English
... expected to work whereas with new technologies from other companies, expectations are not nearly as high.” Mr. East has never been able to rely on any type of level measurement in this particular application and tried to work with other vendors to find a solution but was never presented with any. “W ...
... expected to work whereas with new technologies from other companies, expectations are not nearly as high.” Mr. East has never been able to rely on any type of level measurement in this particular application and tried to work with other vendors to find a solution but was never presented with any. “W ...
ASTRONOMY AND ASTROPHYSICS Properties of solar pores
... visible lines of different formation heights, Thim (1993) finds 3.3 G km;1; the empirical model of Sütterlin (1991) predicts a gradient of 2-3 G km ;1. Theoretical models as well as observations show that the diameter of a pore increases with height in the atmosphere (Simon & Weiss 1970; Zirin & Wan ...
... visible lines of different formation heights, Thim (1993) finds 3.3 G km;1; the empirical model of Sütterlin (1991) predicts a gradient of 2-3 G km ;1. Theoretical models as well as observations show that the diameter of a pore increases with height in the atmosphere (Simon & Weiss 1970; Zirin & Wan ...
Evolution of Primordial Magnetic Fields from Phase
... and is equal to 0.5 pc for the QCDPT (with g⋆ = 15 and T⋆ = 0.15 GeV) and 6 × 10−4 pc for the EWPT (with g⋆ = 100 and T⋆ = 100 GeV), and the comoving primordial magnetic field correlation length ξmax ≤ λH . This inequality assumes only the expansion of the Universe without accounting for MHD turbule ...
... and is equal to 0.5 pc for the QCDPT (with g⋆ = 15 and T⋆ = 0.15 GeV) and 6 × 10−4 pc for the EWPT (with g⋆ = 100 and T⋆ = 100 GeV), and the comoving primordial magnetic field correlation length ξmax ≤ λH . This inequality assumes only the expansion of the Universe without accounting for MHD turbule ...
Current Systems in Planetary Magnetospheres and Ionospheres
... the same order of magnitude as the originally applied field of internal or solar origin. 1.2 Sources of Planetary Plasmas There are mainly three sources of plasmas in planetary environments (e.g., Blanc et al. ...
... the same order of magnitude as the originally applied field of internal or solar origin. 1.2 Sources of Planetary Plasmas There are mainly three sources of plasmas in planetary environments (e.g., Blanc et al. ...
Energetic neutral atoms around HD 209458b
... • Elastic collision with another hydrogen atom, according to the DSMC method described in the next section. All rates above are from Hodges (1994) for Earth, and average solar conditions, scaled by (1/0.045)2 to account for the larger photon fluxes at the orbital distance of HD 209458b. The stellar ...
... • Elastic collision with another hydrogen atom, according to the DSMC method described in the next section. All rates above are from Hodges (1994) for Earth, and average solar conditions, scaled by (1/0.045)2 to account for the larger photon fluxes at the orbital distance of HD 209458b. The stellar ...
Warm Up- Work silently to receive full credit
... • If the distance is multiplied by some number, Fg is divided by the SQUARE of that number • If the distance is divided by some number, Fg is multiplied by the SQUARE of that ...
... • If the distance is multiplied by some number, Fg is divided by the SQUARE of that number • If the distance is divided by some number, Fg is multiplied by the SQUARE of that ...
Document
... Distance is the total distance travelled. It is a scalar quantity. Displacement is the length measured from the starting point of a journey to the finishing point in a straight line. Its direction must be stated because it is a vector quantity. The direction can be given as left or right, up or down ...
... Distance is the total distance travelled. It is a scalar quantity. Displacement is the length measured from the starting point of a journey to the finishing point in a straight line. Its direction must be stated because it is a vector quantity. The direction can be given as left or right, up or down ...
Modelling magnetic fields in spiral galaxies
... Moss: Magnetic fields in spiral galaxies – i.e. by ~3 Gyr after time zero: technological advantages may soon push this “first field” time back very considerably in favourable cases. In general, studies of galactic magnetism have one notable advantage compared with those of solar and stellar magneti ...
... Moss: Magnetic fields in spiral galaxies – i.e. by ~3 Gyr after time zero: technological advantages may soon push this “first field” time back very considerably in favourable cases. In general, studies of galactic magnetism have one notable advantage compared with those of solar and stellar magneti ...
Chapter 3 (Lectures 7
... superficial convection zone, could release so much energy; it is also not clear how the activity could be produced in or by an accretion disk. In any case, a group centred around C. Catala, G. Wade, and E. Alecian have been carrying out a large survey to try to detect magnetic fields in these stars. ...
... superficial convection zone, could release so much energy; it is also not clear how the activity could be produced in or by an accretion disk. In any case, a group centred around C. Catala, G. Wade, and E. Alecian have been carrying out a large survey to try to detect magnetic fields in these stars. ...
Evidence for an oscillation of the magnetic axis of the white dwarf in
... phase. This is a transient phenomenon, as seen in the top panel of Fig. 1, where maxima at orbital phases of about 0.30 and 0.50 appear in the third of three faint-phase intervals, but these maxima are absent from the second interval. Traces appear frequently, in particular of the φ = 0.50 hump. On ...
... phase. This is a transient phenomenon, as seen in the top panel of Fig. 1, where maxima at orbital phases of about 0.30 and 0.50 appear in the third of three faint-phase intervals, but these maxima are absent from the second interval. Traces appear frequently, in particular of the φ = 0.50 hump. On ...
physics with photons of non-zero rest mass
... Since it is now clear that among the founding texts of Special Relativity are the two works of Henri Poincaré “Sur la dynamique de l’électron” (ref. 1 and 2), it is interesting to look for their differences with the work of Einstein (ref. 4). The ref. 2, the “Palermo Memoir” contains a mine of relat ...
... Since it is now clear that among the founding texts of Special Relativity are the two works of Henri Poincaré “Sur la dynamique de l’électron” (ref. 1 and 2), it is interesting to look for their differences with the work of Einstein (ref. 4). The ref. 2, the “Palermo Memoir” contains a mine of relat ...
PDF only
... quantum number = −1 and for both even and odd z -parity as well as singlet and triplet spin symmetry. Additionally they presented energies for electromagnetic transitions within the = −1 subspace and between the = −1 subspace and the = 0 subspace. Also, W. Becken and P. Schmelcher inv ...
... quantum number = −1 and for both even and odd z -parity as well as singlet and triplet spin symmetry. Additionally they presented energies for electromagnetic transitions within the = −1 subspace and between the = −1 subspace and the = 0 subspace. Also, W. Becken and P. Schmelcher inv ...
2 Solar magnetic fields. - High Altitude Observatory
... in the Sun, from the point of view of Newton, and Maxwell. Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots exist in spite of the fact that 100% of the solar luminosity is carried by t ...
... in the Sun, from the point of view of Newton, and Maxwell. Right off the bat, I draw attention to a curious but central issue, captured in one of the best and exquisite images yet obtained of a sunspot (Figure 2.1). Sunspots exist in spite of the fact that 100% of the solar luminosity is carried by t ...
PDF: 154K
... the kinematic viscosity and Z is the magnetic diffusion due to the electrical conductivity of the plasma. In this case m ¼ 2, and the parameter sB o0 even in a turbulent convection. This implies that for small hydrodynamic and magnetic Reynolds numbers there is no dynamo action due to the shear-curr ...
... the kinematic viscosity and Z is the magnetic diffusion due to the electrical conductivity of the plasma. In this case m ¼ 2, and the parameter sB o0 even in a turbulent convection. This implies that for small hydrodynamic and magnetic Reynolds numbers there is no dynamo action due to the shear-curr ...
David L. Meier, , 84 (2001); DOI: 10.1126/science.291.5501.84
... The flow of a magnetized plasma is most generally described by kinetic theory, general relativity, and Maxwell’s equations for the ...
... The flow of a magnetized plasma is most generally described by kinetic theory, general relativity, and Maxwell’s equations for the ...
SCHEME OF WORK – PHYSICS 960, UPPER SIX 2013 Term2
... a. define magnetic flux = BAcos b. state and use Faraday’s law and Lenz’s law c. derive and use the equation for induced emf in linear conductors, discs, and plane coils d. explain the phenomenon of self-inductance and define self-inductance e. use the formulae E L ...
... a. define magnetic flux = BAcos b. state and use Faraday’s law and Lenz’s law c. derive and use the equation for induced emf in linear conductors, discs, and plane coils d. explain the phenomenon of self-inductance and define self-inductance e. use the formulae E L ...
New energy and helicity bounds for knotted and braided magnetic
... writhe and twist contributions, HWr and HTw. In particular, we have HTw ¼ H HWr. Hence, an estimate of HTw can be obtained by direct measurements of total helicity, using (5) and (13) by diagram extraction from visiometric analysis based on observational data and imaging analysis. These methods ha ...
... writhe and twist contributions, HWr and HTw. In particular, we have HTw ¼ H HWr. Hence, an estimate of HTw can be obtained by direct measurements of total helicity, using (5) and (13) by diagram extraction from visiometric analysis based on observational data and imaging analysis. These methods ha ...
(PDF, Unknown) - Natural Philosophy Alliance
... Maxwell’s equations. [4 p. 555 or 5 p. 560] The force of gravity is normally measured between neutral charge bodies. Since the time of Newton, scientists have learned that the neutral atom consists of electrons, protons, and neutrons. Even elementary charged particles such as the neutron and proton ...
... Maxwell’s equations. [4 p. 555 or 5 p. 560] The force of gravity is normally measured between neutral charge bodies. Since the time of Newton, scientists have learned that the neutral atom consists of electrons, protons, and neutrons. Even elementary charged particles such as the neutron and proton ...
PPT
... in rotational frame (including potential from centrifugal force). • The basic MHD equations are integrated into six conservation equations eq (8.11) – (8.16). • These six parameter, f, F, W, rA2, K, E are integral constant. • The unknown variables are also six, r, vr, Br, vf, Bf, p • Hence, if these ...
... in rotational frame (including potential from centrifugal force). • The basic MHD equations are integrated into six conservation equations eq (8.11) – (8.16). • These six parameter, f, F, W, rA2, K, E are integral constant. • The unknown variables are also six, r, vr, Br, vf, Bf, p • Hence, if these ...
Solutions
... (3.4) [3 points] We can derive an equation for the distance ∆L(t) travelled by the top of the slinky at a time t after ‘launch’, up to the moment when it reaches the bottom of the slinky, by combining the equation for the motion of the center of mass with the observation that a compression wave trav ...
... (3.4) [3 points] We can derive an equation for the distance ∆L(t) travelled by the top of the slinky at a time t after ‘launch’, up to the moment when it reaches the bottom of the slinky, by combining the equation for the motion of the center of mass with the observation that a compression wave trav ...
A self-consistent model of isolated neutron stars: the case of the X
... in Tomimura & Eriguchi (2005) where Eq. (1) is generalized by considering µ = µ(x) as a general function of x = r sin θAφ , where Aφ is the φ component of the vector potential. It is not the purpose of this paper to review all previous calculations about the structure of neutron stars with magnetic ...
... in Tomimura & Eriguchi (2005) where Eq. (1) is generalized by considering µ = µ(x) as a general function of x = r sin θAφ , where Aφ is the φ component of the vector potential. It is not the purpose of this paper to review all previous calculations about the structure of neutron stars with magnetic ...
Document
... Sun and other cosmic objects in the sixties of the last century. As was known or at least considered as very probable at that time, magnetic fields as well as the motions inside the electrically conducting interiors of these objects show rather complex geometrical structures and time behaviors. In a ...
... Sun and other cosmic objects in the sixties of the last century. As was known or at least considered as very probable at that time, magnetic fields as well as the motions inside the electrically conducting interiors of these objects show rather complex geometrical structures and time behaviors. In a ...
Investigation of mass flows in the transition region and corona in a
... by Peter et al. (2006), see their Fig. 5. In a static 1D empirical model based on an emission measure inversion, Mariska (1992) found a maximum temperature gradient of the order of 10 K/m (his Table 6.1). Flows present in our 3D model are assumed to smooth out steep temperature gradients, resulting ...
... by Peter et al. (2006), see their Fig. 5. In a static 1D empirical model based on an emission measure inversion, Mariska (1992) found a maximum temperature gradient of the order of 10 K/m (his Table 6.1). Flows present in our 3D model are assumed to smooth out steep temperature gradients, resulting ...
lecture 3 `Rapidly rotating convection, dynamos, and scaling laws`
... We start by finding the critical Rayleigh at which convection first sets in. Since velocities initially are small, there will be no dynamo and so no magnetic field. Rotation has a strong influence on the onset of convection. The key parameter is the Ekman number, Ω/νd2, d being the gap-width as usua ...
... We start by finding the critical Rayleigh at which convection first sets in. Since velocities initially are small, there will be no dynamo and so no magnetic field. Rotation has a strong influence on the onset of convection. The key parameter is the Ekman number, Ω/νd2, d being the gap-width as usua ...
Decay and Amplification of Magnetic Fields
... of the mechanism: first, this works only if the fieldlines are frozen into the fluid, i.e., in the high-Rm regime. Second, mass conservation plays an essential role here; the stretching motion along the tube axis must be accompanied by a compressing fluid motion perpendicular to the axis if mass con ...
... of the mechanism: first, this works only if the fieldlines are frozen into the fluid, i.e., in the high-Rm regime. Second, mass conservation plays an essential role here; the stretching motion along the tube axis must be accompanied by a compressing fluid motion perpendicular to the axis if mass con ...
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.