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C  W The Maxwell Centre
C W The Maxwell Centre

Propagation of cosmic rays in the solar wind
Propagation of cosmic rays in the solar wind

Lecture 2. Thermal evolution and surface emission of neutron stars
Lecture 2. Thermal evolution and surface emission of neutron stars

... prototypes of a different subpopulation of NSs born with low magnetic field (< few 1011 G) and relatively long spin periods (few tenths of a second). These NSs are relatively hot, and probably not very rare. Surprisingly, we do not see objects of this type in our vicinity. In the solar neighbourhood ...
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THE THERMAL INSTABILITY OF SOLAR PROMINENCE THREADS

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Power Point Presentation
Power Point Presentation

Highligh in Physics 2005
Highligh in Physics 2005

... the properties of accretion disks and found that this role may help explain a number of observational properties of young proto-stellar objects, especially of FU Orionis stars [1]. The theory of such self-gravitating disks recognizes that disks in their outer parts cannot be too cold, otherwise they ...
radiation and matter interaction in strong magnetic field of accreting
radiation and matter interaction in strong magnetic field of accreting

ASPERA-3: Analyser of Space Plasmas and
ASPERA-3: Analyser of Space Plasmas and

... wind (the spectrum marked by arrows in Fig. 2). These ENAs can be detected only at the beam edges because they are superimposed on the intense flux of the solar radiation. The shocked solar wind is the strongest source of ENAs because the protons flowing around Mars can interact with dense neutral g ...
Read the report
Read the report

Transcript from 5th Kids Knowledge Seekers Workshop held
Transcript from 5th Kids Knowledge Seekers Workshop held

... mean? Well, let’s say, you take a piece of wood in a fire, and it burns. You burn the wood. Then you get a bit of heat, you cook your food on it or you get warm sitting in front of it. But, at the end of the process, you don’t have wood anymore. Because, the energy, the structure of the plasma, whic ...
Magnetic collapse of a neutron gas: Can magnetars
Magnetic collapse of a neutron gas: Can magnetars

Towards the pair spectroscopy of the Hoyle state in 12C
Towards the pair spectroscopy of the Hoyle state in 12C

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KUVEMPU KUVEMPU UNIVERSITY PHYSICS

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On the Origin of Cosmic Magnetic Fields

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Coronal energy input and dissipation in a solar active region 3D

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High Resolution Chandra Spectroscopy of Gamma Cassiopeia (B0

... while the remainder is affected by only a much lower column density of 3×1021 cm−2 . The hot component has a Fe abundance of only 0.22±.05 solar. The other two or three major emission components are “warm” and are responsible for most other emission lines. These components are dominated by plasma ha ...
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bob_neutrino_EPS04

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SIMULATION OF QUIET-SUN WAVES IN THE Ca ii INFRARED TRIPLET

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“LIFE and SPACE” ECLECTIC - RASC

Bose-Einstein Condensation in a Constant Magnetic Field
Bose-Einstein Condensation in a Constant Magnetic Field

... eld strength, in our case B, and in the order operator , in our case M^ , the magnetization. As a result, at any value of B, M becomes di erent from zero at any temperature. Thus, B reduces the symmetry of the usual more symmetrical phase, and the di erence between the two phases of the usual theor ...
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... In the region of overlap between cold solar wind and heated downstream plasma waves are produced by a right hand resonant instability (solar wind is background, hot plasma is beam). ...
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The Aurora

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Teaching scheme - Pearson Schools and FE Colleges
Teaching scheme - Pearson Schools and FE Colleges

2007_PG - St.Joseph`s College
2007_PG - St.Joseph`s College

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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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