Chapter 11 The Solar Wind
... kinetic energy density ρu2 /2 = 9.4 × 10−9 erg cm−3 . At any given time, part of the sun’s corona is emitting a low-speed wind, and part is emitting a high-speed wind. (The high-speed winds appear to come from “coronal holes” – regions of low density and low temperature where the magnetic field line ...
... kinetic energy density ρu2 /2 = 9.4 × 10−9 erg cm−3 . At any given time, part of the sun’s corona is emitting a low-speed wind, and part is emitting a high-speed wind. (The high-speed winds appear to come from “coronal holes” – regions of low density and low temperature where the magnetic field line ...
Magnetic Reconnection Project
... • Why is the magnetic energy during magnetic reconnection released as an explosion? – Since reconnection can be fast why isn’t the magnetic energy released as fast as external drivers can supply it? – Need to explain why magnetic reconnection is not always fast. ...
... • Why is the magnetic energy during magnetic reconnection released as an explosion? – Since reconnection can be fast why isn’t the magnetic energy released as fast as external drivers can supply it? – Need to explain why magnetic reconnection is not always fast. ...
Long-term evolution of a dipolar-type magnetosphere interacting
... MHD magnetosphere and the formation of winds and jets and not in the evolution of the disk itself. Therefore, we do not include magnetic diffusivity into our simulations. The disk acts only as a boundary condition for the corona/jet region. In this sense we will follow the ideas developed by OP97. T ...
... MHD magnetosphere and the formation of winds and jets and not in the evolution of the disk itself. Therefore, we do not include magnetic diffusivity into our simulations. The disk acts only as a boundary condition for the corona/jet region. In this sense we will follow the ideas developed by OP97. T ...
VELOCITIES MEASURED IN SMALL-SCALE SOLAR MAGNETIC ELEMENTS Øystein Langangen, Mats Carlsson, and
... We make a mean solar spectrogram by adding together all 250 flat-field spectra. The mean aberration corrected spectrum is then compared to the Fourier transform spectroscope (FTS) atlas of Brault & Neckel (1987). This atlas has proved to be well calibrated in wavelength, and it shows no systematic o ...
... We make a mean solar spectrogram by adding together all 250 flat-field spectra. The mean aberration corrected spectrum is then compared to the Fourier transform spectroscope (FTS) atlas of Brault & Neckel (1987). This atlas has proved to be well calibrated in wavelength, and it shows no systematic o ...
Particle precipitation influence in the conductivity of the auroral
... iv) integrate σP and σH in altitude to determine the respective conductances ΣP and ΣH . However, this physical concept is significantly limited by the practical procedures and assumptions to construct a global model and the average statistical models do not accurately describe an instantaneous iono ...
... iv) integrate σP and σH in altitude to determine the respective conductances ΣP and ΣH . However, this physical concept is significantly limited by the practical procedures and assumptions to construct a global model and the average statistical models do not accurately describe an instantaneous iono ...
A precise contact force measuring method for overhead catenary
... The contact force between pantograph and contact wire determines the dynamic performance of current collection. Large contact force furthers wear of contact wire and also causes fatigue of the wire. On the other hand, too small contact force gives rise to arcing. Therefore, keeping contact force in ...
... The contact force between pantograph and contact wire determines the dynamic performance of current collection. Large contact force furthers wear of contact wire and also causes fatigue of the wire. On the other hand, too small contact force gives rise to arcing. Therefore, keeping contact force in ...
Local conservative regularizations of compressible magnetohydrodynamic and neutral flows
... tive regularization νuxx . Also well-known is the NavierStokes (NS) viscous regularization (ν∇2 v) of inviscid Euler equations with its counterpart in visco-resistive MHD. At present, it is an open problem whether these 3D dissipative systems are truly regular (i.e. with classical solutions for all ...
... tive regularization νuxx . Also well-known is the NavierStokes (NS) viscous regularization (ν∇2 v) of inviscid Euler equations with its counterpart in visco-resistive MHD. At present, it is an open problem whether these 3D dissipative systems are truly regular (i.e. with classical solutions for all ...
Development of electric currents in a magnetic field configuration
... Context. In the past the role of magnetic null points in the generation of electric currents was investigated mainly in the close vicinity of the null, with perturbations being applied at nearby boundaries, or for a magnetic null configuration with a dome-shaped fan. In the solar atmosphere, however ...
... Context. In the past the role of magnetic null points in the generation of electric currents was investigated mainly in the close vicinity of the null, with perturbations being applied at nearby boundaries, or for a magnetic null configuration with a dome-shaped fan. In the solar atmosphere, however ...
Modified Coulomb Potential of QED in a strong magnetic field
... The electron-positron peaks are due to the decay of a bound state formed in this new phase induced by a strong and rapidly varying EM field present in the neighborhood of colliding heavy ions ...
... The electron-positron peaks are due to the decay of a bound state formed in this new phase induced by a strong and rapidly varying EM field present in the neighborhood of colliding heavy ions ...
Multidimensional and inhomogeneity effects on scattering
... In order to measure magnetic fields pervading solar prominences one usually performs spectropolarimetric inversion. One of the most common choices for such procedure is He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the ma ...
... In order to measure magnetic fields pervading solar prominences one usually performs spectropolarimetric inversion. One of the most common choices for such procedure is He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the ma ...
What is Beneath the Sunspots? Home Page ____________________________________________
... concentrated in circular areas with a typical size of 30 to 50 Mm [6], and the field lines at these points are usually directed away from the surface, or vertical field [22], and that, while the main plasma body raises towards the surface or drifts westwards, it continually produced intense magnetic ...
... concentrated in circular areas with a typical size of 30 to 50 Mm [6], and the field lines at these points are usually directed away from the surface, or vertical field [22], and that, while the main plasma body raises towards the surface or drifts westwards, it continually produced intense magnetic ...
The Electro Magnetic Cannon Saba Zargham, Hamid
... A “speedometer” was designed to determine the speed of the ball. This device is consistent of four sensors in order to reach the most accurate result. Experiments were done with solenoids of 5 cm length, 3 cm outer diameter, and three different inner diameters of 10, 8, 6 mm. (Fig.5) ...
... A “speedometer” was designed to determine the speed of the ball. This device is consistent of four sensors in order to reach the most accurate result. Experiments were done with solenoids of 5 cm length, 3 cm outer diameter, and three different inner diameters of 10, 8, 6 mm. (Fig.5) ...
55_1.pdf
... knowledge and understanding of the coronal magnetic field has instead come from two indirect sources. Assuming that density reflects magnetic field, we have gleaned the Sun’s magnetism from density structure observed in whitelight images. Polar plumes, the small-scale, faint, thin, hair-like structu ...
... knowledge and understanding of the coronal magnetic field has instead come from two indirect sources. Assuming that density reflects magnetic field, we have gleaned the Sun’s magnetism from density structure observed in whitelight images. Polar plumes, the small-scale, faint, thin, hair-like structu ...
Experimental Evidence for a Reduction in Electron Thermal
... this correction, it becomes clear that the thermal conduction in the midradius is dominated by magnetic diffusion throughout most of the sawtooth cycle. In the core, the magnetic diffusion likely accounts for all of the measured !e after the crash, but there are obviously other mechanisms that becom ...
... this correction, it becomes clear that the thermal conduction in the midradius is dominated by magnetic diffusion throughout most of the sawtooth cycle. In the core, the magnetic diffusion likely accounts for all of the measured !e after the crash, but there are obviously other mechanisms that becom ...
talk-tutorial - Helioseismic and Magnetic Imager
... solar atmosphere. Presently, there are 2 approaches to this problem: • (1) Develop coupled models of the different regions, which communicate across a codecode interface • (2) Implement numerical techniques that can accommodate greatly different physical conditions ...
... solar atmosphere. Presently, there are 2 approaches to this problem: • (1) Develop coupled models of the different regions, which communicate across a codecode interface • (2) Implement numerical techniques that can accommodate greatly different physical conditions ...
force
... • Equal forces acting on one object in opposite directions are called balanced forces • For an object that is not moving, the result of balanced forces is no motion • For an object that is moving, the result of balanced forces is constant velocity ...
... • Equal forces acting on one object in opposite directions are called balanced forces • For an object that is not moving, the result of balanced forces is no motion • For an object that is moving, the result of balanced forces is constant velocity ...
on limiting the thickness of the solar tachocline
... (1992) attribute the thinness of the tachocline to anisotropic turbulence. They argue that, similar to Earth’s atmosphere, the solar tachocline, lying mostly in the stably stratified interior, opposes vertical turbulence. They show that the width of the tachocline is then determined by the degree of ...
... (1992) attribute the thinness of the tachocline to anisotropic turbulence. They argue that, similar to Earth’s atmosphere, the solar tachocline, lying mostly in the stably stratified interior, opposes vertical turbulence. They show that the width of the tachocline is then determined by the degree of ...
Astronomy Astrophysics
... the magnetic field beneath each can be very different. If one changes the plot in Fig. 2 to include flares from only a single GOES classification there is little difference in the appearance other than to simply reduce the number of points plotted as the large scatter remains. To limit the effects o ...
... the magnetic field beneath each can be very different. If one changes the plot in Fig. 2 to include flares from only a single GOES classification there is little difference in the appearance other than to simply reduce the number of points plotted as the large scatter remains. To limit the effects o ...
Lecture 2, the physics of atoms in magnetic fields
... Then magnetic energy is W ~ (evB/c)a0 ~ (eħ/mc)B, and magnetic moment of an electron must be of order (eħ/mc) (eħ/2mc) is called the Bohr magneton. It is magnetic moment of electron spin or of a single unit of electron orbital ...
... Then magnetic energy is W ~ (evB/c)a0 ~ (eħ/mc)B, and magnetic moment of an electron must be of order (eħ/mc) (eħ/2mc) is called the Bohr magneton. It is magnetic moment of electron spin or of a single unit of electron orbital ...
Relativistic electron-positron plasmas
... this, or some large-scale turbulence is required is currently under debate. In particular, it is not clear whether the small-scale fields generated by plasma instabilities can survive for long times needed to explain the astrophysical sources of radiation. 3) Mechanisms of electron and ion injection ...
... this, or some large-scale turbulence is required is currently under debate. In particular, it is not clear whether the small-scale fields generated by plasma instabilities can survive for long times needed to explain the astrophysical sources of radiation. 3) Mechanisms of electron and ion injection ...
Article: - Swift - Sonoma State University
... will continue its motion in a straight line, unless acted on by an unbalanced force. And we need to remember that the Earth is spinning! So Swift and its rocket are also moving in the direction of the Earth’s spin, at the time that they leave the Earth’s surface. The eastward velocity of the spinnin ...
... will continue its motion in a straight line, unless acted on by an unbalanced force. And we need to remember that the Earth is spinning! So Swift and its rocket are also moving in the direction of the Earth’s spin, at the time that they leave the Earth’s surface. The eastward velocity of the spinnin ...
Magnetic field structure in single late
... at the 2-m Bernard Lyot Télescope (TBL) at Pic du Midi Observatory, France, and ESPaDOnS (Donati et al. 2006a), which operates at the 3.6-m Canada-France-Hawaii Telescope (CFHT) of Mauna Kea Observatory, Hawaii. In polarimetric mode, both have a spectral resolution of about 65 000 and a nearly conti ...
... at the 2-m Bernard Lyot Télescope (TBL) at Pic du Midi Observatory, France, and ESPaDOnS (Donati et al. 2006a), which operates at the 3.6-m Canada-France-Hawaii Telescope (CFHT) of Mauna Kea Observatory, Hawaii. In polarimetric mode, both have a spectral resolution of about 65 000 and a nearly conti ...
Growth of the inner core in the mean
... scales of the boundary layers, where helicity of the incompressible fluid is generated, are too small to generate the magnetic field. It means that extrapolation of helicity profiles to the realistic E can lead to the break of the magnetic field generation at all. However, in the compressible fluid ...
... scales of the boundary layers, where helicity of the incompressible fluid is generated, are too small to generate the magnetic field. It means that extrapolation of helicity profiles to the realistic E can lead to the break of the magnetic field generation at all. However, in the compressible fluid ...
Lorentz force velocimetry
Lorentz force velocimetry (LFV) is a noncontact electromagnetic flow measurement technique. LFV is particularly suited for the measurement of velocities in liquid metals like steel or aluminium and is currently under development for metallurgical applications.The measurement of flow velocities in hot and aggressive liquids such as liquid aluminum and molten glass constitutes one of the grand challenges of industrial fluid mechanics. Apart from liquids, LFV can also be used to measure the velocity of solid materials as well as for detection of micro-defects in their structures.A Lorentz force velocimetry system is called Lorentz force flowmeter (LFF). A LFF measures the integrated or bulk Lorentz force resulting from the interaction between a liquid metal in motion and an applied magnetic field. In this case the characteristic length of the magnetic field is of the same order of magnitude as the dimensions of the channel. It must be addressed that in the case where localized magnetic fields are used, it is possible to perform local velocity measurements and thus the term Lorentz force velocimeter is used.