... 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. ...

... Files in red?history) . ... Trapped Motion . ... 10a. Particle Drift . ... Fast Particles . ... The fact charged particles circle around field lines was well known to J.J. Thomson when he experimented with electron and ion beams in a magnetic field. ... The notion of adiabatic invariance is tied with the early years of quantum theory. ... By about1910, physicists realized that these patterns indicated changes in the laws of physics as one approached atomic dimensions. ...

... 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 ...

The UV throughput of the WFPC2 degrades in a predictable way after each monthly decontamination. ... Figure 6.11 shows the photometric monitoring data for the standard star GRW+70D5824 (a white dwarf classified DA3; B-V = -0.09) in the WF3 and PC1 for the set of filters which are routinely monitored. ... Filter . ... 0.007 . ... Figure 6.12 and Figure 6.13 show the throughput decline in all four chips as a function of days since the last decontamination for the F170W filter. ... Time. ...

... Back to the Live Radiation Monitor Data The radiation monitor on board XMM-Newton registers the total count rate and basic spectral information on the background radiation impinging on the spacecraft and its scientific instruments. ... Counting of pulses for a selected energy band and above the low thresholds. ... Sensitivity: due to the electronic threshold, actually only electrons with energy greater than 130 keV and protons greater than 1.3 MeV can be measured by this unit. ...

... Magnetic fields, subatomic particles, etc., traveling in different directions fill the universe. Do they deflect or otherwise affect one another? If so, isnт??t the information we get from them distorted? ... Neutrino astronomy, which is still in its infancy, is attractive because neutrinos interact so weakly with matter that few of these distorting effects occur. Get instant access to subscriber content on Astronomy.com! ...

... 2000 July 20 . AR9077: Solar Magnetic Arcade . Credit: TRACE , Stanford-Lockheed ISR, NASA . Explanation: On July 14th , solar active region 9077 (AR9077) produced a massive flare . ... It shows million degree hot solar plasma cooling down while suspended in an arcade of magnetic loops . ... After the flare, AR9077's activity decayed as it was carried farther across the Earth-facing hemisphere of the Sun by solar rotation . ... About APOD | ... NASA Technical Rep.: ...

The above process keeps the # of protons and the # of neutrons in the early Universe constant. This is extremely important and will result in a testable prediction later. Remember, a free neutron (one that is not bound in an atomic nucleus) will decay into a proton + electron (+ anti-neutrino) in about 900 seconds. ... During this epoch, the proton-to-neutron ratio is 1.0 . ... The Universe consists of protons, neutrons and electrons plus a photon background and a neutrino background. ...

... Nizhnij Arkhyz, 2007 . ... Romanyuk I.I. Speech at the opening ceremony of the conference "Physics of magnetic stars" . ... Gnedin Yu.N. Magnetic fields of stars and fundamental particle physics . ... Landstreet J.D., Andretta V., Bagnulo S., Mason E., Silaj J., Wade G.A. The magnetic fields of peculiar A and B stars in open clusters . ... Wade G.A., Catala C., Alecian E., Folsom C., Bagnulo S., Bohm T., Bouret J.-C., Donati J.-F., Drouin D. , Landstreet J.D. Magnetic fields in Herbig Ae/Be stars . ...

... Since the bulk of the data for rotational modulation were taken during short ( < 11 night) runs, there is a great deal of variation in the sensitivity to periods, depending on the length of the period. The searches are much more sensitive to short periods than to longer ones. ... For the simulation, the input data was a pure sine wave. ... The strength is that in all cases, even down to signal to noise levels of one, a large percentage of the power can be found in the correct period. ...

Teaching courses . for student of the Department of Astrophysics and Stellar Astronomy . ... Geophysics and physics of the planets (Kurt, Panteleev) . ... Close Binary Stars . ... Solar Physics . ... This is introductory course for students of the third year of education which are familiar with elementary astronomy and general physics. ... The one-year course includes theory of radiation transfer, theory of internal stellar structure with account of binary systems with compact comapnions. ...

... 2009 April 15 . Jagged Shadows May Indicate Saturn Ring Particles . ... Explanation: What's causing unusual jagged shadows on Saturn's rings? ... Now Saturn's rings have been known to be made of particles for hundreds of years , but these particles have so far escaped direct imaging. It is therefore particularly exciting that a preliminary hypothesis holds that these jagged shadows are silhouettes of transient groups of ring particles temporarily held close by their own gravity. ...