Context. We present a self-consistent model of solar coronal heating in which we include the dynamical effect of the background magnetic field along a coronal structure by using exact results from wave MHD turbulence. Aims. We evaluate the heating rate and the microturbulent velocity for comparison with observations in the quiet corona, active regions and also coronal holes. Methods. The corona...

Although toddlers in their 2nd year of life generally have phonologically detailed representations of words, a consistent lack of sensitivity to certain kinds of phonological changes has been reported. The origin of these insensitivities is poorly understood, and uncovering their cause is crucial for obtaining a complete picture of early phonological development. The present study explored the ...

This meta-analysis reviewed 12 studies comparing patient-specific instrumentation (PSI) with standard instrumentation (SI) for total knee arthroplasty in terms of postoperative coronal alignment and operation time. There is no significant difference between PSI and SI in terms of hip-knee-ankle angle (overall coronal alignment or mechanical axis), tibial coronal alignment, and operation time.

Coronal observations in X-rays show the sun has many dynamic features that can neither be imagined nor seen with the naked eye. The solar corona has a wide temperature range from less than 1MK (1,000,000K) to more than 10MK. The X-ray telescope (XRT) on board the Hinode satellite has 9 X-ray analysis filters to observe the almost of whole coronal plasma. Using the data observed with this telesc...

Most work on coronal mass ejection (CME) interpretation focuses on the involved active region rather than on the large-scale coronal context. In this paper a global potential-field sourcesurface model of the coronal magnetic field is used to evaluate the sensitivity of the coronal field configuration to the location, orientation, and strength of a bipolar active region relative to a background ...

We highlight 10 key aspects of coronal heating that must be understood before we can consider the problem to be solved. (1) All coronal heating is impulsive. (2) The details of coronal heating matter. (3) The corona is filled with elemental magnetic stands. (4) The corona is densely populated with current sheets. (5) The strands must reconnect to prevent an infinite build-up of stress. (6) Nano...

Amethod for automated coronal hole detection using He I 1083 nm spectroheliograms and photospheric magnetograms is presented here. The unique line formation of the helium line allows for the detection of regions associated with solar coronal holes with minimal line-of-sight obscuration across the observed solar disk. The automated detection algorithm utilizes morphological image analysis, thres...

BACKGROUND: Idiopathic scoliosis is accompanied by postural alterations, instability of gait, and functional disabilities. The objective was to verify radiographic parameters (coronal sagittal) adolescents with idiopathic (AIS) pre- post-surgery direct vertebral rotation (DVR), associated type 1 osteotomies in all segments (except the most proximal) 2 periapical vertebrae curves. METHODS: A pro...

Magnetic resonance imaging is the most important diagnostic method in the investigation of the pituitary lesions. Our aim is to determine whether T2-weighted coronal images may be helpful in the evaluation of the pituitary gland with suspected pituitary adenomas. One hundred and sixty-seven patients were examined prospectively with T2-weighted coronal and T1-weighted coronal images enhanced wit...

Context. In the standard solar flare scenario, a large number of particles are accelerated in the corona. Nonthermal electrons emit both X-rays and radio waves. Thus, correlated signatures of the acceleration process are predicted at both wavelengths, coinciding either close to the footpoints of a magnetic loop or near the coronal X-ray source. Aims. We attempt to study the spatial connection b...