The most popular models for the complex phase and time lags in the rapid aperiodic variability of Galactic X-ray binaries are based Comptonization of soft seed photons in a hot corona, where small-scale flares are induced by flares of the soft seed photon input (presumably from a cold accretion disc). However, in their original version, these models have neglected the additional cooling of the ...

BACKGROUND Hyperactivity of depressor septi nasi muscle leads to smiling deformity and nasal tip depression. Lateral fascicles of this muscle help in widening the nostrils. The purpose of this study was to evaluate the relationship between the nasal length changes and the alar base and the alar flaring changes during smile. METHODS Standard photographs are performed in the face and lat...

Aims. The hydrogen Lyman lines provide important diagnostic information about the dynamics of the chromosphere, but there have been few systematic studies of their variability during flares. We investigate Doppler shifts in these lines in several flares, and use these to calculate plasma speeds. Methods. We use spectral data from the Multiple EUV Grating Spectrograph B (MEGS-B) detector of the ...

We have systematically studied the X-ray emission (both the quiescent component and the flares) of the dM3e star AD Leo, analyzing the existing observations from the Einstein IPC, ROSAT PSPC and ASCA SIS instruments. Using a consistent method which explicitly considers the possibility of sustained heating we have analyzed the six flares which have sufficient statistics, deriving constraints on ...

In previous works we have developed a method to convert solar X-ray data, collected with the Yohkoh/SXT, into templates of stellar coronal observations. Here we apply the method to several solar flares, for comparison with stellar X-ray flares. Eight flares, from weak (GOES class C5.8) to very intense ones (X9) are selected as representative of the flaring Sun. The emission measure distribution...

Context. In classical T Tauri stars, X-rays are produced by two plasma components: a hot low-density plasma, with frequent flaring activity, and a high-density lower temperature plasma. The former is coronal plasma related to the stellar magnetic activity. The latter component, never observed in non-accreting stars, could be plasma heated by the shock formed by the accretion process. However it...

We have systematically studied the X-ray emission (both the quiescent component and the flares) of the dM3e star AD Leo, analyzing the existing observations from the Ein-stein IPC, ROSAT PSPC and ASCA SIS instruments. Using a consistent method which explicitly considers the possibility of sustained heating we have analyzed the six flares which have sufficient statistics, deriving constraints on...

We have analyzed X-ray and EUV spectra of both the quiescent and flaring state of II Peg, obtained from observations with ASCA and EUVE. Coronal temperature structure and abundances have been derived from multi-temperature and differential emission measure (DEM) analyses of the spectra. The abundances are non-solar; in the case of ASCA for most elements (O, Ne,Mg, Si, S, Ar, Ca, Ni) we obtain a...

AIM The aim of this study was to compare sizes of the first instrument with or without a taper that binds at the apical constriction of a root canal after coronal flaring. METHODS AND MATERIALS A total of 310 canals were evaluated in patients presenting for root canal therapy. Canals with intact apices were selected. After gaining straight line endodontic access, the coronal third was flared ...

We show how to estimate the size of spatially unresolved solar and stellar coronal flaring regions from the X-ray light curve and time-resolved temperature and emission measure values during the flare decay. Bymeans of extensive hydrodynamic modeling of decaying flaring loops, we propose and test a relationship between the decay time of the light curve in the band of a specific instrument and t...