Non-thermal emission processes in massive binaries*
... - the emission of thermal X-rays, likely produced by hydrodynamic shocks between plasma shells travelling at different velocities in the wind of isolated stars, and leading to local temperature enhancements of a few 106 K (see Feldmeier et al (1997)). The thermal nature of the X-rays produced within ...
... - the emission of thermal X-rays, likely produced by hydrodynamic shocks between plasma shells travelling at different velocities in the wind of isolated stars, and leading to local temperature enhancements of a few 106 K (see Feldmeier et al (1997)). The thermal nature of the X-rays produced within ...
Observations of the Magnetic Fields Inside and Outside the
... Canadian TV operations for days. In January 1997, another solar energy burst permanently disabled the US AT&T satellite, costing nearly $150 millions US (e.g., Curren 1997 ) - it did this pushing the Earth's magnetosphere boundary much closer to Earth, inside the satellite's orbit around Earth, expo ...
... Canadian TV operations for days. In January 1997, another solar energy burst permanently disabled the US AT&T satellite, costing nearly $150 millions US (e.g., Curren 1997 ) - it did this pushing the Earth's magnetosphere boundary much closer to Earth, inside the satellite's orbit around Earth, expo ...
Ionization in atmospheres of Brown Dwarfs and extrasolar planets IV
... are set to the solar values throughout this paper. We consider a model atmosphere of a brown dwarf, with a surface gravity of log g = 5 and an effective temperature of Teff = 1500 K, as well as model atmospheres for two example giant gas planets, both with log g = 3. The effective temperatures of fr ...
... are set to the solar values throughout this paper. We consider a model atmosphere of a brown dwarf, with a surface gravity of log g = 5 and an effective temperature of Teff = 1500 K, as well as model atmospheres for two example giant gas planets, both with log g = 3. The effective temperatures of fr ...
potenza dei jet nei nuclei galattici attivi radio
... radiation fields responsible for photoionizing the galactic nebulae where they came from. AGNs are thought to host at their centers a massive compact object with mass M ∼ 106 –109 M , where M = 1.9891 · 1033 g corresponds to the unit solar mass. Another feature of an AGN’s optical-UV (Ultra Violet ...
... radiation fields responsible for photoionizing the galactic nebulae where they came from. AGNs are thought to host at their centers a massive compact object with mass M ∼ 106 –109 M , where M = 1.9891 · 1033 g corresponds to the unit solar mass. Another feature of an AGN’s optical-UV (Ultra Violet ...
The energy spectrum of cosmic electrons measured with the MAGIC
... Cosmic rays give us the unique possibility to learn more about our universe at distances out of mankind’s reach. They travel close to the speed of light and can cover huge distances of up to 93 billion light years. However, not all cosmic rays are equally likely to reach the Earth from such distance ...
... Cosmic rays give us the unique possibility to learn more about our universe at distances out of mankind’s reach. They travel close to the speed of light and can cover huge distances of up to 93 billion light years. However, not all cosmic rays are equally likely to reach the Earth from such distance ...
Irregular Shock Refraction in Magnetohydrodynamics
... deuterium-tritium fuel contained within the capsule [1]. When this shock interacts with the perturbed material interfaces within the capsule, vorticity is deposited on them by the shock refraction process. This is the origin of the Richtmyer-Meshkov instability (RMI) that promotes mixing between the ...
... deuterium-tritium fuel contained within the capsule [1]. When this shock interacts with the perturbed material interfaces within the capsule, vorticity is deposited on them by the shock refraction process. This is the origin of the Richtmyer-Meshkov instability (RMI) that promotes mixing between the ...
Construction and Operation of an Axion Helioscope
... trapped in the SN core has been estimated by Turner (1988). The uncertainty in this range is rather severe, perhaps as much as an order of magnitude on either end of the window. This means that the actually excluded regime may be much smaller than stated in Eq. (9). Also, however, the regime where a ...
... trapped in the SN core has been estimated by Turner (1988). The uncertainty in this range is rather severe, perhaps as much as an order of magnitude on either end of the window. This means that the actually excluded regime may be much smaller than stated in Eq. (9). Also, however, the regime where a ...
Dynamical response of magnetic tubes to transverse
... excitation generates longitudinal body waves of twice the frequency. This mode conversion process is not very efficient. A very important result of our computations, however, is the efficient generation of a non-axisymmetric longitudinal body wave which does not derive from magnetic tension forces, ...
... excitation generates longitudinal body waves of twice the frequency. This mode conversion process is not very efficient. A very important result of our computations, however, is the efficient generation of a non-axisymmetric longitudinal body wave which does not derive from magnetic tension forces, ...
Modeling of Intense Laser Driven High Energy Density Plasmas
... states of plasmas with temperatures exceeding ten million degrees Celsius and pressures exceeding one billion earth atmospheres. These high energy density conditions are driven at the microscopic scale by dense currents of relativistic electrons, oscillating violently in the intense laser fields, as ...
... states of plasmas with temperatures exceeding ten million degrees Celsius and pressures exceeding one billion earth atmospheres. These high energy density conditions are driven at the microscopic scale by dense currents of relativistic electrons, oscillating violently in the intense laser fields, as ...
Origin of solar surface activity and sunspots Sarah Jabbari Nordita, Stockholm, Sweden
... context, the excitation of NEMPI in spherical geometry was studied here from a meanfield dynamo that generates the background magnetic field. Previous studies have shown that for NEMPI to work, the background field can neither be too weak nor too strong. To satisfy this condition for the dynamo-gene ...
... context, the excitation of NEMPI in spherical geometry was studied here from a meanfield dynamo that generates the background magnetic field. Previous studies have shown that for NEMPI to work, the background field can neither be too weak nor too strong. To satisfy this condition for the dynamo-gene ...
The Earliest Stages of Star and Planet Formation: Core Collapse
... The formation of stars and planets are connected through disks. Our theoretical understanding of disk formation has undergone drastic changes in recent years, and we are on the brink of a revolution in disk observation enabled by ALMA. Large rotationally supported circumstellar disks, although commo ...
... The formation of stars and planets are connected through disks. Our theoretical understanding of disk formation has undergone drastic changes in recent years, and we are on the brink of a revolution in disk observation enabled by ALMA. Large rotationally supported circumstellar disks, although commo ...
Universitat Autònoma de Barcelona Observing the VHE Gamma Ray Sky
... and Cesarsky, 1983). From the discovery of very narrow X-ray filaments (VHlk et al., 2005) in the shock regions of supernova remnants it is known that the magnetic flux density can be up to two or three orders of magnitude higher, from ∼ 10−10 T to ∼ 10−8 T; with these values the above equation pred ...
... and Cesarsky, 1983). From the discovery of very narrow X-ray filaments (VHlk et al., 2005) in the shock regions of supernova remnants it is known that the magnetic flux density can be up to two or three orders of magnitude higher, from ∼ 10−10 T to ∼ 10−8 T; with these values the above equation pred ...
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 ...
Magnetism in Isolated and Binary White Dwarfs
... Following the discovery by Babcock (1947) of a polar magnetic Ðeld of D1500 G in the Ap star 78 Vir, it became apparent that sizeable magnetic Ðelds were present in stars other than the Sun. If magnetic Ñux was conserved during stellar evolution, white dwarfs should be expected to have magnetic Ðeld ...
... Following the discovery by Babcock (1947) of a polar magnetic Ðeld of D1500 G in the Ap star 78 Vir, it became apparent that sizeable magnetic Ðelds were present in stars other than the Sun. If magnetic Ñux was conserved during stellar evolution, white dwarfs should be expected to have magnetic Ðeld ...
on the rotational dynamics of magnetically threaded disks around
... flow, artificial in the sense that the angular motion could easily be modified by the huge viscous stress estimated for the inner parts of the disk. For a disk around a nonmagnetized star, Glatzel (1992) solved this problem without making the assumption that the rotation rate is Keplerian except in ...
... flow, artificial in the sense that the angular motion could easily be modified by the huge viscous stress estimated for the inner parts of the disk. For a disk around a nonmagnetized star, Glatzel (1992) solved this problem without making the assumption that the rotation rate is Keplerian except in ...
Quantum Theory of Neutrino Spin
... where µ0 = e/2m is the Bohr magneton, mν and m are the neutrino and electron masses, respectively. There are also models [2] in which much large values for magnetic moments of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic ...
... where µ0 = e/2m is the Bohr magneton, mν and m are the neutrino and electron masses, respectively. There are also models [2] in which much large values for magnetic moments of neutrinos are predicted. So far, the most stringent laboratory constraints on the electron, muon, and tau neutrino magnetic ...
Author`s personal copy - Institute of Physics Belgrade Roundcube
... A certain interest for the processes of aerosol forming in conditions of geocosmos can represent and the effect of solid particles of micron size forming in collisions of optically excited alkali atoms with hydrogen (Tam et al., 1977). The rate of the collisional ionization processes in an absorbing ...
... A certain interest for the processes of aerosol forming in conditions of geocosmos can represent and the effect of solid particles of micron size forming in collisions of optically excited alkali atoms with hydrogen (Tam et al., 1977). The rate of the collisional ionization processes in an absorbing ...
The Plasma Physics Processes that Drive Ring Current
... Geomagnetic storms result when energetic particles of solar and ionospheric origin fill Earth’s inner magnetosphere and create a strong westward current, known as the ring current. This dissertation presents results from investigating the plasma dynamics that contribute to the development of Earth’s ...
... Geomagnetic storms result when energetic particles of solar and ionospheric origin fill Earth’s inner magnetosphere and create a strong westward current, known as the ring current. This dissertation presents results from investigating the plasma dynamics that contribute to the development of Earth’s ...
Molecular Clouds and the Onset of Star Formation
... cloud cores. The clouds have been characterized as both clumpy and filamentary. The general properties on selected scales are listed in Table 2.1. In fact each type of structure exhibits a range of properties [335]. The clumpiness of a molecular cloud can be characterized by a so-called volume filli ...
... cloud cores. The clouds have been characterized as both clumpy and filamentary. The general properties on selected scales are listed in Table 2.1. In fact each type of structure exhibits a range of properties [335]. The clumpiness of a molecular cloud can be characterized by a so-called volume filli ...
Telescope Bernard Lyot/Narval The Observatory of Stellar Magnetism
... (requires a large spatial spectral and temporal resolution) ...
... (requires a large spatial spectral and temporal resolution) ...
Can a Fast-Mode EUV Wave Generate a Stationary Front?
... function. The AIA 193 Å emission of the numerical results in Figure 3 is presented in Figure 4, which shows the evolution of the AIA 193 Å base-difference map (color) and the magnetic field (solid lines). Note that the base-difference map is derived by subtracting the initial intensity from each tim ...
... function. The AIA 193 Å emission of the numerical results in Figure 3 is presented in Figure 4, which shows the evolution of the AIA 193 Å base-difference map (color) and the magnetic field (solid lines). Note that the base-difference map is derived by subtracting the initial intensity from each tim ...
Coronal energy input and dissipation in a solar active region 3D
... these loops are located. We also see a slight increase of the viscous heating per particle at these heights, but in the upper corona the viscous heating per particle remains roughly unchanged. Above the smaller hot AR core FOV, the Ohmic heating clearly dominates over the viscous heating by a factor ...
... these loops are located. We also see a slight increase of the viscous heating per particle at these heights, but in the upper corona the viscous heating per particle remains roughly unchanged. Above the smaller hot AR core FOV, the Ohmic heating clearly dominates over the viscous heating by a factor ...
Sardinia_SA - Mullard Space Science Laboratory
... “zero velocity surface” (Roche Lobe) so that some gas might be lost at the L1 point ...
... “zero velocity surface” (Roche Lobe) so that some gas might be lost at the L1 point ...
Polywell
The polywell is a type of nuclear fusion reactor that uses an electric field to heat ions to fusion conditions. It is closely related to the magnetic mirror, the fusor, the biconic cusp and the high beta fusion reactor. A set of electromagnets generates a magnetic field which traps electrons. This creates a negative voltage, which attracts positive ions. As the ions accelerate towards the negative center, their kinetic energy rises. If the ions collide in the center, they can fuse.The polywell is one of many devices that use an electric field to heat ions to fusion conditions. This branch of fusion research is known as inertial electrostatic confinement. The polywell was developed by Robert Bussard, as an improvement over the fusor. His company, EMC2, Inc., developed the initial devices for the U.S. Navy.