相关论文
2021 - 2021 XXXIVth General Assembly and Scientific Symposium of the International Union of Radio Science (URSI GASS)
Modeling Electron Scattering and Acceleration by Whistler Mode Chorus Waves in Jupiter's Magnetosphere: Effects of Magnetic Field Model, Total Electron Density, and Electron Injections

We evaluate the energetic electron scattering and acceleration due to whistler mode chorus waves using realistic magnetic field and density models in Jupiter's magnetosphere, and study the potential effects of electron injections. The bounce-averaged diffusion coefficients are calculated using the total electron density from the diffusive equilibrium model and the magnetic field strength from the VIP4 internal magnetic field and CAN current sheet model. The electron phase space density evolution due to chorus wave is simulated at $M=10$. The typical chorus waves could cause fast pitch angle scattering loss of electrons from tens to several hundred keV, and gradual acceleration of relativistic electrons at several MeV. The latitudinally varying density and $\text{VIP}4+\text{CAN}$ magnetic field model leads to faster pitch angle scattering and acceleration of electrons at energies above 100 keV than the constant density and dipolar magnetic field model. The simulation is compared to the electron dynamics during an electron injection event observed by Juno on 29 October, 2018. The electron flux is enhanced at low energies during the injection event, and the Fokker Planck simulation indicates an enhanced electron acceleration due to chorus waves subsequent to the injections. The modeling indicates an electron flux increase by nearly 1 order of magnitude within 1 day, suggesting the potentially important role of chorus waves in forming Jupiter's radiation belts after injections.

2020 - Saratov Fall Meeting
Numerical simulation of magnetic nanoparticles in the blood stream

The paper presents theoretical study of magnetic nanoparticles through blood stream in the presence of magnetic field. This field created from a permanent magnet localized outside the tube and perpendicular to flow direction. The capillary tube has a rectangular cross-section with a length l and a width w. Behavior of such particles in a permanent magnet depends on the intensity of magnetic field. Therefore, under a uniform magnetic field, particles aligned along the lines of magnetic field strength. However, for a non-uniform magnetic field, the particles move towards the area where the magnetic field strength is higher and, thus, concentration of particles in this region becomes bigger. The capture and accumulation of particles depend on many parameters, such as magnetic field strength and distance between the surface of magnet and the capillary wall. The motion equation describing magnetic nanoparticles / blood flow and governed by a combination of the magnetic equation for the permanent magnet and the Navier-Stokes equation for fluid (blood) was solved numerically using the COMSOL Multiphysics® Modeling Software.

2007 - Key Engineering Materials
Controllability of a Magnetorheological Fluid Squeeze Film Damper under Sinusoidal Magnetic Field

The controllability of a magnetorheological(MR) fluid squeeze film damper under a sinusoidal magnetic field was experimentally studied on a flexible rotor. It is shown that the frequency of the excitation magnetic field has a great effect on the controllability of the MR fluid damper. As the magnetic field frequency increases, the controllability of the MR fluid damper significantly reduces. There is a maximum frequency of the magnetic field for a given magnetic field strength or a minimum strength of the magnetic field for a given magnetic field frequency to make the dynamic behavior of the MR damper be controllable. When the magnetic field frequency is over the maximum one or the magnetic field strength is less than the minimum one, the controllability of the MR fluid damper almost completely disappears and the dynamic behavior of the MR fluid damper with the sinusoidal magnetic field is the same as that without the magnetic field.

2016 - Nuclear Fusion
Improvement of neutral beam injection heating efficiency with magnetic field well structures in a tokamak with a low magnetic field

Magnetic well structures are introduced as an effective means to reduce the prompt loss of fast ions, the so-called first orbit loss from neutral beam injection (NBI), which is beneficial to tokamaks with a low magnetic field strength such as small spherical torus devices. It is found by single-particle analysis that this additional field structure can modify the gradient of the magnetic field to reduce the shift of the guiding center trajectory of the fast ion. This result is verified by a numerical calculation of following the fast ion's trajectory. We apply this concept to the Versatile Experiment Spherical Torus [1], where NBI is under design for the purpose of achieving high-performance plasma, to evaluate the effect of the magnetic well structure on NBI efficiency. A 1D NBI analysis code and the NUBEAM code are employed for detailed NBI calculations. The simulation results show that the orbit loss can be reduced by 70%–80%, thereby improving the beam efficiency twofold compared with the reference case without the well structure. The well-shaped magnetic field structure in the low-field side can significantly decrease orbit loss by broadening the non-orbit loss region and widening the range of the velocity direction, thus improving the heating efficiency. It is found that this magnetic well can also improve orbit loss during the slowing down process.

2003
Effects of Magnetic Field and Prior Austenite Grain Size on the Structure Formed by Reverse Transformation from Lath Martensite to Austenite in an Fe-0.4C Alloy

Effects of magnetic field strength and prior austenite grain size on the microstructure formed by the reverse transformation from lath martensite to austenite have been investigated in Fe-0.4C alloy. The degree of elongation of reverse-transformed austenite increases with increasing applied magnetic field, which is a similar result with that for austenite to ferrite transformation. However, well-elongated austenite is formed not only in small prior austenite grains but also in relatively large prior austenite grains, which is different from the case of austenite to ferrite transformation.

1997 - Corrosion
Detection of Hidden Corrosion of Aircraft Aluminum Alloys by Magnetometry Using a Superconducting Quantum Interference Device

Abstract The distribution and magnitude of the magnetic field resulting from hidden corrosion of Al 2024-T3 (UNS A92024) alloy plates in solutions containing different concentrations of chloride (Cl−) ion were measured using a superconducting quantum interference device (SQUID) magnetometer, with no electrical or mechanical connections intruding on the sample. The magnetic field strength resulting from hidden corrosion occurring on the bottom surface of a 3-mm (0.118-in.) Al 2024-T3 plate in 3.5% (35,000 ppm) sodium chloride (NaCl) solution was measured as a function of distance between the SQUID pickup coils and the top surface of the sample. Results showed magnetic field strength decreased with increasing distance from the top of the sample, approaching the background value at a distance of 13 mm (0.512 in.). When the SQUID pickup coils were located 2 mm (0.079 in.) above the top surface of a sample consisting of a stack of aluminum plates, it was possible to detect hidden corrosion on the bottom surfac...

1979 - The Review of scientific instruments
High-resolution magnetic field measurement system for recording heads and disks.

A high-resolution system for measuring the magnetic fields near recording heads and disks has been built. The perpendicular field components close to the head and disk surfaces are measured with an InSb Hall probe which is moved point-by-point under computer control. The computer also records the magnetic field strength as a function of position in a plane parallel to the head or disk surface. The active area of the probe is 2x2 microm and a roughly 1-microm separation between the probe and the surfaces being measured can be obtained. Measurements of the fields near transitions on a particulate disk and near the gap in in a ferrite recording head are presented and compared with calculated field distributions.

1995 - Ndt & E International
Magnetic leakage field due to sub-surface defects in ferromagnetic specimens

Abstract This paper describes analytical expressions for the magnetic leakage field of two types of internal defects: two dimensional rectangular and elliptical defects as functions of the applied magnetic field strength, the defect size and the distance below the surface. In this study, the magnetic image effects from the spatial boundary and the defect boundary are taken into consideration. That is, the leakage field of rectangular-like defects or elliptically shaped defects ‘below the surface’ are derived by using the modified dipole model and image theory. The profiles and strengths of leakage fields calculated from the proposed analytical forms are presented under various conditions and compared with experimentally measured ones.

2000 - Physical Chemistry Chemical Physics
Steric proficiency of polar 2Σ molecules in congruent electric and magnetic fields

We examine the eigenenergies, spatial orientation, and alignment of polar 2Σ molecules subject to congruent static electric and magnetic fields. In the presence of a magnetic field only, certain pairs of Zeeman states with opposite parity intersect. Introducing a congruent electric field connects such states, thereby creating avoided crossings and a first-order Stark effect which can strongly orient the states. Since this effect, termed ‘‘steric proficiency, ’’ operates over a narrow range of magnetic field strength, with amplitude determined by the electric dipole interaction, it should find use both for state selection and as a diagnostic tool for assigning spectral transitions. Other aspects are illustrated by strategies suggested for some prospective applications. These include a way to test whether formation of the A 2Σ+ excited electronic state of NaO in the Na+O3 reaction results from the orientation dependence of electron transfer, and techniques to enable the ground 2Σ+ states of RbO and CsO, produced by reacting NO2 with alkali atoms, to be loaded into a magnetic trap.

2001
Intersubband optical absorption in a quantum well under a tilted magnetic field

By using an appropriate coordinate transform we have calculated the intersubband optical absorption in the single square well under a tilted magnetic field. In this study the dependence of the intersubband transitions on the magnetic field strength and the direction of the magnetic field (tilt angle) is discussed. We show that intersubband optical absorption is sensitive to the tilt angle. This behaviour in the intersubband optical absorption gives a new degree of freedom in regions of interest device applications.

2005 - The Astrophysical Journal
On the Magnetic Field in the Kiloparsec-Scale Jet of Radio Galaxy M87

Several low-power kiloparsec-scale jets in nearby radio galaxies are known for their synchrotron radiation extending up to optical and X-ray photon energies. Here we comment on high-energy γ-ray emission of one particular object of this kind, i.e., the kiloparsec-scale jet of the M87 radio galaxy, resulting from Comptonization of the starlight photon field of the host galaxy by the synchrotron-emitting jet electrons. In our analysis, we include the relativistic bulk velocity of the jet, as well as the Klein-Nishina effects. We show that upper limits to the kiloparsec-scale jet inverse Compton radiation imposed by the HESS and HEGRA Cerenkov Telescopes—which detected a variable source of very high energy γ-ray emission within 01 (~30 kpc) of the M87 central region—give us an important constraint on the magnetic field strength in this object, namely, that the magnetic field cannot be smaller than the equipartition value (referring solely to the radiating electrons) in the brightest knot of the jet, and most likely, is even stronger. In this context, we point out a need for the amplification of the magnetic energy flux along the M87 jet from the subparsec to kiloparsec scales, suggesting the turbulent dynamo as a plausible process responsible for the aforementioned amplification.

2005 - Neurologia medico-chirurgica
Quantitative analysis of magnetic resonance imaging susceptibility artifacts caused by neurosurgical biomaterials: comparison of 0.5, 1.5, and 3.0 Tesla magnetic fields.

Magnetic resonance (MR) imaging is an important diagnostic tool for neurosurgical diseases but susceptibility artifacts caused by biomaterial instrumentation frequently causes difficulty in visualizing postoperative changes. The susceptibility artifacts caused by neurosurgical biomaterials were compared quantitatively by 0.5, 1.5, and 3.0 Tesla MR imaging. MR imaging of uniform size and shape of pieces ceramic (zirconia), pure titanium, titanium alloy, and cobalt-based alloy was performed at 0.5, 1.5, and 3.0 Tesla. A linear region of interest was defined across the center of the biomaterial in the transverse direction, and the susceptibility artifact diameter was calculated. Susceptibility artifacts developed around all biomaterials at all magnetic field strengths. The artifact diameters caused by pure titanium, titanium alloy, and cobalt-based alloy increased in the order of 0.5, 1.5, to 3.0 Tesla magnetic fields. The artifact diameter of ceramic was not influenced by magnetic field strength, and was the smallest of all biomaterials at all magnetic field strengths. The artifacts caused by biomaterials except ceramic increase with the magnetic field strength. Ceramic instrumentation will minimize artifacts in all magnetic fields.

2006 - Nuclear Fusion
Integrated physics optimization of a quasi-isodynamic stellarator with poloidally closed contours of the magnetic field strength

A quasi-isodynamic stellarator with poloidally closed contours of the magnetic field strength B (Mikhailov 2002 Nucl. Fusion 42 L23) has been obtained by an integrated physics optimization comprising MHD and neoclassical theory. For a configuration with six periods and aspect ratio approximately 12, a main result is the attainability of an essentially MHD-stable high-beta ([beta] approximate to 0.085) plasma with low neoclassical transport, approximately vanishing bootstrap current in the long-mean-free-path regime and excellent a-particle confinement.

2011 - 1106.3008
Confirmation of the magnetic oblique rotator model for the Of?p star HD 191612

This paper reports high-precision Stokes V spectra of HD 191612 acquired using the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope, in the context of the Magnetism in Massive Stars (MiMeS) Project. Using measurements of the equivalent width of the Ha line and radial velocities of various metallic lines, we have updated both the spectroscopic and orbital ephemerides of this star. We confirm the presence of a strong magnetic field in the photosphere of HD 191612, and detect its variability. We establish that the longitudinal field varies in a manner consistent with the spectroscopic period of 537.6d, in an approximately sinusoidal fashion. The phases of minimum and maximum longitudinal field are, respectively, coincident with the phases of maximum and minimum Ha equivalent width and Hp magnitude. This demonstrates a firm connection between the magnetic field and the processes responsible for the line and continuum variability. Interpreting the variation of the longitudinal magnetic field within the context of the dipole oblique rotator model, and adopting an inclination i = 30 degrees obtained assuming alignment of the orbital and rotational angular momenta, we obtain a best-fitting surface magnetic field model with obliquity beta = 67 degrees +/- 5 degrees and polar strength B-d = 2450 +/- 400 G. The inferred magnetic field strength implies an equatorial wind magnetic confinement parameter eta* similar or equal to 50, supporting a picture in which the H alpha emission and photometric variability have their origin in an oblique, rigidly rotating magnetospheric structure resulting from a magnetically channelled wind. This interpretation is supported by our successful Monte Carlo radiative transfer modelling of the photometric variation, which assumes the enhanced plasma densities in the magnetic equatorial plane above the star implied by such a picture, according to a geometry that is consistent with that derived from the magnetic field. Predictions of the continuum linear polarization resulting from Thompson scattering from the magnetospheric material indicate that the Stokes Q and U variations are highly sensitive to the magnetospheric geometry, and that expected amplitudes are in the range of current instrumentation.

2003 - astro-ph/0306065
PSR J1847–0130: A Radio Pulsar with Magnetar Spin Characteristics

We report the discovery of PSR J1847-0130, a radio pulsar with a 6.7 s spin period, in the Parkes Multibeam Pulsar Survey of the Galactic plane. The slowdown rate for the pulsar, 1.3 × 10-12 s s-1, is high and implies a surface dipole magnetic field strength of 9.4 × 1013 G. This inferred dipolar magnetic field strength is the highest by far among all known radio pulsars and over twice the "quantum critical field" above which some models predict radio emission should not occur. The inferred dipolar magnetic field strength and period of this pulsar are in the same range as those of the anomalous X-ray pulsars, which have been identified as being "magnetars" whose luminous X-ray emission is powered by their large magnetic fields. We have examined archival ASCA data and place an upper limit on the X-ray luminosity of J1847-0130 that is lower than the luminosities of all but one anomalous X-ray pulsar. The properties of this pulsar prove that inferred dipolar magnetic field strength and period cannot alone be responsible for the unusual high-energy properties of the magnetars and create new challenges for understanding the possible relationship between these two manifestations of young neutron stars.

2011 - Microfluidics and Nanofluidics
Numerical and experimental investigations of the formation process of ferrofluid droplets

This paper reports both experimental and numerical investigations of the formation process of ferrofluid droplets in a flow focusing configuration with and without an applied magnetic field. In the experiment, the homogenous magnetic field was generated using an electromagnet. The magnetic field in the flow direction affects the formation process and changes the size of the droplets. The change in the droplet size depends on the magnetic field strength and the flow rates. A numerical model was used to investigate the force balance during the droplet breakup process. A linearly magnetizable fluid was assumed. Particle level set method was employed to capture the interface movement between the continuous fluid and the dispersed fluid. Results of the droplet formation process and the flow field are discussed for both cases with and without the magnetic field. Finally, experimental and numerical results are compared.

2017 - 1707.05269
The JCMT BISTRO Survey: The Magnetic Field Strength in the Orion A Filament

We determine the magnetic field strength in the OMC 1 region of the Orion A filament via a new implementation of the Chandrasekhar–Fermi method using observations performed as part of the James Clerk Maxwell Telescope (JCMT) B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. We combine BISTRO data with archival SCUBA-2 and HARP observations to find a plane-of-sky magnetic field strength in OMC 1 of mG, where mG represents a predominantly systematic uncertainty. We develop a new method for measuring angular dispersion, analogous to unsharp masking. We find a magnetic energy density of J m−3 in OMC 1, comparable both to the gravitational potential energy density of OMC 1 (∼10−7 J m−3) and to the energy density in the Orion BN/KL outflow (∼10−7 J m−3). We find that neither the Alfvén velocity in OMC 1 nor the velocity of the super-Alfvénic outflow ejecta is sufficiently large for the BN/KL outflow to have caused large-scale distortion of the local magnetic field in the ∼500 yr lifetime of the outflow. Hence, we propose that the hourglass field morphology in OMC 1 is caused by the distortion of a primordial cylindrically symmetric magnetic field by the gravitational fragmentation of the filament and/or the gravitational interaction of the BN/KL and S clumps. We find that OMC 1 is currently in or near magnetically supported equilibrium, and that the current large-scale morphology of the BN/KL outflow is regulated by the geometry of the magnetic field in OMC 1, and not vice versa.

2009 - Nature
A strong, highly-tilted interstellar magnetic field near the Solar System

Magnetic fields play an important (sometimes dominant) role in the evolution of gas clouds in the Galaxy, but the strength and orientation of the field in the interstellar medium near the heliosphere has been poorly constrained. Previous estimates of the field strength range from 1.8–2.5 μG and the field was thought to be parallel to the Galactic plane or inclined by 38–60° (ref. 2) or 60–90° (ref. 3) to this plane. These estimates relied either on indirect observational inferences or modelling in which the interstellar neutral hydrogen was not taken into account. Here we report measurements of the deflection of the solar wind plasma flows in the heliosheath to determine the magnetic field strength and orientation in the interstellar medium. We find that the field strength in the local interstellar medium is 3.7–5.5 μG. The field is tilted ∼20–30° from the interstellar medium flow direction (resulting from the peculiar motion of the Sun in the Galaxy) and is at an angle of about 30° from the Galactic plane. We conclude that the interstellar medium field is turbulent or has a distortion in the solar vicinity.

2016 - IEEE Transactions on Microwave Theory and Techniques
Coil Design and Measurements of Automotive Magnetic Resonant Wireless Charging System for High-Efficiency and Low Magnetic Field Leakage

For wireless charging of electric vehicle (EV) batteries, high-frequency magnetic fields are generated from magnetically coupled coils. The large air-gap between two coils may cause high leakage of magnetic fields and it may also lower the power transfer efficiency (PTE). For the first time, in this paper, we propose a new set of coil design formulas for high-efficiency and low harmonic currents and a new design procedure for low leakage of magnetic fields for high-power wireless power transfer (WPT) system. Based on the proposed design procedure, a pair of magnetically coupled coils with magnetic field shielding for a 1-kW-class golf-cart WPT system is optimized via finite-element simulation and the proposed design formulas. We built a 1-kW-class wireless EV charging system for practical measurements of the PTE, the magnetic field strength around the golf cart, and voltage/current spectrums. The fabricated system has achieved a PTE of 96% at the operating frequency of 20.15 kHz with a 156-mm air gap between the coils. At the same time, the highest magnetic field strength measured around the golf cart is 19.8 mG, which is far below the relevant electromagnetic field safety guidelines (ICNIRP 1998/2010). In addition, the third harmonic component of the measured magnetic field is 39 dB lower than the fundamental component. These practical measurement results prove the effectiveness of the proposed coil design formulas and procedure of a WPT system for high-efficiency and low magnetic field leakage.

2006 - Magnetic Resonance in Medicine
High magnetic field water and metabolite proton T1 and T2 relaxation in rat brain in vivo

Comprehensive and quantitative measurements of T1 and T2 relaxation times of water, metabolites, and macromolecules in rat brain under similar experimental conditions at three high magnetic field strengths (4.0 T, 9.4 T, and 11.7 T) are presented. Water relaxation showed a highly significant increase (T1) and decrease (T2) with increasing field strength for all nine analyzed brain structures. Similar but less pronounced effects were observed for all metabolites. Macromolecules displayed field‐independent T2 relaxation and a strong increase of T1 with field strength. Among other features, these data show that while spectral resolution continues to increase with field strength, the absolute signal‐to‐noise ratio (SNR) in T1/T2‐based anatomical MRI quickly levels off beyond ∼7 T and may actually decrease at higher magnetic fields. Magn Reson Med, 2006. © 2006 Wiley‐Liss, Inc.

Magnetic processes in a collapsing dense core I. Accretion and ejection

P. Hennebelle
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P. Hennebelle
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S. Fromang
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S. Fromang

Abstract:Context. To understand the star formation process, it is important to study the collapse of a prestellar dense core. Aims. We investigate the effect of the magnetic field during the first collapse up to the formation of the first core, focusing particularly on the magnetic braking and the launching of outflows. Methods. We perform 3D AMR high resolution numerical simulations of a magnetically supercritical collapsing dense core using the RAMSES MHD code and develop semi-analytical models that we compare with the numerical results. Results. We study in detail the various profiles within the envelope of the collapsing core for various magnetic field strengths. Even modest values of magnetic field strength modify the collapse significantly. This is largely due to the amplification of the radial and toroidal components of the magnetic field by the differential motions within the collapsing core. For a weak magnetic intensity corresponding to an initial mass-to-flux over critical mass-to-flux ratio, μ equals 20 a centrifugally supported disk forms. The strong differential rotation triggers the growth of a slowly expanding magnetic tower. For higher magnetic field strengths corresponding to μ = 2, the collapse occurs primarily along the field lines, therefore delivering weaker angular momentum into the inner part whereas at the same time, strong magnetic braking occurs. As a consequence no centrifugally supported disk forms. An outflow is launched from the central thermally supported core. Detailed comparisons with existing analytical predictions indicate that it is magneto-centrifugally driven. Conclusions. For cores having a mass-to-flux over critical mass-to-flux radio μ < 5, the magnetic field appears to have a significant impact. The collapsing envelope is denser and flatter than in the hydrodynamical case and no centrifugally supported disk forms. For values μ < 20, the magnetic field drastically modifies the disk evolution. In a companion paper, the influence of the magnetic field on the dense core fragmentation is studied.

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引用
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Front. Astron. Space Sci.
2019
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2012
First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt
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2017
DETECTION OF A MAGNETIZED DISK AROUND A VERY YOUNG PROTOSTAR
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On the diversity and statistical properties of protostellar discs
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Grain growth in the envelopes and disks of Class I protostars
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ALMA Observations of Polarized 872 μm Dust Emission from the Protostellar Systems VLA 1623 and L1527
The Astrophysical Journal
2018
Multiline Observations of Molecular Bullets from a High-mass Protostar
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OUTFLOW FEEDBACK REGULATED MASSIVE STAR FORMATION IN PARSEC-SCALE CLUSTER-FORMING CLUMPS
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THE INFLUENCE OF MAGNETIC FIELDS ON THE THERMODYNAMICS OF PRIMORDIAL STAR FORMATION
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Small-scale dynamo action during the formation of the first stars and galaxies - I. The ideal MHD limit
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2010
H II REGIONS: WITNESSES TO MASSIVE STAR FORMATION
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Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
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ON THE ROLE OF PSEUDODISK WARPING AND RECONNECTION IN PROTOSTELLAR DISK FORMATION IN TURBULENT MAGNETIZED CORES
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Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO
Astronomy & Astrophysics
2020
The Role of Magnetic Fields in the Formation of Protostellar Discs
Front. Astron. Space Sci.
2018