseismological techniques that provide new insight into the subresolution plasma structuring of the lower solar atmosphere.

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The Magnetic Landscape of the Sun's Polar Region

Cited by 190 publications

References 43 publications

Solar Magnetism in the Polar Regions

Solar Magnetism in the Polar Regions

A 17 June 2011 polar jet and its presence in the background solar wind

MHD Wave Modes Resolved in Fine‐Scale Chromospheric Magnetic Structures

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