Thermal Convection, Magnetic Field, and Differential Rotation in
... For example, Charbonneau et al. (1999) show that the center of the tachocline is rt /R⊙ = 0.693 ± 0.003 at the equator which is below the base of the convection zone and rt /R⊙ = 0.717 ± 0.003 at the pole which is slightly above the base. Although the thickness of the tachocline is still controversi ...
... For example, Charbonneau et al. (1999) show that the center of the tachocline is rt /R⊙ = 0.693 ± 0.003 at the equator which is below the base of the convection zone and rt /R⊙ = 0.717 ± 0.003 at the pole which is slightly above the base. Although the thickness of the tachocline is still controversi ...
X-ray Emission Line Profiles from ... Confined Wind Shock Model
... of 10- 6 solar masses per year, a terminal velocity of 2500 km s-1, and a radius of 15 R 8 , we find the typical wind density to be about 1010 cm- 3 . Hot stars must use radiation to drive their stellar winds, rather than gas pressure, ...
... of 10- 6 solar masses per year, a terminal velocity of 2500 km s-1, and a radius of 15 R 8 , we find the typical wind density to be about 1010 cm- 3 . Hot stars must use radiation to drive their stellar winds, rather than gas pressure, ...
General chemistry laboratory activities, Lorentz
... effects of the glass), which is usually 20°C. Cylinders can be graduated with stopper polished without spout and are also no-tier cylinders. Anyway, with graduated cylinders measurements are approximate. To measure the volume of a liquid with the cylinder (liquid transparent and wetting cylinder wal ...
... effects of the glass), which is usually 20°C. Cylinders can be graduated with stopper polished without spout and are also no-tier cylinders. Anyway, with graduated cylinders measurements are approximate. To measure the volume of a liquid with the cylinder (liquid transparent and wetting cylinder wal ...
Irregular Shock Refraction in Magnetohydrodynamics
... Figure 4: Solution regimes for the MHD shock refraction problem for M = 2, η = 3, γ = 7/5 and varying α and β. For strong magnetic fields (low β), RS and T S are slow shocks in the regular solutions. As β increases, first T S then RS transition to intermediate shocks. These transitions are seen to b ...
... Figure 4: Solution regimes for the MHD shock refraction problem for M = 2, η = 3, γ = 7/5 and varying α and β. For strong magnetic fields (low β), RS and T S are slow shocks in the regular solutions. As β increases, first T S then RS transition to intermediate shocks. These transitions are seen to b ...
application of densitometers to liquid measurement
... measurement system. Whilst there are tables and calculations (discussed later in this paper) enabling density to be referred to conditions other than the measurement conditions enabling the line and laboratory measurements to be referred to the same conditions the calculations themselves add uncerta ...
... measurement system. Whilst there are tables and calculations (discussed later in this paper) enabling density to be referred to conditions other than the measurement conditions enabling the line and laboratory measurements to be referred to the same conditions the calculations themselves add uncerta ...
Collisionless interaction of an energetic laser produced plasma C. Constantin
... and Thiell 1984). An energy of 25 J (more than 4 times the total energy in the ambient plasma) would be sufficient to maintain the required ion-temperatures for a MA = 1 ...
... and Thiell 1984). An energy of 25 J (more than 4 times the total energy in the ambient plasma) would be sufficient to maintain the required ion-temperatures for a MA = 1 ...
The magnetic field configuration of a solar prominence inferred from
... highly inclined with respect to the local vertical (e.g., Athay et al. 1983). For instance, Leroy et al. (1983) found a mean inclination of 60◦ from the local vertical in a sampling of 15 prominences. Their data were limited to single point measurements, and their estimated rms error was about 15◦ . ...
... highly inclined with respect to the local vertical (e.g., Athay et al. 1983). For instance, Leroy et al. (1983) found a mean inclination of 60◦ from the local vertical in a sampling of 15 prominences. Their data were limited to single point measurements, and their estimated rms error was about 15◦ . ...
2014 HSC Physics - Board of Studies
... the direction of the force acting on the cathode ray as a result of the magnetic field? ...
... the direction of the force acting on the cathode ray as a result of the magnetic field? ...
Magnetic resonance imaging of laser polarized liquid xenon
... a variety of fundamental scientific investigations. For example, light scattering experiments near xenon’s critical point have served as powerful probes of universal phenomena such as the range and lifetime of order parameter fluctuations @1#, as well as the ‘‘critical slowing down’’ of diffusive an ...
... a variety of fundamental scientific investigations. For example, light scattering experiments near xenon’s critical point have served as powerful probes of universal phenomena such as the range and lifetime of order parameter fluctuations @1#, as well as the ‘‘critical slowing down’’ of diffusive an ...
Current status of turbulent dynamo theory
... helicity of streamlines (at low conductivity) or of vortex lines (at high conductivity). In this review we discuss our current knowledge of dynamos covering both largescale and small-scale turbulent dynamos. In practice, all dynamos of astrophysical relevance tend to be “fast” and thus have a finite ...
... helicity of streamlines (at low conductivity) or of vortex lines (at high conductivity). In this review we discuss our current knowledge of dynamos covering both largescale and small-scale turbulent dynamos. In practice, all dynamos of astrophysical relevance tend to be “fast” and thus have a finite ...
physics and technology i - OCExternal
... 2. Attend and listen to the pre-lab lecture and take notes in your student manual. Ensure that all questions that you have about the reading or how to work any problems are answered during the pre-lab lecture or that you ask specific questions during the lecture to resolve these misunderstandings fo ...
... 2. Attend and listen to the pre-lab lecture and take notes in your student manual. Ensure that all questions that you have about the reading or how to work any problems are answered during the pre-lab lecture or that you ask specific questions during the lecture to resolve these misunderstandings fo ...
3D WHOLE-PROMINENCE FINE STRUCTURE MODELING
... a more dense spacing only in the y-z plane (see Fig. 4). We further assume that cross-sections of all prominence fine structures are parallel to the y-z plane instead of being strictly perpendicular to the local magnetic field vector. This allows us to significantly simplify the development of this ...
... a more dense spacing only in the y-z plane (see Fig. 4). We further assume that cross-sections of all prominence fine structures are parallel to the y-z plane instead of being strictly perpendicular to the local magnetic field vector. This allows us to significantly simplify the development of this ...
PDF only - at www.arxiv.org.
... measured temperature of the intracluster medium8) at radius R ~ 25 kpc; tidal acceleration is smaller by 2l/R. The most likely force to balance a filament against gravity is that due to the tangential component of a magnetic field, as suggested by the filamentary morphology. Consider first a horizon ...
... measured temperature of the intracluster medium8) at radius R ~ 25 kpc; tidal acceleration is smaller by 2l/R. The most likely force to balance a filament against gravity is that due to the tangential component of a magnetic field, as suggested by the filamentary morphology. Consider first a horizon ...
PDF only
... Dresselhaus Effect [14] and the Rashba Effect [15] have noted the orbitally induced spin transitions during conduction by voltage induction within the bulk and on the surface during conduction, respectively. For all these cases, the spin and magnetics have been limited to the application of the Paul ...
... Dresselhaus Effect [14] and the Rashba Effect [15] have noted the orbitally induced spin transitions during conduction by voltage induction within the bulk and on the surface during conduction, respectively. For all these cases, the spin and magnetics have been limited to the application of the Paul ...
Conceptual Design of the International Axion Observatory (IAXO)
... Peccei-Quinn mechanism [3, 4] proposed to solve the long-standing strong-CP problem [5]. Together with the weakly interacting massive particles (WIMPs) of supersymmetric theories, axions are also favored candidates to solve the Dark Matter (DM) problem [6, 7]. Their appeal comes from the fact that, ...
... Peccei-Quinn mechanism [3, 4] proposed to solve the long-standing strong-CP problem [5]. Together with the weakly interacting massive particles (WIMPs) of supersymmetric theories, axions are also favored candidates to solve the Dark Matter (DM) problem [6, 7]. Their appeal comes from the fact that, ...
Magnetic quenching of turbulent diffusivity - Andrés Muñoz
... theoretical estimates based on mixing-length theory, which suggest much higher values for turbulent diffusivity. To make matters worse, kinematic dynamo simulations cannot yield sustainable magnetic cycles using these theoretical estimates. In this work, we show that magnetic cycles become viable if ...
... theoretical estimates based on mixing-length theory, which suggest much higher values for turbulent diffusivity. To make matters worse, kinematic dynamo simulations cannot yield sustainable magnetic cycles using these theoretical estimates. In this work, we show that magnetic cycles become viable if ...
Probing magnetic fields with Square Kilometre array and its precursors
... inclination of the magnetic field vector to the line of sight and number density of thermal electrons (in cm−3 ), respectively. The integral is carried out along the line of sight from source at r to the the observer. When the emission originates from a single FD, it is equivalent to the Faraday rot ...
... inclination of the magnetic field vector to the line of sight and number density of thermal electrons (in cm−3 ), respectively. The integral is carried out along the line of sight from source at r to the the observer. When the emission originates from a single FD, it is equivalent to the Faraday rot ...
The magnetic field and wind confinement of b Cephei: new clues for
... (e.g. the dashed line labelled ‘‘ ¼ 2f’ crosses the 10-M( star track only once in fig. 2, while it should cross it four times according to fig. 1), implying that their analysis is thus at least partly incorrect. Note that it is not clear either why these authors did not consider the other possible i ...
... (e.g. the dashed line labelled ‘‘ ¼ 2f’ crosses the 10-M( star track only once in fig. 2, while it should cross it four times according to fig. 1), implying that their analysis is thus at least partly incorrect. Note that it is not clear either why these authors did not consider the other possible i ...
7. Paradise Gravity
... Absolute gravity is a long-range interaction between individual ultimatons and the Isle of Paradise, which has “a potential infinity of gravity extension.” 11:8.9 Unlike other later forms of materialization evolved from cosmic force, ultimatons do not gravitationally interact with other ultimatons ...
... Absolute gravity is a long-range interaction between individual ultimatons and the Isle of Paradise, which has “a potential infinity of gravity extension.” 11:8.9 Unlike other later forms of materialization evolved from cosmic force, ultimatons do not gravitationally interact with other ultimatons ...
The imprint of the crustal magnetic field on the thermal
... the average surface temperature is also higher than in the non-magnetic case. The first consequence is an enhancement of the persistent luminosity: the most magnetized objects (magnetars, high-B pulsars) are systematically brighter, and they are much easier to detect than the weakly magnetised ones. ...
... the average surface temperature is also higher than in the non-magnetic case. The first consequence is an enhancement of the persistent luminosity: the most magnetized objects (magnetars, high-B pulsars) are systematically brighter, and they are much easier to detect than the weakly magnetised ones. ...
Dynamics of a Skydiver
... Figures 2 and 3 illustrate the position of the skydiver between the jump and the landing. Contrary to the motion of a regular projectile without air resistance, the horizontal position quickly converges asymptotically to a value of about 350m from the jump site. In approximately 20 seconds, the sky ...
... Figures 2 and 3 illustrate the position of the skydiver between the jump and the landing. Contrary to the motion of a regular projectile without air resistance, the horizontal position quickly converges asymptotically to a value of about 350m from the jump site. In approximately 20 seconds, the sky ...
Sardinia_SA - Mullard Space Science Laboratory
... • Light curves are strongly variable on orbital timescales • If accretion is occurring mainly near one magnetic pole, then, depending on the latitude of the accretion region, this can come into view and disappear over the limb as the synchronised binary rotates: “bright” and “faint” phases ...
... • Light curves are strongly variable on orbital timescales • If accretion is occurring mainly near one magnetic pole, then, depending on the latitude of the accretion region, this can come into view and disappear over the limb as the synchronised binary rotates: “bright” and “faint” phases ...
Surface temperature distribution and absorption features in Isolated
... where the NS orbits a Be star in a very eccentric orbit, accreting material only occasionally when the NS crosses a disk of material surrounding the Be star. Far from the companion, accretion stops and the NS cools and is weakly magnetized. These systems have been used to make radius measurements [8 ...
... where the NS orbits a Be star in a very eccentric orbit, accreting material only occasionally when the NS crosses a disk of material surrounding the Be star. Far from the companion, accretion stops and the NS cools and is weakly magnetized. These systems have been used to make radius measurements [8 ...
Origin and Evolution of Neutron Star Magnetic Fields - if
... to a more massive particle through a Coulomb (or other) collision. However, any decrease in the current I implies a decrease of the magnetic flux Φ = cLI through the stellar equatorial plane, where c is the speed of light, L ∼ R/c is the star’s self-inductance, and R is its radius. [Here and below, I ...
... to a more massive particle through a Coulomb (or other) collision. However, any decrease in the current I implies a decrease of the magnetic flux Φ = cLI through the stellar equatorial plane, where c is the speed of light, L ∼ R/c is the star’s self-inductance, and R is its radius. [Here and below, I ...
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.