Magnetised
A signature in the X-ray light emitted by a highly magnetised dead star known as a magnetar suggests the star has a solid surface with no atmosphere, according to a new study by an international collaboration co-led by UCL researchers.
magnetised
Quantum theory predicts that light propagating in a strongly magnetised environment is polarised in two directions, parallel and perpendicular to the magnetic field. The amount and direction of the observed polarisation bear the imprint of the magnetic field structure and of the physical state of matter in the vicinity of the neutron star, providing information inaccessible otherwise.
"General Fusion wants to transform how the world is energised by replicating the process that powers the sun and the stars," said AL_A when the project was first unveiled in 2020. "Their prototype fusion facility will be the first magnetised fusion facility in the world."
If your watch does get magnetised, you don't normally know or realise exactly when it happened. This can be confusing, because the unexpected timekeeping change seems to have come out of nowhere. Contrast this with problems like dropping the watch, or getting water into it, when you can instantly see the problem and usually know exactly when and how it happened.
The small amount of motion, here and with the ETA movement, when the magnet approaches illustrates that both vintage and new Nivarox springs are only slightly affected by magnets. To be fair, this little magnet is very strong, and the balance spring performs very well under these circumstances. The other steel parts of the watch will have been fully magnetised by this action, and will need de-magnetising.
Some theories concerning the aggregation of magnetic and non-magnetic dust particles show that the resulting bigger objects could also remain magnetised, allowing them to also be influenced by the magnetic fields of the proto-planetary disc.
A simple study to show the benefits of magnetised water is to take two identical plants, feed one the magnetised Mineral Pot Water and the other Tap Water and see the difference in health & growth (Many progressive farmers are magnetising their water supplies for greater crop yeilds)
When making magnetised water, the N pole must be used. The N pole of the magnets improves work efficiency, promotes the metabolism, has healing effects, relieves pain, is useful for the treatment of allergies and is good for calming the emotions.
The method for making magnetised water is based on the principle that water molecules become smaller by going through the process of hydrogen separation and recombination when the water flows through a powerful magnetic field. If water is placed above a magnet or allowed to flow through a magnetic field, electricity occurs in the water when the water flows through the magnetic field, by which the water gets ionised and becomes magnetised water. When a magnetic field is applied to water, changes in its physical property, magnetic susceptibility, light absorption, viscosity coefficient, electrical resistance and surface tension take place.
Cluster plasmas are magnetised already at very low magnetic field strength. Low collisionality implies that conservation of the first adiabatic invariant results in an anisotropic viscous stress (Braginskii viscosity) or, equivalently, anisotropic plasma pressure. This triggers firehose and mirror instabilities, which have growth rates proportional to the wavenumber down to scales of the order of ion Larmor radius. This means that MHD equations with Braginskii viscosity are not well posed and fully kinetic description is necessary. In this paper, we review the basic picture of small-scale dynamo in the cluster plasma and attempt to reconcile it with the existence of plasma instabilities at collisionless scales.
This paper considers the parametric decay of an electromagnetic wave incident on a weakly-inhomogeneous magnetised plasma into a Langmuir wave and an ion-acoustic wave. The Vlasov model is used in order to calculate the low-frequency electron-density perturbation produced by the beating of the side-band modes with the pump wave. The results show that the threshold value of the pump wave to undergo a decay instability drops in the presence of an inhomogeneity in the plasma.
The stability of a collisionless, magnetised plasma to local convectivedisturbances is examined, with a focus on kinetic and finite-Larmor-radiuseffects. Specific application is made to the outskirts of galaxy clusters,which contain hot and tenuous plasma whose temperature increases in thedirection of gravity. At long wavelengths (the "drift-kinetic" limit), weobtain the kinetic version of the magnetothermal instability (MTI) and itsAlfv\'enic counterpart (Alfv\'enic MTI), which were previously discovered andanalysed using a magnetofluid (i.e. Braginskii) description. At sub-ion-Larmorscales, we discover an overstability driven by the electron temperaturegradient of kinetic-Alfv\'en drift waves -- the electron MTI (eMTI) -- whosegrowth rate is even larger than the standard MTI. At intermediate scales, wefind that ion finite-Larmor-radius effects tend to stabilise the plasma. Wediscuss the physical interpretation of these instabilities in detail, andcompare them both with previous work on magnetised convection in a collisionalplasma and with temperature-gradient-driven drift-wave instabilities well-knownto the magnetic-confinement-fusion community. The implications of having bothfluid and kinetic scales simultaneously driven unstable by the same temperaturegradient are briefly discussed.
We consider a model for the propagation and absorption of electromagnetic waves (in the time-harmonic regime) in a magnetised plasma. We present a rigorous derivation of the model and several boundary conditions modelling wave injection into the plasma. Then we propose several variational formulations, mixed and non-mixed, and prove their well-posedness thanks to a theorem by Sébelin et al. Finally, we propose a non-overlapping domain decomposition framework, show its well-posedness and equivalence with the one-domain formulation. These results appear strongly linked to the spectral properties of the plasma dielectric tensor.
N2 - Space Infrared Telescope for Cosmology and Astrophysics (SPICA), the cryogenic infrared space telescope recently pre-selected for a `Phase A' concept study as one of the three remaining candidates for European Space Agency (ESA's) fifth medium class (M5) mission, is foreseen to include a far-infrared polarimetric imager [SPICA-POL, now called B-fields with BOlometers and Polarizers (B-BOP)], which would offer a unique opportunity to resolve major issues in our understanding of the nearby, cold magnetised Universe. This paper presents an overview of the main science drivers for B-BOP, including high dynamic range polarimetric imaging of the cold interstellar medium (ISM) in both our Milky Way and nearby galaxies. Thanks to a cooled telescope, B-BOP will deliver wide-field 100-350 μm images of linearly polarised dust emission in Stokes Q and U with a resolution, signal-to-noise ratio, and both intensity and spatial dynamic ranges comparable to those achieved by Herschel images of the cold ISM in total intensity (Stokes I). The B-BOP 200 μm images will also have a factor 30 higher resolution than Planck polarisation data. This will make B-BOP a unique tool for characterising the statistical properties of the magnetised ISM and probing the role of magnetic fields in the formation and evolution of the interstellar web of dusty molecular filaments giving birth to most stars in our Galaxy. B-BOP will also be a powerful instrument for studying the magnetism of nearby galaxies and testing Galactic dynamo models, constraining the physics of dust grain alignment, informing the problem of the interaction of cosmic rays with molecular clouds, tracing magnetic fields in the inner layers of protoplanetary disks, and monitoring accretion bursts in embedded protostars.
AB - Space Infrared Telescope for Cosmology and Astrophysics (SPICA), the cryogenic infrared space telescope recently pre-selected for a `Phase A' concept study as one of the three remaining candidates for European Space Agency (ESA's) fifth medium class (M5) mission, is foreseen to include a far-infrared polarimetric imager [SPICA-POL, now called B-fields with BOlometers and Polarizers (B-BOP)], which would offer a unique opportunity to resolve major issues in our understanding of the nearby, cold magnetised Universe. This paper presents an overview of the main science drivers for B-BOP, including high dynamic range polarimetric imaging of the cold interstellar medium (ISM) in both our Milky Way and nearby galaxies. Thanks to a cooled telescope, B-BOP will deliver wide-field 100-350 μm images of linearly polarised dust emission in Stokes Q and U with a resolution, signal-to-noise ratio, and both intensity and spatial dynamic ranges comparable to those achieved by Herschel images of the cold ISM in total intensity (Stokes I). The B-BOP 200 μm images will also have a factor 30 higher resolution than Planck polarisation data. This will make B-BOP a unique tool for characterising the statistical properties of the magnetised ISM and probing the role of magnetic fields in the formation and evolution of the interstellar web of dusty molecular filaments giving birth to most stars in our Galaxy. B-BOP will also be a powerful instrument for studying the magnetism of nearby galaxies and testing Galactic dynamo models, constraining the physics of dust grain alignment, informing the problem of the interaction of cosmic rays with molecular clouds, tracing magnetic fields in the inner layers of protoplanetary disks, and monitoring accretion bursts in embedded protostars.