相关论文
2018 - Astroparticle Physics
Binary neutron star merger remnants as sources of cosmic rays below the “Ankle”

Abstract We investigate non-thermal electron and nuclei energy losses within the binary neutron star merger remnant produced by the event GW170817. The lack of a cooling feature within the detected synchrotron emission from the source is used to constrain the magnetic field at the mG level, assuming that this emission is electron synchrotron in origin, and that the accelerated spectrum in the electrons follows the form d N / d E e ∝ E e − 2 . The level of subsequent gamma-ray emission from the source is demonstrated to provide a further constraint on the source magnetic field strength. We also put forward alternative strong ( ∼ G) magnetic field scenarios able to support this emission. For such stronger fields, the photo-disintegration of non-thermal nuclei within the source is considered, and a bottleneck period of  ∼ 5–30 days is found when this process peaks. We find that this class of source is in principle able to support the population of cosmic rays detected at Earth below the “ankle”.

1974
An investigation of the effect of an axial magnetic field on the He-Cd + laser

The drastic effect that a weak axial magnetic field can have upon the output of an He-Cd+ metal vapor laser is reported. A 37-percent increase in output power has been observed for a tube current of 55 mA and magnetic field strength of 70 G. Also described are parametric and spectroscopic studies performed to elucidate the cause of the large power output change.

1999 - Optics & Photonics
Electromagnetic Location System for Trapped Miners

Electromagnetic signals in the very low frequency range (VLF, below 10 kHz) can penetrate rock sufficiently far for miner's location with nearly no distribution of the field structure, if the near field condition is fulfilled. The relevant solutions of the Maxwell's equations for a magnetic dipole (transmitting antenna to be carried by the miner) in a dissipative medium then are independent of the medium. From these equations the magnetic field strength in any point of reception can be calculated. The key for the location method is the inverse distance function (locus curve), describing the possible location of the dipole from the measured field strength and direction in a point of reception (performed by the rescue team). At least two of these measurements give locus curves intersecting in two points, the correct solution can be found by means of an additional direction information calculated in the points of interest. A system has been built and successfully tested with miner's transmitters which can be activated by a coded signal on the rescue team, a receiver device measuring the field amplitude and field direction and a software package to calculate the miner's location on a notebook directly in the mine.

2020 - Physical Review D
Chiral phase structure of three flavor QCD in a background magnetic field

We investigate the chiral phase structure of three flavor QCD in a background $U(1)$ magnetic field using the standard staggered action and the Wilson plaquette gauge action. We perform simulations on lattices with a temporal extent of $N_\tau=4$ and four spatial extents of $N_\sigma = 8,16, 20$ and 24. We choose a smaller-than-physical quark mass in lattice spacing as $am = 0.030$ such that there exists a crossover transition at vanishing magnetic fields, and adopt two values of magnetic field strength in lattice spacing $a \sqrt{ e{B}}\simeq 1.5$ and 2. We find that the transition becomes stronger in the presence of a background magnetic field, and turns into a first order as seen from the volume scaling of the order parameter susceptibility as well as the metastable states in the time history of the chiral condensate. On the other hand, the chiral condensate and transition temperature always increase with $B$ even within the regime of a first order phase transition. This suggests that the discrepancy in the behavior of chiral condensates and transition temperature as a function of $B$ between earlier lattice studies using larger-than-physical pion masses with standard staggered fermions and those using physical pions with improved staggered fermions is mainly due to lattice cutoff effects.

1999 - IEEE Transactions on Magnetics
The STAR railgun concept

A novel concept for a staged augmented railgun is evaluated in which an external augmenting field would be applied to the bore of the railgun in addition to the self-induced magnetic field resulting from the current flow in the main rails. The augmenting magnetic field would be provided by multiple saddle-shaped coils located on the exterior of the gun barrel. These magnet coils, which would operate at high magnetic field strengths, would be transiently powered so that their magnetic field would only be present in the vicinity of the projectile. The energy contained in the coils would be transferred forward to successive coils as the projectile travels down the barrel. In principle, energy losses could therefore be minimized compared with other barrel concepts. However, a more detailed evaluation of this concept shows that very high voltages could be needed to power the coil, so that the concept may be unattractive for short barrels and high velocity applications.

2013 - 1312.0272
Submillimetre polarization and magnetic field properties in the envelopes of protoplanetary nebulae CRL 618 and OH 231.8+4.2

We have carried out continuum and line polarisation observations of two Proto-planetary nebulae (PPNe), CRL 618 and OH 231.8+4.2, using the Submillimeter Array (SMA) in its compact configuration. The frequency range of observations, 330-345 GHz, includes the CO(J=3-2) line emission. CRL 618 and OH 231.8+4.2 show quadrupolar and bipolar optical lobes, respectively, surrounded by a dusty envelope reminiscent of their AGB phase. We report a detection of dust continuum polarised emission in both PPNe above 4 sigma but no molecular line polarisation detection above a 3 sigma limit. OH 231.8+4.2 is slightly more polarised on average than CRL 618 with a mean fractional polarisation of 4.3 and 0.3 per cent, respectively. This agrees with the previous finding that silicate dust shows higher polarisation than carbonaceous dust. In both objects, an anti-correlation between the fractional polarisation and the intensity is observed. Neither PPNe show a well defined toroidal equatorial field, rather the field is generally well aligned and organised along the polar direction. This is clearly seen in CRL 618 while in the case of OH 231.8+4.2, the geometry indicates an X-shaped structure coinciding overall with a dipole/polar configuration. However in the later case, the presence of a fragmented and weak toroidal field should not be discarded. Finally, in both PPNe, we observed that the well organised magnetic field is parallel with the major axis of the 12CO outflow. This alignment could indicate the presence of a magnetic outflow launching mechanism. Based on our new high resolution data we propose two scenarios to explain the evolution of the magnetic field in evolved stars.

2011 - Physics of Fluids
Controllable adhesion using field-activated fluids

We demonstrate that field-responsive magnetorheological fluids can be used for variable-strength controllable adhesion. The adhesive performance is measured experimentally in tensile tests (a.k.a. probe-tack experiments) in which the magnetic field is provided by a cylindrical permanent magnet. Increasing the magnetic field strength induces higher peak adhesive forces. We hypothesize that the adhesion mechanism arises from the shear resistance of a yield stress fluid in a thin gap. This hypothesis is supported by comparing the experimentally measured adhesive performance to the response predicted by a lubrication model for a non-Newtonian fluid with a field-dependent yield stress. The model predictions are in agreement with experimental data up to moderate field strengths. Above a critical magnetic field strength the model over-predicts the experimentally measured values indicating non-ideal conditions such as local fluid dewetting from the surface.

2013
Measurement of Ion Cyclotron Emissions by Using High-Frequency Magnetic Probes in the LHD

Two pairs of high-frequency magnetic probes were installed in the Large Helical Device (LHD). During the injection of a perpendicular neutral beam, ion cyclotron emissions (ICEs) with the fundamental frequency corresponding to the ion cyclotron frequency at the plasma edge were detected, which are the same type of ICE as measured with the former spare ion cyclotron range of frequencies (ICRF) heating antennas. This type of ICE was further investigated with regard to the phase and intensity of signals. Another type of ICE was found in the LHD, and these ICEs were synchronized with bursts of toroidicity induced Alfvén eigenmodes (TAE) and the rise of intensity of lost ion flux. Therefore the source of these ICEs was thought to be the particles transferred from the core to the outer region of plasma by the TAE bursts. The frequency of ICEs induced by the TAE bursts increases linearly with the magnetic field strength, since the ion cyclotron frequency increases with the magnetic field strength.

2003 - astro-ph/0311121
Spot-like structures of neutron star surface magnetic fields

There is growing evidence, based on both X-ray and radio observations of isolated neutron stars, that besides the large-scale (dipolar) magnetic field, which determines the pulsar spin-down behaviour, small-scale poloidal field components are present, which have surface strengths one to two orders of magnitude larger than the dipolar component. We argue in this paper that the Hall-eect can be an ecient process in producing such small-scale field structures just above the neutron star surface. It is shown that due to a Hall-drift induced instability, poloidal magnetic field structures can be generated from strong subsurface toroidal fields, which are the result of either a dynamo or a thermoelectric instability acting at early times of a neutron star's life. The geometrical structure of these small-scale surface anomalies of the magnetic field resembles that of some types of "star-spots". The magnetic field strength and the length-scales are comparable with values that can be derived from various observations.

1983 - Ndt International
Measurements of the mechanical stress in mild steel by means of rotation of magnetic field strength —part 3: practical applications

Abstract An annealed disc of mild steel, 400 mm diameter and 12.7 mm thick, was compressed at the ends of a diameter. The isochromatic and isoclinic stress contours were measured magnetically using equipment called the Rotation Rig. The isochromatics agreed with the theoretical stress contours to within 20% and the agreement between isoclinics was ± 5°. Results are also given for the residual stresses around a weld in a steel plate, but these are not confirmed by an alternative method.

1996 - IEEE Transactions on Magnetics
The finite element modeling of static and stationary electric and magnetic fields

A finite-element method is described for computing static and stationary electric and magnetic fields directly in terms of the electric or magnetic field strength. In this way the use of (vector) potentials is avoided and a much higher accuracy is achieved with the same computational effort. The curl equation is supplemented with the electromagnetic compatibility relations and a problem is defined which is known to have a unique solution. For satisfying the conditions at the interfaces between different media use is made of both edge and nodal elements. The validity of our approach is illustrated by solving a simple sample problem.

1975 - Journal of Physics D
The vacuum arc in an axial magnetic field

An experimental and theoretical study of the behaviour of a vacuum arc on Cu and Mo electrodes in an axial magnetic field at currents between 150 A and 16 kA has been carried out. The maximum magnetic field strength was 0.25 T. It was found that the influence of the magnetic field on both the high- and low-current arc was determined by the ratio between the cyclotron frequency and collision frequency of the electrons. The relatively small difference in behaviour of the Mo and Cu arcs was explained by the presence of neutrals in the Cu arc, while in the Mo arc these particles were practically absent. Some conclusions have been made about the electron temperature and the energy losses of the individual arc columns observed at high magnetic field strengths.

2011 - 1107.0704
Detection of jet precession in the active nucleus of M 81

We report on very-long-baseline-interferometry (VLBI) monitoring observations of the low-luminosity active galactic nucleus (LLAGN) in the galaxy M 81 at the frequencies of 1.7, 2.3, 5.0, and 8.4 GHz. The observations reported here are phase-referenced to the supernova SN 1993J (located in the same galaxy) and cover from late 1993 to late 2005. The large amount of available observations allows us to study the stability of the AGN position in the frame of its host galaxy at different frequencies and chromatic effects in the jet morphology, together with their time evolution. The source consists at all frequencies of a slightly resolved core and a small jet extension towards the northeast direction (position angle of ~65 degrees) in agreement with previous publications. We find that the position of the intensity peak in the images at 8.4 GHz is very stable in the galactic frame of M 81 (proper motion upper limit about 10 μas per year). We confirm previous reports that the peaks at all frequencies are systematically shifted among them, possibly due to opacity effects in the jet as predicted by the standard relativistic jet model. We use this model, under plausible assumptions, to estimate the magnetic field in the jet close to the jet base and the mass of the central black hole. We obtain a black-hole mass of ~2 × 107 M âS(tm), comparable to estimates previously reported using different approaches, but the magnetic fields obtained are 10 3-104 times lower than previous estimates. We find that the positions of the cores at 1.7, 2.3, and 5.0 GHz are less stable than that at 8.4 GHz and evolve systematically, shifting southward at a rate of several tens of μas per year. The evolution in the jet orientation seems to be related to changes in the inclination of the cores at all frequencies. These results can be interpreted as due to a precessing jet. The evolving jet orientation also seems to be related to a flare in the peak flux densities at 5.0 and 8.4 GHz, which lasts ~4 years (from mid 1997 to mid 2001). An increase in the accretion rate of the black hole, and its correlation with the jet luminosity via the disk-jet connection model, seems insufficient to explain this long flare and the simultaneous evolution in the jet orientation. A continued monitoring of the flux density and the jet structure evolution in this LLAGN will be necessary to further confirm our jet precession model. © 2011 ESO.

2013 - Journal of geophysical research. Space physics
On the generation of magnetosheath high-speed jets by bow shock ripples

The terrestrial magnetosheath is embedded with coherent high‒speed jets of about 1RE in scale, predominantly during quasi‒radial interplanetary magnetic field (IMF). When these high dynamic pressure (Pdyn) jets hit the magnetopause, they cause large indentations and further magnetospheric effects. The source of these jets has remained controversial. One of the proposed mechanisms is based on ripples of the quasi‒parallel bow shock. In this paper, we combine for the first time, 4 years of subsolar magnetosheath observations from the Time History of Events and Macroscale Interactions during Substorms mission and corresponding NASA/OMNI solar wind conditions with model calculations of a rippled bow shock. Concentrating on the magnetosheath close to the shock during intervals when the angle between the IMF and the Sun‒Earth line was small, we find that (1) 97% of the observed jets can be produced by local ripples of the shock under the observed upstream conditions; (2) the coherent jets form a significant fraction of the high Pdyn tail of the magnetosheath flow distribution; (3) the magnetosheath Pdyn distribution matches the flow from a bow shock with ripples that have a dominant amplitude to wavelength ratio of about 9% (∼0.1RE/1RE) and are present ∼12% of the time at any given location.

2010 - Journal of Materials Chemistry
Non-contact actuation of triple-shape effect in multiphase polymer network nanocomposites in alternating magnetic field

Triple-shape polymers (TSP) can memorize two independent shapes, which are recovered when the temperature is subsequently increased. Certain applications do not allow triggering of the triple-shape effect (TSE) by environmental heating (e.g. potential damaging of surrounding tissue) and therefore require a non-contact activation. Here we explored whether polymer nanocomposites can be designed, which enable non-contact activation of TSE in an alternating magnetic field. A series of nanocomposites were synthesized by incorporation of silica coated iron(III)oxide nanoparticles into a polymer network matrix containing poly(e-caprolactone) (PCL) and poly(cyclohexyl methacrylate) (PCHMA) segments. Triple-shape functionalization of the materials was realized by application of different thermomechanical procedures (single or two dual-step), in which samples were deformed by bending to minimize changes in S/V ratio during shape recovery. For quantification of triple-shape properties inductive heating experiments were conducted in an alternating magnetic field at frequency of f = 258 kHz. By increasing the magnetic field strength H the triple-shape effect was triggered, while the maximum achievable temperature Tmax and the shape change was monitored using an infrared video camera. Excellent triple-shape properties were achieved for nanocomposites containing 40 wt-% of PCL exhibiting a two-step recovery of shapes B and C, when stimulated by step-wise increasing the magnetic field strength. In this way the TSE could be characterized by two distinct switching magnetic strengths Hsw,1(A → B) and Hsw,2(B → C) corresponding to the switching temperatures determined in cyclic, thermomechanical tensile tests for thermally-induced TSP.

2013 - Physical review letters
Critical magnetic field strength for suppression of the Richtmyer-Meshkov instability in plasmas.

The critical strength of a magnetic field required for the suppression of the Richtmyer-Meshkov instability (RMI) is investigated numerically by using a two-dimensional single-mode analysis. For the cases of magnetohydrodynamic parallel shocks, the RMI can be stabilized as a result of the extraction of vorticity from the interface. A useful formula describing a critical condition for magnetohydrodynamic RMI is introduced and is successfully confirmed by direct numerical simulations. The critical field strength is found to be largely dependent on the Mach number of the incident shock. If the shock is strong enough, even low-β plasmas can be subject to the growth of the RMI.

2019 - Physica A: Statistical Mechanics and its Applications
An experimental investigation for study the rheological behavior of water–carbon nanotube/magnetite nanofluid subjected to a magnetic field

Abstract This study aims at experimentally investigating the influence of magnetic field on the rheological behavior of water–carbon nanotube (CNT)/magnetite (Fe3O4) nanofluid. Tetramethylammonium hydroxide (TMAH) and Gum arabic (GA) are respectively used to stabilize the nanofluid. Scanning Electron Microscope (SEM), Dynamic Light Scattering (DLS) and X-ray Diffraction (XRD) methods were used to characterize the prepared nanofluid samples. Experiments were performed to evaluate the viscosity of water–CNT/magnetite nanofluid in the shear rate range of 1–100 s−1, volume fraction range of 0.5-1.5%, and magnetic field strength range of 0–480 mT. It was found that the presence of an external magnetic field causes an increase in the viscosity of the water–CNT/magnetite nanofluid. In addition, the results depicted that the viscosity of the nanofluid augments by boosting the concentration of the nano-materials. Moreover, it was reported that increasing the magnetic field strength to more than 360 mT has a negligible influence on the augmentation of nanofluid viscosity. Furthermore, the non-Newtonian shear thinning behavior was depicted because of the decrease in viscosity with intensifying the shear rates.

1985 - Journal of Geophysical Research
An ISEE 3 study of average and substorm conditions in the distant magnetotail

Average and substorm conditions in the lobe and plasma sheet regions of the earth's magnetotail are studied as a function of downstream distance and east-west location using ISEE 3 magnetometer and plasma analyzer measurements. On the basis of 756 magnetopause crossings a low-latitude magnetotail diameter of 60±5 RE at |X| = 130 - 225 RE is determined. The strength of the lobe magnetic field from |X| = 20 to 130 RE is shown to fall off as X−0.53±0.05. Flaring ceases on average at |X| = 120 ± 10 RE with a relatively constant BL = 9.2 nT beyond that distance. The ratios |By/Bx| and |Bz/Bx| in the translunar tail lobes are small and relatively constant with mean values of 0.10 and 0.06, respectively. These results are shown to be in good agreement with the Coroniti-Kennel flaring tail models of lobe magnetic field configuration with slightly enhanced By due to Maxwell stresses exerted at the magnetopause by the solar wind. The plasma parameters Vx, ne, βe, and MA in the lobes all increase with distance down the tail while Te decreases. The mean values of these lobe quantities at |X| = 200 - 220 RE are Vx = −200 - 250 km/s, n = 0.1 - 0.2 cm−3, βe = 0.02 - 0.05, MA = 0.3 - 0.4, and Te = 5 - 8×105 °K. Strong density and weak velocity and temperature gradients are observed as ISEE 3 moves from the center of the lobes out toward the magnetopause. In particular, factor of 3–6 increases in plasma density are observed as the spacecraft moves from the center of the tail at |Y′| 20 RE. Good agreement is found between the leaky magnetopause model of Pilipp and Morfill (1978) and the strong density/weak velocity gradients observed in the lobes. Substorm activity, as measured by AE(9), is only weakly correlated with magnetic field strength, electron beta, or Alfvenic Mach number in the lobes at |X| > 200 RE. The plasma sheet magnetic field intensity and electron temperature decrease with increasing downstream distance, while flow speed, density, and Alfvenic Mach number all increase. Average plasma sheet parameters at |X| = 200 - 220 RE are B = 4.0 nT, Vx = −500 km/s, ne = 0.3 cm−3, Te = 1.2×106 °K, and MA = 2.7. Electron beta is independent of downstream distance with a mean value of approximately 0.7. On the basis of pressure balance arguments the estimated total plasma beta in the |X| > 60 RE plasma sheet is 4.5, and the Ti/Te ratio is 5.5. With respect to reconnection, the most significant results are the correlations between Bz, Vx, and AE(9) in the plasma sheet, the variation in these parameters with X and ± Y, and their implications for the location of the distant neutral line. The highest tailward flow speeds are found to be proportional to the magnitude of the embedded southward Bz. Furthermore, both tailward Vx and southward Bz are shown to be well correlated with AE(9). Earthward of |X| = 100 RE the average Bz is northward and the flow is on average sub-Alfvenic. Between |X| = 100 and 180 RE the flow becomes predominantly tailward and super-Alfvenic, MA = 1 - 2, across the entire width of the tail. However, the average magnetic field is found to be southward only in a 10 RE wide region near the aberrated noon-midnight meridian. At |X| = 180 - 225 RE the flow speed is somewhat higher, MA = 2 - 3, and the width of the region of southward Bz grows to 30 RE. Tailward flow speed and electron temperature exhibit maxima in the central portion of the plasma sheet where Bz 15 RE, where Bz > 0, the flow direction remains tailward, albeit at a reduced speed. The magnetic field results are interpreted in terms of a curved distant neutral line which is located at |X| = 100 - 140 RE near local midnight. Along the flanks of the magnetotail closed field lines are apparently still being swept tailward at |X| = 200 RE. In summary, there is general agreement between the ISEE 3 magnetic field and plasma measurements in the distant magnetotail and many of the predictions of reconnection theory, but the existing theoretical models will have to be extended to three dimensions before these observations can be fully understood.

2001 - The Astrophysical Journal
Intergalactic Magnetic Fields from Quasar Outflows

Outflows from quasars inevitably pollute the intergalactic medium (IGM) with magnetic fields. The short-lived activity of a quasar leaves behind an expanding magnetized bubble in the IGM. We model the expansion of the remnant quasar bubbles and calculate their distribution as a function of size and magnetic field strength at different redshifts. We generically find that by a redshift z ~ 3, about 5%-20% of the IGM volume is filled by magnetic fields with an energy density 10% of the mean thermal energy density of a photoionized IGM (at ~104 K). As massive galaxies and X-ray clusters condense out of the magnetized IGM, the adiabatic compression of the magnetic field could result in the field strength observed in these systems without a need for further dynamo amplification. The intergalactic magnetic field could also provide a nonthermal contribution to the pressure of the photoionized gas that may account for the claimed discrepancy between the simulated and observed Doppler width distributions of the Ly? forest.

1987 - Physica Scripta
Atoms in strong magnetic fields

We review recent results of investigations of hydrogen-like systems at magnetic field strengths where the Lorentz forces are comparable to, or larger than, the Coulomb binding forces. This situation is realized for low-lying states at field strengths typical of magnetic white dwarfs and neutron stars, while for Rydberg states already laboratory field strengths are sufficient. We discuss the wavelength spectrum of the hydrogen atom in magnetic fields of arbitrary strength, and describe in which way the spectroscopy of "stationary lines", which appear in this spectrum, has made possible the detection of the largest magnetic field strength ever found in a white dwarf star to date. For Rydberg states in strong laboratory fields we perform a quantitative comparison between experimental and theoretical spectra, and demonstrate that symptoms of "quantum stochasticity" are recovered in the spectra of magnetized Rydberg atoms. In particular we point out that the breakdown of quasi-separability in the quantal problem is closely related to the disappearance of regular orbits in the classical problem. We conclude that magnetized Rydberg atoms lend themselves as ideal objects in which to study, theoretically and experimentally, manifestations of quantum stochasticity.

Toward a Universal Scaling Relation between Jet Power and Radio Power

C. Carilli
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P. Nulsen
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L. Bîrzan
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D. Rafferty
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B. McNamara
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M. Wise

Abstract:We present an analysis of the energetics and particle content of the lobes of 24 radio galaxies at the cores of cooling clusters. The radio lobes in these systems have created visible cavities in the surrounding hot, X-ray-emitting gas, which allow direct measurement of the mechanical jet power of radio sources over six decades of radio luminosity, independently of the radio properties themselves. We find that jet (cavity) power increases with radio synchrotron power approximately as P-jet similar to L-radio(beta), where 0.35 <= beta <= 0.70 depending on the bandpass of measurement and state of the source. However, the scatter about these relations caused by variations in radiative efficiency spans more than 4 orders of magnitude. A number of factors contribute to this scatter, including aging, entrainment, variations in magnetic field strengths, and the partitioning of energy between electrons and nonradiating heavy particles. After accounting for variations in synchrotron break frequency (age), the scatter is reduced by approximate to 50%, yielding the most accurate scaling relation available between the lobe radio power and the jet (cavity) power. Furthermore, we place limits on the magnetic field strengths and particle content of the radio lobes using a variety of X-ray constraints. We find that the lobe magnetic field strengths vary between a few to several tens of microgauss depending on the age and dynamical state of the lobes. If the cavities are maintained in pressure balance with their surroundings and are supported by internal fields and particles in equipartition, the ratio of energy in electrons to heavy particles (k) must vary widely from approximately unity to 4000, consistent with heavy (hadronic) jets.

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引用
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