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Improved period of a slowly rotating cool magnetic CP star HD 188041
Improved period of a slowly rotating cool magnetic CP star HD 188041

Sun Physics
Sun Physics

0119.PDF
0119.PDF

... The solution to the original Bloch equation clearly satisfies the augmented system, p — p, by construction and from the uniqueness property of the heat equation with a source-sink term [3] it is the only solution. This augmented system now allows probabilistic methods to be used to sample the positi ...
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RAS_waves - University of Glasgow

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talk-tutorial - Helioseismic and Magnetic Imager

Modelling Mercury`s magnetospheric magnetic field
Modelling Mercury`s magnetospheric magnetic field

High Energy Processes in Young Stellar Objects
High Energy Processes in Young Stellar Objects

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... Far from the FFS the particles move virtually along the magnetic field lines. Their energy is determined from the balance between the power of accelerated electric field forces and the curvature radiation intensity. When intersecting the FFS, the particles oscillate ultrarelativistically, their ener ...
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... temperature is more than one million K. We can see the solar corona at the visible light when the strong radiation of the solar disk is blocked in a total solar eclipse. We can observe the solar corona in X-rays and UVs from the satellite. Solar Flare : 【太陽フレア】 Violent event accompanied with sudden ...
Lorentz Invariance on Trial - Physics Department, Princeton University
Lorentz Invariance on Trial - Physics Department, Princeton University

... trivial background fields such as the field illustrated in figure 1. The Lorentz violation therefore also appears as a Comagnetometers Modern descendants of Hughes–Drever experiments prospontaneous symmetry breaking. One can classify all possible interaction operators by vide very stringent constrai ...
turbulence - "A" Laboratory, Department of Physics/Astrophysics
turbulence - "A" Laboratory, Department of Physics/Astrophysics

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Chapter 7 Plasma Basics

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The solar dynamo(s) - Center for Magnetic Self Organization

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Solar and Stellar Active Regions

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Plasma Seminar 4/23/07 "Negative Ion Plasmas"
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Spheromak

Not to be confused with the spherical tokamak, another topic in fusion research.A spheromak is an arrangement of plasma formed into a toroidal shape similar to a smoke ring. The spheromak contains large internal electric currents and their associated magnetic fields arranged so the magnetohydrodynamic forces within the spheromak are nearly balanced, resulting in long-lived (microsecond) confinement times without external fields. Spheromaks belong to a type of plasma configuration referred to as the compact toroids.The physics of the spheromak and their collisions is similar to a variety of astrophysical events, like coronal loops and filaments, relativistic jets and plasmoids. They are particularly useful for studying magnetic reconnection events, when two or more spheromaks collide. Spheromaks are easy to generate using a ""gun"" that ejects spheromaks off the end of an electrode into a holding area, called the flux conserver. This has made them useful in the laboratory setting, and spheromak guns are relatively common in astrophysics labs. These devices are often, confusingly, referred to simply as ""spheromaks"" as well; the term has two meanings.Spheromaks have been proposed as a magnetic fusion energy concept due to their long confinement times, which was on the same order as the best tokamaks when they were first studied. Although they had some successes during the 1970s and 80s, these small and lower-energy devices had limited performance and most spheromak research ended when fusion funding was dramatically curtailed in the late 1980s. However, in the late 1990s research demonstrated that hotter spheromaks have better confinement times, and this led to a second wave of spheromak machines. Spheromaks have also been used to inject plasma into a bigger magnetic confinement experiment like a tokamak.
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