The Solar Eclipse of 2006 and the Origin of Raylike Features in the White‐Light Corona

Wang, Y. M.; Biersteker, John B.; Sheeley, N. R.; Koutchmy, S.; Mouette, J.; Druckmüller, Miloslav

doi:10.1086/512480

Cited by 71 publications

(57 citation statements)

References 66 publications

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“…Their data allowed us to follow plumes from the low corona (via, for instance, the SOHO/EIT telescope -see Delaboudinière et al, 1995 -that has a Field of View of approximately 1.5 ⊙ ) to far out in the corona, via e.g., the SOHO/LASCO C2 and C3 coronagraphs (Brueckner et al, 1995) that acquire WL images of the corona out to 30 ⊙ . Studies by DeForest et al (1997), DeForest et al (2001b), and Wang et al (2007a) where the base of plumes is identified via SOHO data, confirmed the continuity of plumes and WL rays. However, analogously using data from SOHO/EIT and LASCO, e.g., Llebaria et al (1998), conclude that plumes and ray are distinct phenomena.…”

Section: Introductionmentioning

confidence: 69%

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: Introductionmentioning

confidence: 69%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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“…A fraction of the magnetic flux will remain in the equatorial region, forming a smaller streamer (Figure 3, second panel, t 2 ). The rest of the magnetic flux reconnects and forms new plume/pseudostreamer structures at mid-latitudes (as in Pinto et al 2010 andWang et al 2007). The letter B indicates the pseudo-streamer position.…”

Section: Coronal Magnetic Fieldmentioning

confidence: 91%

Coupling the Solar Dynamo and the Corona: Wind Properties, Mass, and Momentum Losses During an Activity Cycle

Pinto

Brun

Jouve

et al. 2011

ApJ

112

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We study the connections between the Sun's convection zone and the evolution of the solar wind and corona. We let the magnetic fields generated by a 2.5-dimensional (2.5D) axisymmetric kinematic dynamo code (STELEM) evolve in a 2.5D axisymmetric coronal isothermal magnetohydrodynamic code (DIP). The computations cover an 11 year activity cycle. The solar wind's asymptotic velocity varies in latitude and in time in good agreement with the available observations. The magnetic polarity reversal happens at different paces at different coronal heights. Overall the Sun's mass-loss rate, momentum flux, and magnetic braking torque vary considerably throughout the cycle. This cyclic modulation is determined by the latitudinal distribution of the sources of open flux and solar wind and the geometry of the Alfvén surface. Wind sources and braking torque application zones also vary accordingly.

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“…5 and 6 that the NE streamer centered at position angle 55 degrees can be identified as a "pseudostreamer", because it has two neutral lines within it (Wang et al 2007a). The 2006 eclipse also had a pseudostreamer, but on the SW limb (Wang et al 2007b). The finescale features observed in the (sharpened) eclipse image are also not very emphasized in the simulation, although the simulated magnetic field does contain fine-scale features (see below).…”

Section: The Mhd Model Predictionmentioning

confidence: 99%

Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction

Rusin¹,

Druckmüller

Aniol³

et al. 2010

A&A

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Context. The structure of the white-light and emission solar coronas and their MHD modelling are the context of our work. Aims. A comparison is made between the structure of the solar corona as observed during the 2008 August 1 total eclipse from Mongolia and that predicted by an MHD model. Methods. The model has an improved energy formulation, including the effect of coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and acceleration by Alfvén waves. Results. The white-light corona, which was visible up to 20 solar radii, was of an intermediate type with well-pronounced helmet streamers situated above a chain of prominences at position angles of 48, 130, 241, and 322 degrees. Two polar coronal holes, filled with a plethora of thin polar plumes, were observed. High-quality pictures of the green (530.3 nm, Fe XIV) corona were obtained with the help of two narrow-passband filters (centered at the line itself and the vicinity of 529.1 nm background), with a FWHM of 0.15 nm. Conclusions. The large-scale shape of both the white-light and green corona was found to agree well with that predicted by the model. In this paper we describe the morphological properties of the observed corona, and how it compares with that predicted by the model. A more detailed analysis of the quantitative properties of the corona will be addressed in a future publication.

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The Solar Eclipse of 2006 and the Origin of Raylike Features in the White‐Light Corona

Cited by 71 publications

References 66 publications

Solar Coronal Plumes

Solar Coronal Plumes

Coupling the Solar Dynamo and the Corona: Wind Properties, Mass, and Momentum Losses During an Activity Cycle

Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction

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