O N TH E MAGNETI C FIEL D ORIGI N O F A p STAR S A . ... We assume that the surface magnetic field strength may be influenced by the high energy flux of cosmic rays (CR) and by intensity of hard ultraviolet radiation (UV), changing the effectivity of diffusion processes. ... FOSSIL MAGNETIC FIELD STRENGTH We study the dependence of the fossil field strength of stars upon ionizing radiation power with the computer program of numerical study of protostar evolution (see Dudorov, this volume) . ...

Magnetic Stars, 2011, pp. ... It follows, in particular, from Fig. 1a, where points show the central intensity of line in 2008 ­ 2009, and asterisks -- the ELODIE Archive (EA) spectra in 2002 ­ 2003 smoothed to the resolution of the MSS. ... Figure 2a demonstrates the distribution of temperature in the atmosphere in the phase = 0.07 and Fig. 2b -- in the phase = 0.53 of the rotation period, obtained from the hydrogen line profiles in 2008 ­ 2009. ...

THE STUDY OF A MAGNETIC FIELD STRUCTURE IN BLAZAR JETS BY OPTICAL PHOTOPOLARIMETRIC DATA Yu.S. Efimov1 , E.Yu. ... Besides the Faraday rotation of p olarization plane there are observational parameters which are connected directly with the intensity of magnetic field and its structure: a p olarization degree and a sp ectral index. ... Moreover, such a comparison allows to follow the variations of the magnetic field intensity from observed variations of p olarization degree and sp ectral index. ...

... Corresponding gates in each row are connected in parallel at both edges of the array. ... Other gates. ... otherwise indicated, 45 kpixels/sec and standard voltages using a dual slope CDS circuit (8 µs integration time) Minimum Format Pixel Size Imaging Area Dark current (MPP), 20° C equivalent Readout noise Front Back Full Well signal Output gain CTE per pixel Typical 512 x 512 pixels 24 µm x 24 µm 12.3 mm x 12.3 mm 50 pa/cm2 5 electrons 7 electrons 350,000 electrons 1.5 µV/ electron 0 ...