Magnetic field generation in weak-line T Tauri stars
... of avoiding the singularity at the origin of the coordinate system, it does not allow detailed radial profiles of density, magnetic diffusivity and other relevant parameters. We use averaged values for these quantities as well as for their gradients where necessary. Moreover, it is not very convenie ...
... of avoiding the singularity at the origin of the coordinate system, it does not allow detailed radial profiles of density, magnetic diffusivity and other relevant parameters. We use averaged values for these quantities as well as for their gradients where necessary. Moreover, it is not very convenie ...
COSPAR WORKSHOP ON CAPACITY DEVELOPMENT
... lines that are closer to the Earth than those of a dipole The existence of stretched field line requires tangential stress, or a force parallel to the boundary In ordinary fluid flow tangential stress (or drag as sometimes called) is caused by the viscous interaction Particles are scattered from the ...
... lines that are closer to the Earth than those of a dipole The existence of stretched field line requires tangential stress, or a force parallel to the boundary In ordinary fluid flow tangential stress (or drag as sometimes called) is caused by the viscous interaction Particles are scattered from the ...
The centrifugal term is nearly equal to zero.
... The driving force of the CD kink mode is an asymmetrically distribution of hoop-stress (the magnetic tension force). This is caused by a sudden decrease of jet rotation and a concentration of the poloidal magnetic flux toward the central axis (which is related to a reverse slow-mode MHD ...
... The driving force of the CD kink mode is an asymmetrically distribution of hoop-stress (the magnetic tension force). This is caused by a sudden decrease of jet rotation and a concentration of the poloidal magnetic flux toward the central axis (which is related to a reverse slow-mode MHD ...
Spontaneous radiative alignment of dipole moments of atoms
... The overwhelming majority of papers deal with that reaction-force component which performs work and determines thereby the radiation power. Yet the reaction-force component perpendicular to the source velocity, while performing no work, does induce rotation. It will be shown here that the reaction-f ...
... The overwhelming majority of papers deal with that reaction-force component which performs work and determines thereby the radiation power. Yet the reaction-force component perpendicular to the source velocity, while performing no work, does induce rotation. It will be shown here that the reaction-f ...
Evolution of filamentary molecular clouds in the presence of
... infall velocity; with increasing distance from the axis the infall velocity increases, which is shown in Figure 4, assuming γ = 1.66 and we change the initial value of the toroidal component of the magnetic field. Also, its negative sign shows the direction of velocity with respect to the axis, i.e. ...
... infall velocity; with increasing distance from the axis the infall velocity increases, which is shown in Figure 4, assuming γ = 1.66 and we change the initial value of the toroidal component of the magnetic field. Also, its negative sign shows the direction of velocity with respect to the axis, i.e. ...
Angular momentum evolution
... Observational constraints • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and ...
... Observational constraints • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and ...
Stockholm University
... force-free magnetic field such that the field can deviate from a force-free state locally in regions where the field cannot easily be made force-free. This could be done by solving the induction equation with an additional ambipolar diffusion term, which implies the presence of an effective velocity c ...
... force-free magnetic field such that the field can deviate from a force-free state locally in regions where the field cannot easily be made force-free. This could be done by solving the induction equation with an additional ambipolar diffusion term, which implies the presence of an effective velocity c ...
SolarDermatology
... Spicules: jets of hot material seen in the chromosphere, flowing 20 km/sec from the ...
... Spicules: jets of hot material seen in the chromosphere, flowing 20 km/sec from the ...
PPT
... How much the theoretical 2-D reconnection picture is valid in actual experiments, How does guide field affect reconnection rate What kinds of non-MHD effects would dominate in the reconnection layer, How the magnetic energy is converted to plasma flows and thermal energy, What is a guiding principle ...
... How much the theoretical 2-D reconnection picture is valid in actual experiments, How does guide field affect reconnection rate What kinds of non-MHD effects would dominate in the reconnection layer, How the magnetic energy is converted to plasma flows and thermal energy, What is a guiding principle ...
Hubble - schoolphysics
... Hubble's constant and the expansion of the Universe. In 1925 the American astronomer Edwin Hubble (1889-1953) proposed a very simple relationship between the distance of a galaxy and its velocity of recession or approach (v). The Hubble formula provides a very powerful way of determining not only di ...
... Hubble's constant and the expansion of the Universe. In 1925 the American astronomer Edwin Hubble (1889-1953) proposed a very simple relationship between the distance of a galaxy and its velocity of recession or approach (v). The Hubble formula provides a very powerful way of determining not only di ...
Self-Similar Energy Decay in Magnetohydrodynamic Turbulence
... initial ratio of kinetic to magnetic energy may be relevant as well as it is known to lead to different regimes [27]. These issues require a large parametric study and will be tackled in the future [11]. The present computations, at least in 2D, seem sufficient to rule out the 21 law predicted in [6 ...
... initial ratio of kinetic to magnetic energy may be relevant as well as it is known to lead to different regimes [27]. These issues require a large parametric study and will be tackled in the future [11]. The present computations, at least in 2D, seem sufficient to rule out the 21 law predicted in [6 ...
Evolution of the multipolar magnetic field in isolated neutron stars
... numerically using the Crank±Nicholson method of differencing. We have modified the numerical code developed by Konar (1997) and used by Konar & Bhattacharya (1997) to compute the evolution of multipolar magnetic fields satisfying the appropriate boundary conditions given by equation (3). ...
... numerically using the Crank±Nicholson method of differencing. We have modified the numerical code developed by Konar (1997) and used by Konar & Bhattacharya (1997) to compute the evolution of multipolar magnetic fields satisfying the appropriate boundary conditions given by equation (3). ...
poster
... Most models of jet launching rely on a magnetic field in either the central source, the accretion disk or both. However, the well-studied nearby young Herbig Ae star HD 163296 has a measured weak stellar magnetic field (main-sequence A stars do not have magnetic fields at all), and even indications ...
... Most models of jet launching rely on a magnetic field in either the central source, the accretion disk or both. However, the well-studied nearby young Herbig Ae star HD 163296 has a measured weak stellar magnetic field (main-sequence A stars do not have magnetic fields at all), and even indications ...
Magnetic reconnection
... Original idea is converting magnetic field energy to plasma kinetic energy. Recently plasma heating, particle acceleration and wave excitation are also well discussed in the category of magnetic reconnection. These energy conversion rates are heavily depending on the plasma conditions. In that sense ...
... Original idea is converting magnetic field energy to plasma kinetic energy. Recently plasma heating, particle acceleration and wave excitation are also well discussed in the category of magnetic reconnection. These energy conversion rates are heavily depending on the plasma conditions. In that sense ...
Improved period of a slowly rotating cool magnetic CP star HD 188041
... value 34 d, which is the other synodic month alias to the long period. The same elements were used later in photometric studies by Jones & Wolff (1973), Musielok et al.(1980), Musielok (1986) and Musielok & Madej (1988). Panov & Schöneich (1975) and Schöneich (1975) came to the period P = 224.93 d ...
... value 34 d, which is the other synodic month alias to the long period. The same elements were used later in photometric studies by Jones & Wolff (1973), Musielok et al.(1980), Musielok (1986) and Musielok & Madej (1988). Panov & Schöneich (1975) and Schöneich (1975) came to the period P = 224.93 d ...
Discovery Of A Magnetic Field In The O9 Sub-Giant Star HD
... 11 high-resolution (R ∼ 65 000), broad-band (370–1050 nm) circular polarization (Stokes V) spectra of HD 57682 were obtained with the ESPaDOnS spectropolarimeter, mounted on the 3.6-m CFHT, as part of the Survey Component of the MiMeS Large Program. The spectra were acquired and reduced in a manner ...
... 11 high-resolution (R ∼ 65 000), broad-band (370–1050 nm) circular polarization (Stokes V) spectra of HD 57682 were obtained with the ESPaDOnS spectropolarimeter, mounted on the 3.6-m CFHT, as part of the Survey Component of the MiMeS Large Program. The spectra were acquired and reduced in a manner ...
ISP 205 Review Questions, Week 13
... km/sec per million light years, how far away is the galaxy from us? Hint... Solve for the distance d in the equation v = H0d , where v is the velocity you found in the previous question. ...
... km/sec per million light years, how far away is the galaxy from us? Hint... Solve for the distance d in the equation v = H0d , where v is the velocity you found in the previous question. ...
Lecture 4: Molecular Clouds (1)
... The original gas is presumably atomic. Molecular clouds then form inside the condensing medium through their self-shielding from UV radiation. The observed drop in the H2 surface density between the arms implies that a typical GMC cannot survive as long as the interarm travel time of the Galactic ga ...
... The original gas is presumably atomic. Molecular clouds then form inside the condensing medium through their self-shielding from UV radiation. The observed drop in the H2 surface density between the arms implies that a typical GMC cannot survive as long as the interarm travel time of the Galactic ga ...
Lecture 17 Fluid Dynamics: handouts
... • Laplace transform of response to general time-dependent source z(s) ...
... • Laplace transform of response to general time-dependent source z(s) ...
Document
... These graphs allow us to see where a positive slope in velocity space develops in relation to the required minimum velocity for Type III radio emission and hence at what distance along the field line a wave resulting in this sort of emission is created. Thus we can postulate where Type III emission ...
... These graphs allow us to see where a positive slope in velocity space develops in relation to the required minimum velocity for Type III radio emission and hence at what distance along the field line a wave resulting in this sort of emission is created. Thus we can postulate where Type III emission ...
A regular period for Saturn’s magnetic field that G. Giampieri
... peak in the spectrum. A simple inspection of the field components in the time domain reveals that the phase of the periodic signal varies by less than 0.58 from orbit to orbit. Can this periodic signal be a direct signature of Saturn’s rotation rate? If we accept that the radio emission period is re ...
... peak in the spectrum. A simple inspection of the field components in the time domain reveals that the phase of the periodic signal varies by less than 0.58 from orbit to orbit. Can this periodic signal be a direct signature of Saturn’s rotation rate? If we accept that the radio emission period is re ...
Key Points on Chapter 15: Fluid Mechanics • Pressure is force per
... Viscosity is often used to characterize the ease of flow. Honey is very viscous. Highly viscous fluids resist flow and do not flow easily, e.g., ketchup. There is a sort of internal friction as parts of the fluid try to flow or move past other parts. Fluids can be very complicated. To make things si ...
... Viscosity is often used to characterize the ease of flow. Honey is very viscous. Highly viscous fluids resist flow and do not flow easily, e.g., ketchup. There is a sort of internal friction as parts of the fluid try to flow or move past other parts. Fluids can be very complicated. To make things si ...
Figure 1 - Research
... surface distance less flux is confined within magnetic loops and there is more open flux going into the heliosphere. • There is a cyclic variation: n is highest soon after sunspot maxima and smallest during sunspot minima. This is partly due to the solar cycle variation of the heliospheric magnetic ...
... surface distance less flux is confined within magnetic loops and there is more open flux going into the heliosphere. • There is a cyclic variation: n is highest soon after sunspot maxima and smallest during sunspot minima. This is partly due to the solar cycle variation of the heliospheric magnetic ...
Modelling ripple transport in two dimensions
... Here, as the particle approaches the field minimum, δB→B0. ...
... Here, as the particle approaches the field minimum, δB→B0. ...
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.