I present a novel view on the problem of solar coronal heating. In my picture, coronal heating should be viewed as a self-regulating process that works to keep the coronal plasma marginally collisionless. The self-regulating mechanism is based on the interplay between two effects: (1) Plasma density controls coronal energy release via the transition between the slow collisional Sweet-Parker reg...

We have recently noticed cellular features in Fe xii 193 Å images of the 1.2 MK corona. They occur in regions bounded by a coronal hole and a filament channel, and are centered on flux elements of the photospheric magnetic network. Like their neighboring coronal holes, these regions have minority-polarity flux that is ∼0.1–0.3 times their flux of majority polarity. Consequently, the minority-po...

BACKGROUND Magnetic resonance cholangiopancreatography (MRCP) is an established technique for the evaluation of intra- and extrahepatic bile ducts in patients with known or suspected hepatobiliary disease. However, the ideal acquisition and reconstruction plane for optimal bile duct evaluation with 3D technique has not been evaluated. The purpose of our study was to compare different acquisitio...

BACKGROUND Isolated coronal plane fractures of the distal femoral condyles (Hoffa fractures) occur uncommonly, are difficult to diagnose, and may be challenging to treat. The combination of supracondylar distal femoral fractures and these coronal plane fractures is thought to occur rarely. The purposes of the present study were to identify the frequency of the association between supracondylar-...

Heterozygous loss of Twist1 function causes coronal synostosis in both mice and humans. We showed previously that in mice this phenotype is associated with a defect in the neural crest-mesoderm boundary within the coronal suture, as well as with a reduction in the expression of ephrin A2 (Efna2), ephrin A4 (Efna4) and EphA4 in the coronal suture. We also demonstrated that mutations in human EFN...

We report a detailed analysis of the coronal abundance of 4 stars with varying levels of activity and with accurately known photospheric abundances. The coronal abundance is determined here using a line flux analysis and a full determination of the differential emission measure. Photospheric abundance values are taken from the literature. Previous coronal abundance determinations have generally...

coronal T2 coronal FLAIR SOS 12.8/13.6 12.5/11.4 2x 14.8/17.3 14.5/13.2 3x 19.8/24.8 14.8/12.5 4x 22.9/25.8 16.1/14.3 Table 1: SNR (reader1/reader2) coronal T2 coronal FLAIR SOS 2.9/3.0 2.7/2.9 2x 2.8/2.6 2.1/2.2 3x 2.3/2.4 1.4/1.9 4x 2.0/2.0 1.1/1.3 Table 3: average qualitative scoring (reader1/reader2); (scoring: 1-poorly defined, 2-seen, 3-well defined); (green-diagnostic quality; yellowsome...