Electroplastic Deformation by Twinningmetals

The article deals with theoretical and experimental approaches to electroplastic deformation caused by twinning of metals. The author specifies physical fundamentals of Kinetics regarding the development of twinning caused by the excitation of electronic subsystem of metals. Physical models of new channels for the realization of twinning aroused under conditions of electroplasticity have been discussed. Mechanisms of plasticized influence of a surface electric charge have been defined as well as the contribution of a dynamic pinch-effect in the elastic plastic deformation of metals with the participation of the intrinsic magnetic field of the current. The dynamic pinch effect creates ultrasonic vibration of the lattice system while Kinetics changes and plastic deformation are stimulated increasing the amplitude of the oscillations of rectilinear dislocations and the periodic change in the position of the dislocation loops with an increase in the probability of detachment of dislocations from the stoppers. When deformed above the yield point and due to the pinch effect the intrinsic magnetic field of the current diffuses into the crystal where the diffusion rate depends both on the conductivity of the metal and on the frequency of the current. It is necessary to take into account the physical conditions for the creation of ponderomotive effects in relation to specific technically important materials for the practical use of electroplastic deformation technology, especially when processing metals with pressure.

Why an intrinsic magnetic field does not protect a planet against atmospheric escape

The presence or absence of a magnetic field determines the nature of how a planet interacts with the solar wind and what paths are available for atmospheric escape. Magnetospheres form both around magnetised planets, such as Earth, and unmagnetised planets, like Mars and Venus, but it has been suggested that magnetised planets are better protected against atmospheric loss. However, the observed mass escape rates from these three planets are similar (in the approximate (0.5–2) kg s−1 range), putting this latter hypothesis into question. Modelling the effects of a planetary magnetic field on the major atmospheric escape processes, we show that the escape rate can be higher for magnetised planets over a wide range of magnetisations due to escape of ions through the polar caps and cusps. Therefore, contrary to what has previously been believed, magnetisation is not a sufficient condition for protecting a planet from atmospheric loss. Estimates of the atmospheric escape rates from exoplanets must therefore address all escape processes and their dependence on the planet’s magnetisation.