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Longitudinal analysis of the proportion of repertoire occupied by the three clonal groups in SLE (top 50, >95th percentile, <95th percentile) during quiescence (A), pre-flare (B), and flare (C).
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Apart from the higher class solar flares (C to X), a solar flare of class B8.5 also produced enhancements both on the amplitude and phase.
Thus, for most of the daytime flares for C class and above, the VLF signatures were quite clearly identified and correlated with the peak flux density.
This difference in the level of β is found to be more pronounced for intense M and X class flares than for weak C class flares.
This difference in the level of β and H′ is found to be more pronounced for strong M and X class flares than for low C class flares.
A hepatitis C flare has been described in a coinfected patient who had HBeAg/HBV DNA clearance in response to IFN [ 56].
M-class flares can cause brief radio blackouts in the polar regions and occasional minor radiation storms, while C flares have few noticeable consequences.
VLF perturbations might not be observed during daylight hours, for all the flares, because either the VLF transmitters were off (or no data were available) or weaker flares of class C and below may not have produced any detectable VLF perturbations.
To our knowledge, solar flares of class C and above have been reported so far to show detectable effect on VLF transmissions.
Their results suggest that the occurrence of SPAs due to weak solar flares, of class C and below, was higher during solar minima, but the occurrence of SPAs was not dependent on the solar activity for stronger class flares.
Radiographs show several morphological appearances of multiplex dysostosis in long bones, with proximal humeral notching (white arrow, a), long and narrow femoral neck (curved white arrow, b), and frayed and flared tibial metaphyses (c).
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Justyna Jupowicz-Kozak
CEO of Professional Science Editing for Scientists @ prosciediting.com