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Non-thermal emission processes in massive binaries*
Non-thermal emission processes in massive binaries*

ELECTRICITY AND MAGNETISM Chapter 1. Electric Fields 1.1
ELECTRICITY AND MAGNETISM Chapter 1. Electric Fields 1.1

Magnetic fields and mass loss in massive stars
Magnetic fields and mass loss in massive stars

... Over the last decades, fields have been discovered in all stages of stellar evolution and on scales from single stars to whole galaxies. From the µG to mG fields in galaxies (e.g. Beck et al. 1996) and star forming molecular clouds (Crutcher 1999), to 10 1 – 104 G fields in planets and stars, and to ...
Shock structure and ion dynamics
Shock structure and ion dynamics

Magnetism in Isolated and Binary White Dwarfs
Magnetism in Isolated and Binary White Dwarfs

... the gasdynamics of mass transfer and the radiation properties. The process of magnetized accretion onto compact stars can now be examined in great detail using magnetic white dwarfs in the MCVs, complementing similar work in the X-ray band with neutron star binaries. Since the MCVs harbor magnetic w ...
EUV and X-ray Spectroscopy of the Active Sun
EUV and X-ray Spectroscopy of the Active Sun

Origin of solar surface activity and sunspots Sarah Jabbari Nordita, Stockholm, Sweden
Origin of solar surface activity and sunspots Sarah Jabbari Nordita, Stockholm, Sweden

The Earliest Stages of Star and Planet Formation: Core Collapse
The Earliest Stages of Star and Planet Formation: Core Collapse

THE SPECIFIC ACCELERATION RATE IN LOOP
THE SPECIFIC ACCELERATION RATE IN LOOP

Unit 13 - Magnetism
Unit 13 - Magnetism

Accreting magnetars: a new type of high-mass X-ray binaries? P. Reig,
Accreting magnetars: a new type of high-mass X-ray binaries? P. Reig,

making measurements of susceptibility, remanence and Q in the field
making measurements of susceptibility, remanence and Q in the field

Effects of Thomson-Scattering Geometry on White-Light
Effects of Thomson-Scattering Geometry on White-Light

Observations of the Magnetic Fields Inside and Outside the
Observations of the Magnetic Fields Inside and Outside the

Magnetic collapse of a neutron gas: Can magnetars
Magnetic collapse of a neutron gas: Can magnetars

On the origin of El Chichón volcano and subduction of
On the origin of El Chichón volcano and subduction of

Further VLBA Observations of SiO Masers toward Mira
Further VLBA Observations of SiO Masers toward Mira

... the Mira variable stars reported in Cotton et al. (2004) (o Ceti=Mira, U Orionis=U Ori, R Aquarii=R Aqr) over a period of 16 months, extending the observations to several pulsation cycles. The observed size of the maser rings varied by 3-14% with time but show no clear correlation with pulsation pha ...
Foreword You`ll notice here that I hardly make mention of gravity, if
Foreword You`ll notice here that I hardly make mention of gravity, if

MRI SAFETY JEOPARDY (NONTechnologist Edition) Questions
MRI SAFETY JEOPARDY (NONTechnologist Edition) Questions

Optical hydrogen absorption consistent with a thin bow shock
Optical hydrogen absorption consistent with a thin bow shock

Numerical models of sunspot formation and fine structure
Numerical models of sunspot formation and fine structure

The Trouble with Cosmological Magnetic Fields
The Trouble with Cosmological Magnetic Fields

... or even larger coherence scales Filaments: There are indications of magnetic fields in filaments with strengths up to B ∼ 10−8 – 10−7 Gauss and coherence scales over 1Mpc (Kronberg 2010). ...
RADIO RELICS AND MAGNETIC FIELDS IN GALAXY CLUSTERS
RADIO RELICS AND MAGNETIC FIELDS IN GALAXY CLUSTERS

... the non-detection of inverse Compton emission from these sources. These limits will be combined with the constraints obtained from the analysis of the thickness of relics. The spatial profile of the magnetic field in GCs is still poorly known. In this respect constraints on magnetic fields at the di ...
Latitudinal and radial gradients of galactic cosmic ray protons in the
Latitudinal and radial gradients of galactic cosmic ray protons in the

William Gilbert Founder Of Terrestrial Magnetism
William Gilbert Founder Of Terrestrial Magnetism

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Aurora



An aurora is a natural light display in the sky, predominantly seen in the high latitude (Arctic and Antarctic) regions. Auroras are produced when the magnetosphere is sufficiently disturbed by the solar wind that the trajectories of charged particles in both solar wind and magnetospheric plasma, mainly in the form of electrons and protons, precipitate them into the upper atmosphere (thermosphere/exosphere), where their energy is lost. The resulting ionization and excitation of atmospheric constituents emits light of varying colour and complexity. The form of the aurora, occurring within bands around both polar regions, is also dependent on the amount of acceleration imparted to the precipitating particles. Precipitating protons generally produce optical emissions as incident hydrogen atoms after gaining electrons from the atmosphere. Proton auroras are usually observed at lower latitudes. Different aspects of an aurora are elaborated in various sections below.
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