Chapter 1 Introduction: Matter and Measurement
... substances from liquids and solutions. Mixture: K2Cr2O7(s) +NaNO3(s) ...
... substances from liquids and solutions. Mixture: K2Cr2O7(s) +NaNO3(s) ...
- Achieve the Core
... region where the Voyagers are now "the heliosheath." It is essentially the border crossing between the Solar System and the rest of the Milky Way. Lots of things try to get across— interstellar clouds, knots of galactic magnetism, cosmic rays and so on. Will these intruders encounter a riot of bubbl ...
... region where the Voyagers are now "the heliosheath." It is essentially the border crossing between the Solar System and the rest of the Milky Way. Lots of things try to get across— interstellar clouds, knots of galactic magnetism, cosmic rays and so on. Will these intruders encounter a riot of bubbl ...
Attitude Determination and Orbital Estimation Using Earth Position
... of both the orbital position and the orientation of a body fixed coordinate system with respect to an orbital reference coordinate system. One possible way to determine the latter is by utilizing an EKF to estimate the attitude quaternion and the axis rates [6], [8], [9]. This requires the estimatio ...
... of both the orbital position and the orientation of a body fixed coordinate system with respect to an orbital reference coordinate system. One possible way to determine the latter is by utilizing an EKF to estimate the attitude quaternion and the axis rates [6], [8], [9]. This requires the estimatio ...
Synchrotron and inverse-Compton emission from
... a result of the acceleration process, then at some later time t > 0 we expect N(E) to have a characteristic form depending on t. Since for synchrotron radiation the characteristic time-scale for energy losses goes as 1/E, N(E) at t > 0 will always be characterized by depletion of the highest energy ...
... a result of the acceleration process, then at some later time t > 0 we expect N(E) to have a characteristic form depending on t. Since for synchrotron radiation the characteristic time-scale for energy losses goes as 1/E, N(E) at t > 0 will always be characterized by depletion of the highest energy ...
Radiato-Magneto-Thermal Winds from an Accretion Disk
... magnetic field is detected and believed to be a main force. In recent years, gamma-ray bursts (GRBs) are recognized to be some type of astrophysical jets that occurs in supernova explosions. In this case the jets are highly relativistic with a Lorentz factor of ∼ 100. It is believed, in any case, th ...
... magnetic field is detected and believed to be a main force. In recent years, gamma-ray bursts (GRBs) are recognized to be some type of astrophysical jets that occurs in supernova explosions. In this case the jets are highly relativistic with a Lorentz factor of ∼ 100. It is believed, in any case, th ...
Overview spherical accretion
... http://www.astro.virginia.edu/class/whittle/astr553/Topic08/Lecture_8.html ...
... http://www.astro.virginia.edu/class/whittle/astr553/Topic08/Lecture_8.html ...
Jets in Active Galactic Nuclei Alan P. Marscher
... roughly self-similar over several orders of magnitude in distance from the black hole. This is easiest to understand if the jets are mainly fluid phenomena so that they are governed by the laws of gas dynamics and magnetohydrodynamics. Images of jets contain a bright, nearly unresolved “core” at the ...
... roughly self-similar over several orders of magnitude in distance from the black hole. This is easiest to understand if the jets are mainly fluid phenomena so that they are governed by the laws of gas dynamics and magnetohydrodynamics. Images of jets contain a bright, nearly unresolved “core” at the ...
Perlite of composition SiO2 73.6%, A1203 12.4%, Fe203 1.25
... In order to study the behaviour of minerals in a magnetic field of different strength, tests were made with a laboratory Frantz separator. Table 6 shows that better separation is achieved with smaller particles but the differences are of little practical significance. However, with the-70+100 mesh f ...
... In order to study the behaviour of minerals in a magnetic field of different strength, tests were made with a laboratory Frantz separator. Table 6 shows that better separation is achieved with smaller particles but the differences are of little practical significance. However, with the-70+100 mesh f ...
Pore Scale Modeling of Rock Properties and Comparison to Laboratory Measurements
... binarized to clearly distinguish the pore space and rock matrix by ANU. The BS500 core sample is digitized into a 18403 voxel tomogram with 2.8 micron resolution. This sample contains some clay; the mineralogy of BS500 is listed in Table 1. The volume fraction of clay was determined by the X-ray att ...
... binarized to clearly distinguish the pore space and rock matrix by ANU. The BS500 core sample is digitized into a 18403 voxel tomogram with 2.8 micron resolution. This sample contains some clay; the mineralogy of BS500 is listed in Table 1. The volume fraction of clay was determined by the X-ray att ...
Optimization of SMES Coil by Using Virial Theorem
... Next, we calculate the stress distribution of the helical coil with A = 2 using (35)-(37). The results for some kinds of coils are shown in Fig. 4. To compare them in the condition of a fixed magnetic energy, they are normalized by the magnetic energy UM . The poloidal angle θ is defined so as to take ...
... Next, we calculate the stress distribution of the helical coil with A = 2 using (35)-(37). The results for some kinds of coils are shown in Fig. 4. To compare them in the condition of a fixed magnetic energy, they are normalized by the magnetic energy UM . The poloidal angle θ is defined so as to take ...
Radiative Processes in Astrophysics. Radio Polarization
... oscillation period is then given by 2Θ = 2π∆v /c. For a given frequency the total rotation angle (θ) is proportional to the distance travelled by the wave (D) divided by λ. ...
... oscillation period is then given by 2Θ = 2π∆v /c. For a given frequency the total rotation angle (θ) is proportional to the distance travelled by the wave (D) divided by λ. ...
Theory of pulsar winds and nebulae - Max-Planck
... Electric and magnetic fields dominate the dynamics in the near zone inside the light cylinder. However, this is also true in at least part of the “far zone”, that lies well outside the light cylinder — a region that is not conventionally thought of as the pulsar magnetosphere. Here, we follow conven ...
... Electric and magnetic fields dominate the dynamics in the near zone inside the light cylinder. However, this is also true in at least part of the “far zone”, that lies well outside the light cylinder — a region that is not conventionally thought of as the pulsar magnetosphere. Here, we follow conven ...
Accretion to Stars with Non
... First, for reference we show the results of simulations of accretion to a star with a pure dipole field with µ = 0.5 inclined relative to the spin axis at an angle Θ = 30◦ . Figure 2a (left panel) shows the density distribution in the x − z plane (this is also the µ − Ω plane). One can see that most ...
... First, for reference we show the results of simulations of accretion to a star with a pure dipole field with µ = 0.5 inclined relative to the spin axis at an angle Θ = 30◦ . Figure 2a (left panel) shows the density distribution in the x − z plane (this is also the µ − Ω plane). One can see that most ...
Magnetic Doppler imaging of the roAp star HD 24712⋆
... stars with light (Wolff & Morrison 1973), spectrum and magnetic variations that was discovered to pulsate by Kurtz (1982). Matthews et al. (1988) found radial velocity variations with an amplitude of 0.4±0.05 km s−1 and the main photometric period of 6.14 min. During an observing campaign with the W ...
... stars with light (Wolff & Morrison 1973), spectrum and magnetic variations that was discovered to pulsate by Kurtz (1982). Matthews et al. (1988) found radial velocity variations with an amplitude of 0.4±0.05 km s−1 and the main photometric period of 6.14 min. During an observing campaign with the W ...
Conservation of momentum:
... voxels need not even be neighbouring voxels but could be located far away from the voxel to be updated. If a data-parallel approach is chosen, this fact may cause race conditions as several threads may try to access a given voxel at the same time. Restricting the user defined velocities/forces would ...
... voxels need not even be neighbouring voxels but could be located far away from the voxel to be updated. If a data-parallel approach is chosen, this fact may cause race conditions as several threads may try to access a given voxel at the same time. Restricting the user defined velocities/forces would ...
Solar flare mechanism based on magnetic arcade reconnection and island... C. Z. Cheng and G. S. Choe
... although the conjugate footpoint distance may not be defined and diverge in the separatrix connected to the X-line (Choe and Lee, 1996), the toroidal flux in a finite flux volume does not diverge and the magnetic shear in the underlying arcade is always decreased after reconnection. Thus, the magnet ...
... although the conjugate footpoint distance may not be defined and diverge in the separatrix connected to the X-line (Choe and Lee, 1996), the toroidal flux in a finite flux volume does not diverge and the magnetic shear in the underlying arcade is always decreased after reconnection. Thus, the magnet ...
the fragmentation of magnetized, massive star-forming
... We present a set of three-dimensional, radiation-magnetohydrodynamic calculations of the gravitational collapse of massive (300 M ), star-forming molecular cloud cores. We show that the combined effects of magnetic fields and radiative feedback strongly suppress core fragmentation, leading to the p ...
... We present a set of three-dimensional, radiation-magnetohydrodynamic calculations of the gravitational collapse of massive (300 M ), star-forming molecular cloud cores. We show that the combined effects of magnetic fields and radiative feedback strongly suppress core fragmentation, leading to the p ...
Precipitation Behavior and Magnetic Properties of Cu-Fe
... on annealing temperature. Figure 2 shows the mean sizes of precipitates versus time for different annealing temperatures in the Cu-Fe-Co alloy. The growth rate increases with annealing temperature, consistent with previous observations in CuCo and Cu-Fe alloys [7–9, 13–15]. The growth rates of preci ...
... on annealing temperature. Figure 2 shows the mean sizes of precipitates versus time for different annealing temperatures in the Cu-Fe-Co alloy. The growth rate increases with annealing temperature, consistent with previous observations in CuCo and Cu-Fe alloys [7–9, 13–15]. The growth rates of preci ...
Our Dynamic Universe - St Andrew`s Academy
... Calculate the potential energy of the cycle and rider at the top of the slope Calculate the kinetic energy of the cycle and rider at the top of the slope. Calculate the kinetic energy of the cycle and rider at the bottom of the slope. Describe the energy changes during the course of the journey down ...
... Calculate the potential energy of the cycle and rider at the top of the slope Calculate the kinetic energy of the cycle and rider at the top of the slope. Calculate the kinetic energy of the cycle and rider at the bottom of the slope. Describe the energy changes during the course of the journey down ...
Magnetic Fields in Stars
... we are in the process of learning more about how they are distributed over stellar surfaces, and we understand some of the ways in which these fields reflect—and sometimes influence—the evolution of the stars which possess them. The first stellar magnetic fields were detected in sunspots (see SUNSPO ...
... we are in the process of learning more about how they are distributed over stellar surfaces, and we understand some of the ways in which these fields reflect—and sometimes influence—the evolution of the stars which possess them. The first stellar magnetic fields were detected in sunspots (see SUNSPO ...
2003 Venkatakrishnan and Ravindra Relation between CME speed
... (upper limit). The potential magnetic field was determined from the observed line-of-sight field using the Fourier method [Alissandrakis, 1981]. Using this computed potential field, the potential magnetic energy of the active region was determined by the application of the virial theorem to the phot ...
... (upper limit). The potential magnetic field was determined from the observed line-of-sight field using the Fourier method [Alissandrakis, 1981]. Using this computed potential field, the potential magnetic energy of the active region was determined by the application of the virial theorem to the phot ...
constraints on primordial magnetic fields with cmb anisotropies
... cosmological scales the charged component of the cascade interacts with the magnetic fields reducing the flux of secondary photons in the GeV range from the blazar (Dolag et al. 2000). FERMI observations of the Blazar 1ES 0229+200 presents a lack of flux of GeV photons with respect to the prediction ...
... cosmological scales the charged component of the cascade interacts with the magnetic fields reducing the flux of secondary photons in the GeV range from the blazar (Dolag et al. 2000). FERMI observations of the Blazar 1ES 0229+200 presents a lack of flux of GeV photons with respect to the prediction ...
The origin of magnetism on the upper main sequence
... stars such as HD 191612 (B ≈ 1500 G, spectral-type O6; Donati et al. 2002). Petit et al. (2008) have argued that 25 per cent of the massive stars (M > 20 M ) in the Orion Nebula have extremely high magnetic fields (B 1000 G), but it has also been noted that this cluster exhibits a highly abnormal ...
... stars such as HD 191612 (B ≈ 1500 G, spectral-type O6; Donati et al. 2002). Petit et al. (2008) have argued that 25 per cent of the massive stars (M > 20 M ) in the Orion Nebula have extremely high magnetic fields (B 1000 G), but it has also been noted that this cluster exhibits a highly abnormal ...
contributed talk in splinter session
... the location and extent of the accretion funnels (inferred from optical and UV observations) is as much of a puzzle as the mass accretion rate that they carry. Mass and angular momentum are not only gained by the star in the process of accretion, but also lost in either jets or winds. Linking all th ...
... the location and extent of the accretion funnels (inferred from optical and UV observations) is as much of a puzzle as the mass accretion rate that they carry. Mass and angular momentum are not only gained by the star in the process of accretion, but also lost in either jets or winds. Linking all th ...
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.