... Magnetic trapping . ... 10a. Particle Drift . ... The magnetic force on a moving particle is always perpendicular to the motion, as well as to the magnetic field lines. ... Similarly with the charged particle, the magnetic and centrifugal forces are always balanced. ... Because no energy is needed to keep up the motion, it can (in principle) persist indefinitely. ... Out in space, it usually takes electric forces, not just magnetic ones, to change the total speed and energy of the particles. ...

A full explanation of the motion of trapped particles would be too abstract and mathematical for this level, but some basic ideas may be described on an intuitive level. The magnetic force on a moving particle is always perpendicular to the motion, as well as to the magnetic field lines. That is why the basic pattern is motion in a circle, around a magnetic field line. ... The best-known periodic motion is the back-and-forth swing of a pendulum, say of a weight suspended by a string (drawing). ...

... Credit: TRACE , Stanford-Lockheed ISR, NASA Explanation: On July 14th , solar active region 9077 (AR9077) produced a massive flare . ... Collectively resembling a popular "slinky" toy, the enormous loops are actually magnetic field lines which trap the glowing, cooling plasma above the relatively dark solar surface. ... NASA Official: Jay Norris. ... Publications with keywords: Sun - flare - active region - magnetic field . Publications with words: Sun - flare - active region - magnetic field . ...

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

SPECTRUM ANALYZER OF MAGNETIC PHENOMENA SAMW . Spectrum analyzer allows onboard computation of electromagnetic waves spectra registered (observed) in the ionosphere and magnetosphere in the ELF/VLF frequency band. ... It consists of magnetic antenna, preamplifier, 16 bit sigma delta AD converter, DSP processor and telemetry interface. ... The channels of lower frequencies are averaged and transmitted with lower repetition rate so the telemetry volume is reduced. ... Dynamic range: 90 dB . ...

Pulsar radio emission - oscillating model M. Verdon, D. Melrose University of Sydney 10 th June, 2010 Outline Problems understanding pulsar radio emission Magnetosphere model Emission mechanisms Oscillating model Wave modes Time-dependence Coupling What is a pulsar? rotation axis magnetic axis polar cap open field line region closed field line region Emission models Production of ...

... Magnetic fields of the Sun are generally concentrated in small regions characterized by opposite polarities (the so-called "sunspots"), the nature of which change within a short-time scale. ... For instance, the magnetic field of some early-type stars and white dwarfs is constant at least over a time scale of decades, but is not symmetric about the star's rotation axis, so that the observer sees a magnetic configuration that changes as the star rotates. ...

Next: A Universal Diagram for Up: ``Ecology'' of Magnetic Rotators Previous: The Corotation Radius . The interaction of a magnetic rotator with the surrounding plasma to a large extent depends on the relation between the four characteristic radii: the stopping radius, , the gravitational capture radius,   , the light cylinder radius,   , and the corotation radius,   . ... Hence, the classification of the interaction regimes may well mean the classification of magnetic rotators. ...

... As a first step, the short dark and pre-flashed dark exposures have to be averaged to produce the BIAS and pre-flashed BIAS frame. A method which performs the averaging and which at the same time discards bad pixels due to e.g. cosmic events is AVERAGE/WINDOW Before actually executing this command, prepare a catalogue containing all input files to be averaged via: . ... where inputspec is either a single file name or the catalogue with the list of input files, to be specified as catname.cat. ...

... public class EDM . ... Euclidean Distance Map: The value of each pixel is the distance to the nearest background pixel (for background pixels, the EDM is 0) - Ultimate Eroded Points (UEPs) are maxima of the EDM. ... static int . ... Unit in old make16bitEDM: this pixel value corresponds to a distance of one pixel. static int . ... int . ... For compatibility with previous versions of ImageJ only. public FloatProcessor makeFloatEDM ( ImageProcessor ip, int backgroundValue, boolean edgesAreBackground)...

... The forces of the mobile are calculated using a grid scheme. ... The initial parameters are coded in the file names: The number after Speed is the pattern speed of the initial quadrupole field and frac is the fraction of disk particles . [agris@mizar ~/ Mar ]# ll ~/public_html/Larry/ 6033838 Mar 2 10:14 Speed -0.08- frac -0.0g.ps 6035344 Mar 2 10:14 Speed -0.08- frac -0.1g.ps 6040839 Mar 2 10:14 Speed -0.16- frac -0.0g.ps 8778756 Mar 2 10:14 ...