Thermodynamics of the Solar Corona and Evolution of the Solar Magnetic Field as Inferred From the Total Solar Eclipse Observations of 2010 July 11

Habbal, Shadia Rifai; Druckmüller, Miloslav; Morgan, Huw; Ding, A.; Johnson, J.; Druckmüllerová, Hana; Daw, A. N.; Arndt, M. B.; Dietzel, Martin; Saken, Jon M.

doi:10.1088/0004-637x/734/2/120

Cited by 78 publications

(72 citation statements)

References 24 publications

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“…The shape of the open strands shows a diverging pattern, as do the fanlike structures identified in EUV wavelengths in the low corona (Habbal et al 2011;Seaton et al 2013). In addition, at the intersection of the closed and open flux, we notice a thin extended region that becomes brighter and thinner as the system evolves.…”

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confidence: 78%

Dynamics of the Transition Corona

Masson

McCauley

Golub

et al. 2014

ApJ

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Magnetic reconnection between the open and closed magnetic fields in the corona is believed to play a crucial role in the corona/heliosphere coupling. At large scale, the exchange of open/closed connectivity is expected to occur in pseudo-streamer (PS) structures. However, there is neither clear observational evidence of how such coupling occurs in PSs, nor evidence for how the magnetic reconnection evolves. Using a newly developed technique, we enhance the off-limb magnetic fine structures observed with the Atmospheric Imaging Assembly and identify a PS-like feature located close to the northern coronal hole. We first identify that the magnetic topology associated with the observation is a PS, null-point (NP) related topology bounded by the open field. By comparing the magnetic field configuration with the EUV emission regions, we determined that most of the magnetic flux associated with plasma emission are small loops below the PS basic NP and open field bounding the PS topology. In order to interpret the evolution of the PS, we referred to a three-dimensional MHD interchange reconnection modeling the exchange of connectivity between small closed loops and the open field. The observed PS fine structures follow the dynamics of the magnetic field before and after reconnecting at the NP obtained by the interchange model. Moreover, the pattern of the EUV plasma emission is the same as the shape of the expected plasma emission location derived from the simulation. These morphological and dynamical similarities between the PS observations and the results from the simulation strongly suggest that the evolution of the PS, and in particular the opening/closing of the field, occurs via interchange/slipping reconnection at the basic NP of the PS. Besides identifying the mechanism at work in the large-scale coupling between the open and closed fields, our results highlight that interchange reconnection in PSs is a gradual physical process that differs from the impulsive reconnection of the solar-jet model.

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confidence: 78%

Dynamics of the Transition Corona

Masson

McCauley

Golub

et al. 2014

ApJ

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“…Habbal et al (2010aHabbal et al ( , 2011aHabbal et al ( , 2011bHabbal et al ( , 2012Habbal et al ( , 2013 Our images provide the latest value of the flattening index, ε, combining the radial distances, as shown in Figure 6(a), and called E i (for Equatorial structure) and P i (for Polar structure): …”

Section: Prominent Features Of the Structure Of The White-light Coronamentioning

confidence: 93%

Structure and Dynamics of the 2012 November 13/14 Eclipse White-Light Corona

Pasachoff

Rusin

Санига

et al. 2015

ApJ

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Continuing our series of observations of coronal motion and dynamics over the solar-activity cycle, we observed from sites in Queensland, Australia, during the 2012 November 13 (UT)/14 (local time) total solar eclipse. The corona took the low-ellipticity shape typical of solar maximum (flattening index ε = 0.01), a change from the composite coronal images we observed and analyzed in this journal and elsewhere for the 2006 and 2008-2010 eclipses. After crossing the northeast Australian coast, the path of totality was over the ocean, so further totality was seen only by shipborne observers. Our results include velocities of a coronal mass ejection (CME; during the 36 minutes of passage from the Queensland coast to a ship north of New Zealand, we measured 413 km s−1 ) and we analyze its dynamics. We discuss the shapes and positions of several types of coronal features seen on our higherresolution composite Queensland coronal images, including many helmet streamers, very faint bright and dark loops at the bases of helmet streamers, voids, and radially oriented thin streamers. We compare our eclipse observations with models of the magnetic field, confirming the validity of the predictions, and relate the eclipse phenomenology seen with the near-simultaneous images from NASA's Solar Dynamics Observatory (SDO/AIA), NASA's Extreme Ultraviolet Imager on Solar Terrestrial Relations Observatory, ESA/Royal Observatory of Belgium's Sun Watcher with Active Pixels and Image Processing (SWAP) on PROBA2, and Naval Research Laboratory's Large Angle and Spectrometric Coronagraph Experiment on ESA's Solar and Heliospheric Observatory. For example, the southeastern CME is related to the solar flare whose origin we trace with a SWAP series of images.

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“…These characteristics are dictated by the need of creating artificial eclipses, that are reproduced via internal or external occulters. Natural eclipses offer the ideal solution to decrease the sky brightness and to get the highest spatial resolution, on the order of 1 arcsec (see, e.g., Habbal et al (2011); for a comparison, SOHO/EIT data have a spatial resolution of the order of 5 arcsec).…”

Section: Future Eclipse Campaignsmentioning

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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Thermodynamics of the Solar Corona and Evolution of the Solar Magnetic Field as Inferred From the Total Solar Eclipse Observations of 2010 July 11

Abstract: We report on the first multi-wavelength coronal observations, taken simultaneously in white light, Hα 656.3 nm,

Cited by 78 publications

References 24 publications

Dynamics of the Transition Corona

Dynamics of the Transition Corona

Structure and Dynamics of the 2012 November 13/14 Eclipse White-Light Corona

Solar Coronal Plumes

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