Association of Extreme-Ultraviolet Imaging Telescope (EIT) Polar Plumes with Mixed-Polarity Magnetic Network

Wang, Y.-M.; Sheeley, N. R.; Dere, K. P.; Duffin, R. T.; Howard, R. A.; Michels, D. J.; Moses, J. D.; Harvey, J. W.; Branston, D.; Delaboudinière, J. P.; Artzner, G.; Hochedez, J.‐F.; Defise, J. M.; Catura, R. C.; Lemen, J. R.; Gurman, J. B.; Neupert, W. M.; Newmark, Jeffrey; Thompson, B. J.; Maucherat, A.; Clette, F.

doi:10.1086/310773

Cited by 44 publications

(15 citation statements)

References 19 publications

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“…Early observers suggested plumes to be rooted in rosettes, typically found in the network and Newkirk Jr and Harvey (1968), as well as later scientists, claimed the base of plumes corresponds to bright portions of the network (DeForest et al, 1997). Nowadays, we recognize plumes to overlie small bipolar regions within dominant unipolar open field areas (Wang and Sheeley Jr, 1995b;Wang et al, 1997;Wang and Muglach, 2008): indeed the area analyzed by hosted a couple of plumes, located above bright points (as seen in the Si ii line) but no relevant Doppler velocity signature was found to be associated with them. Analogously, Wilhelm et al (2000) found no significant Doppler shift in bright plumes.…”

Section: Plume Outflows In the Low Coronamentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL) images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV) and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features. 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: Plume Outflows In the Low Coronamentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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“…This returns us to the question of whether the proper motions of these two kinds of plumes have a common origin. Wang et al (1997) and Raouafi & Stenborg (2014) have suggested that plumes may be produced during the reconnection between field lines from the unipolar flux concentration and a wandering element of opposite polarity. Although such episodic reconnections may create the occasional jets that occur during the formation of a plume, it seems doubtful that they could be responsible for sustained five to eight minute quasi-periodic motions within the plume.…”

Section: Cellular Plumesmentioning

confidence: 99%

Using Running Difference Images to Track Proper Motions of Xuv Coronal Intensity on the Sun

Sheeley

Warren

Lee

et al. 2014

ApJ

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We have developed a procedure for observing and tracking proper motions of faint XUV coronal intensity on the Sun and have applied this procedure to study the collective motions of cellular plumes and the shorter-period waves in sunspots. Our space/time maps of cellular plumes show a series of tracks with the same 5-8 minute repetition times and ∼100 km s −1 sky-plane speeds found previously in active-region fans and in coronal hole plumes. By synchronizing movies and space/time maps, we find that the tracks are produced by elongated ejections from the unipolar flux concentrations at the bases of the cellular plumes and that the phases of these ejections are uncorrelated from cell to cell. Thus, the large-scale motion is not a continuous flow, but is more like a system of independent conveyor belts all moving in the same direction along the magnetic field. In contrast, the proper motions in sunspots are clearly waves resulting from periodic disturbances in the sunspot umbras. The periods are ∼2.6 minutes, but the sky-plane speeds and wavelengths depend on the heights of the waves above the sunspot. In the chromosphere, the waves decelerate from 35-45 km s −1 in the umbra to 7-8 km s −1 toward the outer edge of the penumbra, but in the corona, the waves accelerate to ∼60-100 km s −1 . Because chromospheric and coronal tracks originate from the same space/time locations, the coronal waves must emerge from the same umbral flashes that produce the chromospheric waves.

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“…Primarily, Send offprint requests to: D. Banerjee, e-mail: dipu@wis.kuleuven.ac.be coronal holes are overwhelmingly unipolar. This fact further suggests that plumes are not the source of the high speed polar wind (Wang et al 1997).…”

Section: Introductionmentioning

confidence: 95%

Long period oscillations in the inter-plume regions of the Sun

Banerjee

O’Shea

Doyle

et al. 2001

A&A

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Abstract. We examine long spectral time series of inter-plume lanes observed on the 14th and 15th March 2000 with the Coronal Diagnostic Spectrometer (CDS) on-board SoHO. The observations were obtained in lines over a wide temperature range, from the chromosphere to the corona. The statistical significance of the oscillations was estimated by using a randomisation method. Our observations indicate the presence of compressional waves with periods of 20-50 min or longer, both off-limb and on-disk and up to 70 min further out to at least 25 arcsec off-limb. To our knowledge this is the first time that long period oscillations in the inter-plume regions close to the limb of the Sun have been detected. We interpret these oscillations as outward propagating slow magneto-acoustic waves which may contribute significantly to the heating of the lower corona by compressive dissipation and which may also provide some of the enough energy flux required for the acceleration of the fast solar wind. These slow waves may have been produced at the network boundaries in the coronal hole.

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Association of Extreme-Ultraviolet Imaging Telescope (EIT) Polar Plumes with Mixed-Polarity Magnetic Network

Cited by 44 publications

References 19 publications

Solar Coronal Plumes

Solar Coronal Plumes

Using Running Difference Images to Track Proper Motions of Xuv Coronal Intensity on the Sun

Long period oscillations in the inter-plume regions of the Sun

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