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 ...
... 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 ...
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 ...
... 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 ...
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 ...
... 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 ...
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). ...
... 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
... 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 ...
... 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 ...
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.