Oieroset_ARTEMIS_tail_science
... Two-spacecraft measurements can be used to identify non-linear KH vortices which have been suggested to provide significant solar wind entry into the tail during northward IMF conditions. ...
... Two-spacecraft measurements can be used to identify non-linear KH vortices which have been suggested to provide significant solar wind entry into the tail during northward IMF conditions. ...
Static structure factor of electrons around a heavy positively charged
... charged particle, such as a proton or an heavy ion in a one component classical rare plasma which one encounters in semiconductors, ionosphere and intergalactic space to name a few examples, has been derived taking into account nonlinear effects [1]. The expression is dependent upon certain distance ...
... charged particle, such as a proton or an heavy ion in a one component classical rare plasma which one encounters in semiconductors, ionosphere and intergalactic space to name a few examples, has been derived taking into account nonlinear effects [1]. The expression is dependent upon certain distance ...
Two-stream instability in collisionless shocks and foreshock
... plasma slabs are magnetized such that ωp = 2ωc and β = 0.05. The magnetic field B is aligned with the z-axis. The slabs move along the x-direction and collide at a speed of 4.5 VA . A forward and reverse shock develop, as shown by the supplementary movie 1. The plasma in the overlap region of the pl ...
... plasma slabs are magnetized such that ωp = 2ωc and β = 0.05. The magnetic field B is aligned with the z-axis. The slabs move along the x-direction and collide at a speed of 4.5 VA . A forward and reverse shock develop, as shown by the supplementary movie 1. The plasma in the overlap region of the pl ...
Discovery Of A Magnetic Field In The O9 Sub-Giant Star HD
... The longitudinal magnetic field (B ) was inferred from each LSD Stokes V profile in the manner described by Silvester et al. (2009). The longitudinal field measurements, which are reported in Table 1, vary between −167 G and +282 G, with a typical uncertainty of 20–40 G. While the longitudinal fie ...
... The longitudinal magnetic field (B ) was inferred from each LSD Stokes V profile in the manner described by Silvester et al. (2009). The longitudinal field measurements, which are reported in Table 1, vary between −167 G and +282 G, with a typical uncertainty of 20–40 G. While the longitudinal fie ...
PDF
... universe). For the typical width of the universe the latency for excess correlation across its extent would be about 8 min. In other words it would not be “instantaneous”, although it would appear as such for current comparisons even when “perceiving” distances of separation of thousands of parsecs. ...
... universe). For the typical width of the universe the latency for excess correlation across its extent would be about 8 min. In other words it would not be “instantaneous”, although it would appear as such for current comparisons even when “perceiving” distances of separation of thousands of parsecs. ...
my brief profile
... Equation by replacing zero with a fundamental term , thereby trying to explain Super fluidity concepts by taking magnetic monopole assumptions and magnetic field generation during rotation of Super fluid Helium which can be utilized in understanding Pulsars ( Pulsating Radio stars) or neutron stars ...
... Equation by replacing zero with a fundamental term , thereby trying to explain Super fluidity concepts by taking magnetic monopole assumptions and magnetic field generation during rotation of Super fluid Helium which can be utilized in understanding Pulsars ( Pulsating Radio stars) or neutron stars ...
Black Hole`` Systems.`
... accretion disk. The magnetic propeller also creates radial outflows of atomic nuclei (shown in indigo blue) and relativistic jets of electrons (shown in red) along the rotation axis. A bright blue-white ring forms where the MECO's rotating magnetic field sweeps the inner edge of the accretion disk, ...
... accretion disk. The magnetic propeller also creates radial outflows of atomic nuclei (shown in indigo blue) and relativistic jets of electrons (shown in red) along the rotation axis. A bright blue-white ring forms where the MECO's rotating magnetic field sweeps the inner edge of the accretion disk, ...
model the Earth`s and Sun`s magnetic fields using a
... a cow magnet along the axis of the Earth in the picture (over the magnet in the picture). Where is the North Pole in the picture? The South Pole? Do these areas relate to the poles of the magnet? 6. Explain that the magnetic North Pole of the Earth is relatively close to the geographic North Pole; t ...
... a cow magnet along the axis of the Earth in the picture (over the magnet in the picture). Where is the North Pole in the picture? The South Pole? Do these areas relate to the poles of the magnet? 6. Explain that the magnetic North Pole of the Earth is relatively close to the geographic North Pole; t ...
Radiative energy transport
... • In the radiative zone of the solar interior, the energy is transported by radiation: mean free path of photons is small (~2 cm). • The radiative energy exchange in the photosphere defines its temperature structure and is responsible for convective instability. • In the photosphere photons escape: ...
... • In the radiative zone of the solar interior, the energy is transported by radiation: mean free path of photons is small (~2 cm). • The radiative energy exchange in the photosphere defines its temperature structure and is responsible for convective instability. • In the photosphere photons escape: ...