Structure of solar coronal loops: from miniature to large-scale

@article{Peter2013StructureOS,
  title={Structure of solar coronal loops: from miniature to large-scale},
  author={H. Peter and Sven Bingert and James A. Klimchuk and C. de Forest and Jonathan W. Cirtain and Leon Golub and Amy R. Winebarger and K. Kobayashi and Kelly E. Korreck},
  journal={Astronomy and Astrophysics},
  year={2013},
  volume={556}
}
Aims. We use new data from the High-resolution Coronal Imager (Hi-C) with its unprecedented spatial resolution of the solar corona to investigate the structure of coronal loops down to 0.2 (cid:48)(cid:48) . Methods. During a rocket flight, Hi-C provided images of the solar corona in a wavelength band around 193Å that is dominated by emission from Fe  showing plasma at temperatures around 1.5MK. We analyze part of the Hi-C field-of-view to study the smallest coronal loops observed so far and… 
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References

SHOWING 1-10 OF 52 REFERENCES
Constant cross section of loops in the solar corona
Context. The corona of the Sun is dominated by emission from loop-like structures. When observed in X-ray or extreme ultraviolet emission, these million K hot coronal loops show a more or less…
Observations of Active Region Loops with the EUV Imaging Spectrometer on Hinode
Previous solar observations have shown that coronal loops near 1 MK are difficult to reconcile with simple heating models. These loops have lifetimes that are long relative to a radiative cooling…
Observing the Fine Structure of Loops through High-resolution Spectroscopic Observations of Coronal Rain with the CRISP Instrument at the Swedish Solar Telescope
Observed in cool chromospheric lines, such as H? or Ca II H, coronal rain corresponds to cool and dense plasma falling from coronal heights. Considered as a peculiar sporadic phenomenon of active…
High Spatial Resolution Observations of Loops in the Solar Corona
Understanding how the solar corona is structured is of fundamental importance to determine how the Sun's upper atmosphere is heated to high temperatures. Recent spectroscopic studies have suggested…
SOLAR CORONAL LOOPS RESOLVED BY HINODE AND THE SOLAR DYNAMICS OBSERVATORY
Despite decades of studying the Sun, the coronal heating problem remains unsolved. One fundamental issue is that we do not know the spatial scale of the coronal heating mechanism. At a spatial…
Observing Coronal Nanoflares in Active Region Moss
The High-resolution Coronal Imager (Hi-C) has provided Fe XII?193? images of the upper transition region moss at an unprecedented spatial (~0.''3-0.''4) and temporal (5.5?s) resolution. The Hi-C…
The Magnetic Structure of Coronal Loops Observed by TRACE
Previous studies have found that coronal loops have a nearly uniform thickness, which seems to disagree with the characteristic expansion of active region magnetic fields. This is one of the most…
Dynamics of solar coronal loops I. Condensation in cool loops and its effect on transition region lines
We report numerical calculations of the condensation of plasma in short coronal loops, which have several interesting physical consequences. Firstly, we propose a connection between small, cool loops…
The Formation of Coronal Loops by Thermal Instability in Three Dimensions
Plasma loops in solar active regions have been observed in EUV and soft X-rays for decades. Their formation mechanism and properties, however, are still not fully understood. Predictions by early…
The plasma filling factor of coronal bright points - II. Combined EIS and TRACE results
TLDR
Higher spatial resolution observations with the Transition Region and Corona Explorer (TRACE) indicate the median value of their plasma filling factor is 0.04, which can be interpreted as evidence of a considerable subresolution structure in coronal bright points or as the result of a single completely filled plasma loop with widths on the order of 0.2–1.5 �� that has not been spatially resolved in these measurements.
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