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Results for “MAGNETIC DIPOLES”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 199 records · Page 11
All sourcesNASA NTRSDOE OSTI
DOE OSTI2013

Near-field heat transfer between gold nanoparticle arrays

The radiative heat transfer between gold nanoparticle layers is presented using the coupled dipole method. Gold nanoparticles are modelled as effective electric and magnetic dipoles interacting via electromagnetic fluctuations. The effect of higher-order multipoles is implemented in the expression of electric polarizability to calculate the interactions at short distances. Our findings show that the near-field radiation reduces as the radius of the nanoparticles is increased. Also, the magnetic dipole contribution to the heat exchange becomes more important for larger particles. When one layer is displayed in parallel with respect to the other layer, the near-field heat transfer exhibits oscillatory-like features due to the influence of the individual nanostructures. Further details about the effect of the nanoparticles size are also discussed.

71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSIC↗
DOE OSTI2014

Rare-RI ring for mass measurements at RIBF

The rare-RI (radioactive isotope) ring at the RIKEN RI Beam Factory is described. The main purpose of the rare-RI ring is to measure the mass of short-lived rare RI. In the rare-RI ring, the mass is determined by measuring the revolution time of each nucleus based on isochronous mass spectrometry. The rare-RI ring consists of six magnetic sectors, and each sector consists of four dipole magnets. To precisely optimize the isochronous conditions of the circulating particles for large acceptance, we install 10 trim coils to half of the dipole magnets. Individual injection system enables efficient injection of the produced rare RI into the ring one by one. With facilitating efficient extraction of the circulating particles, time-of-flight measurements can be performed to the each rare RI. Construction of the rare-RI ring was begun in the middle of the fiscal year 2012, and the ring is expected to be fully functional by 2015, when we can start the mass measurements for unknown masses.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2019

Bistable and Multi-Domain States of α-Fe/(PrDy)(FeCo)B Ferromagnetic Microwires

In this paper, we obtained α-Fe(50 at %)(PrDy)(FeCo)B(48 at %) microwires by extraction of a hanging drop of the (PrDy)(FeCo)B melt in the electron beam. A single microwire with a diameter of 50 μm and a length of 0.8–6 mm and with an amorphous (PrDy)(FeCo)B content of ~48% and a polycrystalline α‑Fe phase of ~52% is shown to have a rectangular narrow magnetic hysteresis loop and, accordingly, a bistable state with a switching field of ~100 Oe. Shortening the wire to ~0.6 mm leads to a sharp deviation from the loop rectangularity and a decrease in the slope of the dependence of magnetization on the field and coercive force to 20 Oe. In the near-surface layers consisting of an amorphous phase (PrDy)(FeCo)B, oriented regions of reverse magnetization are observed. The role of the magnetic dipole interaction in the formation of the magnetic hysteresis loop of chaotic ensembles of microwires with various compositions is discussed.

75 CONDENSED MATTER PHYSICS, SUPERCONDUCTIVITY AND↗
DOE OSTI2019

Theoretical level energies and transition data for 4p{sup 6}4d{sup 5}, 4p{sup 5}4d{sup 6} and 4p{sup 6}4d{sup 4}4f configurations of W{sup 33+} ion

The ab initio quasirelativistic approach developed specifically for the calculation of spectral parameters of highly charged ions was used to derive transition data for the Nb-like tungsten ion W{sup 33+}. The configuration interaction method was applied to include electron correlation effects. The relativistic effects were taken into account in the Breit–Pauli approximation. The level energies, radiative lifetimes τ, Landé g-factors were determined for the ground configuration 4p{sup 6}4d{sup 5} and two excited configurations 4p{sup 5}4d{sup 6} and 4p{sup 6}4d{sup 4}4f. The radiative transition wavelengths λ and emission transition probabilities A for the electric dipole, electric quadrupole, electric octupole, magnetic dipole, and magnetic quadrupole transitions among the levels of these configurations were produced. The uncertainties of computed spectroscopic parameters were evaluated.

74 ATOMIC AND MOLECULAR PHYSICS↗
DOE OSTI2021

Light(ly)-coupled dark matter in the keV range: freeze-in and constraints

Dark matter produced from thermal freeze-out is typically restricted to have masses above roughly 1 MeV. However, if the couplings are small, the freeze-in mechanism allows for production of dark matter down to keV masses. We consider dark matter coupled to a dark photon that mixes with the photon and dark matter coupled to photons through an electric or magnetic dipole moment. We discuss contributions to the freeze-in production of such dark matter particles from standard model fermion-antifermion annihilation and plasmon decay. We also derive constraints on such dark matter from the cooling of red giant stars and horizontal branch stars, carefully evaluating the thermal processes as well as the bremsstrahlung process that dominates for masses above the plasma frequency. We find that the parameters needed to obtain the observed relic abundance from freeze-in are excluded below a few tens of keV, depending on the value of the dark gauge coupling constant for the dark photon portal model, and below a few keV, depending on the reheating temperature for dark matter with an electric or magnetic dipole moment. While laboratory probes are unlikely to probe these freeze-in scenarios in general, we show that for dark matter with an electric or magnetic dipole moment and for dark matter masses above the reheating temperature, the couplings needed for freeze-in to produce the observed relic abundance can be probed partially by upcoming direct-detection experiments.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2016

Comparison of electric dipole and magnetic loop antennas for exciting whistler modes

The excitation of low frequency whistler modes from different antennas has been investigated experimentally in a large laboratory plasma. One antenna consists of a linear electric dipole oriented across the uniform ambient magnetic field B{sub 0}. The other antenna is an elongated loop with dipole moment parallel to B{sub 0}. Both antennas are driven by the same rf generator which produces a rf burst well below the electron cyclotron frequency. The antenna currents as well as the wave magnetic fields from each antenna are measured. Both the antenna currents and the wave fields of the loop antenna exceed that of the electric dipole by two orders of magnitude. The conclusion is that loop antennas are far superior to dipole antennas for exciting large amplitude whistler modes, a result important for active wave experiments in space plasmas.

70 PLASMA PHYSICS AND FUSION TECHNOLOGY↗
DOE OSTI2016

Measurement of the radiative decay rate and energy of the metastable (2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub (J=0)} level in Fe xvii

Measurements at the Livermore electron beam ion trap have been performed in order to infer the energy and the radiative lifetime of the (1s{sup 2}2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub J=0} level in the Fe xvii spectrum. This is the longest-lived level in the neonlike iron ion, and its radiative decay produces the Fe xvii line at 1153 Å, feeding the population of the (1s{sup 2}2s{sup 2}2p{sub 3/2}{sup 5}3s{sub 1/2}){sub J=1} upper level of one of the most prominent lines in the Fe xvii L-shell X-ray spectrum, commonly dubbed 3G. In the presence of a strong (⩾ few kG) magnetic field, the (1s{sup 2}2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub J=0} level has a finite probability to decay directly to the (1s{sup 2}2s{sup 2}2p{sup 6}){sub J=0} neonlike ground level via the emission of an L-shell X-ray. Our measurements allow us to observe this X-ray line in the Fe xvii L-shell spectrum and from it to infer the radiative rate for the magnetic dipole decay of the (1s{sup 2}2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub J=0} level to the (1s{sup 2}2s{sup 2}2p{sub 3/2}{sup 5}3s{sub 1/2}){sub J=1}. Our result of (1.45±0.15)×10{sup 4} s{sup −1} is in agreement with predictions. We have also measured the wavelength of the associated X-ray line to be 16.804 ± 0.002 Å, which means that the line is displaced 1.20 ± 0.05 eV from the neighboring (2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub J=1}→(2s{sup 2}2p{sup 6}){sub J=0} transition, commonly labeled 3F. From our measurement, we infer 5950570 ± 710 cm{sup −1} for the energy of the (1s{sup 2}2s{sup 2}2p{sub 1/2}{sup 5}3s{sub 1/2}){sub J=0} level.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2016

Mergers of charged black holes: gravitational-wave events, short gamma-ray bursts, and fast radio bursts

The discoveries of GW150914, GW151226, and LVT151012 suggest that double black hole (BH–BH) mergers are common in the universe. If at least one of the two merging black holes (BHs) carries a certain amount of charge, possibly retained by a rotating magnetosphere, the inspiral of a BH–BH system would drive a global magnetic dipole normal to the orbital plane. The rapidly evolving magnetic moment during the merging process would drive a Poynting flux with an increasing wind power. The magnetospheric activities during the final phase of the merger would make a fast radio burst (FRB) if the BH charge can be as large as a factor of q-hat ∼(10{sup −9}--10{sup −8}) of the critical charge Q {sub c} of the BH. At large radii, dissipation of the Poynting flux energy in the outflow would power a short-duration high-energy transient, which would appear as a detectable short-duration gamma-ray burst (GRB) if the charge can be as large as q-hat ∼(10{sup −5}--10{sup −4}). The putative short GRB coincident with GW150914 recorded by Fermi GBM may be interpreted with this model. Future joint GW/GRB/FRB searches would lead to a measurement or place a constraint on the charges carried by isolate BHs.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

Quadrupole magnet for a rapid cycling synchrotron

Rapid Cycling Synchrotrons (RCS) feature interleaved warm and cold dipole magnets; the field of the warm magnets is used to modulate the average bending field depending on the particle energy. It has been shown that RCS can be an attractive option for fast acceleration of particles, for example, muons, which decay quickly. In previous studies it was demonstrated that in principle warm dipole magnets can be designed which can provide the required ramp rates, which are equivalent to frequencies of about 1 kHz. To reduce the losses it is beneficial to employ two separate materials for the yoke; it was also shown that by employing an optimized excitation coil geometry the eddy current losses are acceptable. In this paper we show that the same principles can be applied to quadrupole magnets targeting 30 T/m with a repetition rate of 1kHz and good field quality.

43 PARTICLE ACCELERATORS↗
DOE OSTI2013

Energy levels, wavelengths, and transition rates of multipole transitions (E1, E2, M1, M2) in Au{sup 67+} and Au{sup 66+} ions

The fully relativistic configuration interaction method of the FAC code is used to calculate atomic data for multipole transitions in Mg-like Au (Au{sup 67+}) and Al-like Au (Au{sup 66+}) ions. Generated atomic data are important in the modeling of M-shell spectra for heavy Au ions and Au plasma diagnostics. Energy levels, oscillator strengths and transition rates are calculated for electric-dipole (E1), electric quadrupole (E2), magnetic dipole (M1), and magnetic quadrupole (M2) for transitions between excited and ground states 3l−nl{sup ′}, such that n=4,5,6,7. The local central potential is derived using the Dirac–Fock–Slater method. Correlation effects to all orders are considered by the configuration interaction expansion. All relativistic effects are included in the calculations. Calculated energy levels are compared against published values that were calculated using the multi-reference many body perturbation theory, which includes higher order QED effects. Favorable agreement was observed, with less than 0.15% difference.

74 ATOMIC AND MOLECULAR PHYSICS↗
DOE OSTI2019

Energy levels and transition rates for Al-like Cu XVII

Energy levels and transition rates for electric-dipole, electric-quadrupole, magnetic-dipole, and magnetic-quadrupole transitions among the levels arising from the n≤5 configurations in Al-like Cu XVII are calculated respectively by two state-of-the-art methods, namely, the Multi-Configuration Dirac–Hartree–Fock approach and the second-order many-body perturbation theory. Our results are compared with available experimental and other theoretical values. In addition, effective collision strengths of direct excitation between these levels are provided using the distorted wave approximation. Several line pairs are pointed out that might be useful for density diagnostics.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2015

Deep NuSTAR and Swift monitoring observations of the magnetar 1E 1841−045

We report on a 350 ks NuSTAR observation of the magnetar 1E 1841–045 taken in 2013 September. During the observation, NuSTAR detected six bursts of short duration, with T{sub 90} ≲ 1 s. An elevated level of emission tail is detected after the brightest burst, persisting for ∼1 ks. The emission showed a power-law decay with a temporal index of 0.5 before returning to the persistent emission level. The long observation also provided detailed phase-resolved spectra of the persistent X-ray emission of the source. By comparing the persistent spectrum with that previously reported, we find that the source hard-band emission has been stable for over approximately 10 yr. The persistent hard-X-ray emission is well fitted by a coronal outflow model, where e{sup ±} pairs in the magnetosphere upscatter thermal X-rays. Our fit of phase-resolved spectra allowed us to estimate the angle between the rotational and magnetic dipole axes of the magnetar, α{sub mag}=0.25, the twisted magnetic flux, 2.5 × 10{sup 26} G cm{sup 2}, and the power released in the twisted magnetosphere, L{sub j} = 6 × 10{sup 36} erg s{sup −1}. Assuming this model for the hard-X-ray spectrum, the soft-X-ray component is well fit by a two-blackbody model, with the hotter blackbody consistent with the footprint of the twisted magnetic field lines on the star. We also report on the 3 yr Swift monitoring observations obtained since 2011 July. The soft-X-ray spectrum remained stable during this period, and the timing behavior was noisy, with large timing residuals.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

H{sub 2} X{sup 1}Σ{sub g}{sup +}−c{sup 3}Π{sub u} Excitation by Electron Impact: Energies, Spectra, Emission Yields, Cross-sections, and H(1s) Kinetic Energy Distributions

The c{sup 3}Π{sub u} state of the hydrogen molecule has the second largest triplet-state excitation cross-section, and plays an important role in the heating of the upper thermospheres of outer planets by electron excitation. Precise energies of the H{sub 2}, D{sub 2}, and HD c{sup 3}Π{sub u}{sup −}(v,N) levels are calculated from highly accurate ab initio potential energy curves that include relativistic, radiative, and empirical non-adiabatic corrections. The emission yields are determined from predissociation rates and refined radiative transition probabilities. The excitation function and excitation cross-section of the c{sup 3}Π{sub u} state are extracted from previous theoretical calculations and experimental measurements. The emission cross-section is determined from the calculated emission yield and the extracted excitation cross-section. The kinetic energy (E {sub k}) distributions of H atoms produced via the predissociation of the c{sup 3}Π{sub u} state, the c{sup 3}Π{sub u}{sup −} – b{sup 3}Σ{sub u}{sup +} dissociative emission by the magnetic dipole and electric quadrupole, and the c{sup 3}Π{sub u} – a{sup 3}Σ{sub g}{sup +} – b{sup 3}Σ{sub u}{sup +} cascade dissociative emission by the electric dipole are obtained. The predissociation of the c{sup 3}Π{sub u}{sup +} and c{sup 3}Π{sub u}{sup −} states both produce H(1s) atoms with an average E {sub k} of ∼4.1 eV/atom, while the c{sup 3}Π{sub u}{sup −} – b{sup 3}Σ{sub u}{sup +} dissociative emissions by the magnetic dipole and electric quadrupole give an average E {sub k} of ∼1.0 and ∼0.8 eV/atom, respectively. The c{sup 3}Π{sub u} – a{sup 3}Σ{sub g}{sup +} – b{sup 3}Σ{sub u}{sup +} cascade and dissociative emission gives an average E {sub k} of ∼1.3 eV/atom. On average, each H{sub 2} excited to the c{sup 3}Π{sub u} state in an H{sub 2}-dominated atmosphere deposits ∼7.1 eV into the atmosphere while each H{sub 2} directly excited to the a{sup 3}Σ{sub g}{sup +} and d{sup 3}Π{sub u} states contribute ∼2.3 and ∼3.3 eV, respectively, to the atmosphere. The spectral distribution of the calculated continuum emission arising from the X{sup 1}Σ{sub g}{sup +} – c{sup 3}Π{sub u} excitation is significantly different from that of direct a{sup 3}Σ{sub g}{sup +} or d{sup 3}Π{sub u} excitations.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2015

High-precision three-dimensional field mapping of a high resolution magnetic spectrometer for hypernuclear spectroscopy at JLab

The High Resolution Kaon Spectrometer (HKS), which consists of two quadrupole magnets and one dipole magnet, was designed and constructed for high-resolution spectroscopy of hypernuclei using the (e,e'K+) reaction in Hall C, Jefferson Lab (JLab). It was used to analyze momenta of around 1.2 GeV/c K^+ s with a resolution of 2 ×10^-4 (FWHM). To achieve the target resolution, a full three-dimensional magnetic field measurement of each magnet was successfully performed, and a full three-dimensional magnetic field map of the HKS magnets was reconstructed. Using the measured field map, the initial reconstruction function was generated. The target resolution would be achieved via careful tuning of the reconstruction function of HKS with the p(e,e'K+)Lambda,Sigma^0 and C-12 (e,e'K+)12_Lambda B_g.s. reactions. After tuning of the initial reconstruction function generated from the measured map, the estimated HKS momentum resolution was 2.2×10^-4 (FWHM).

Fujii, Yuu (ORCID:0000000166252241)↗
DOE OSTI2014

Magnetohydrodynamic simulations of hot jupiter upper atmospheres

Two-dimensional simulations of hot Jupiter upper atmospheres including the planet's magnetic field are presented. The goal is to explore magnetic effects on the layer of the atmosphere that is ionized and heated by stellar EUV radiation, and the imprint of these effects on the Lyα transmission spectrum. The simulations are axisymmetric, isothermal, and include both rotation and azimuth-averaged stellar tides. Mass density is converted to atomic hydrogen density through the assumption of ionization equilibrium. The three-zone structure—polar dead zone (DZ), mid-latitude wind zone (WZ), and equatorial DZ—found in previous analytic calculations is confirmed. For a magnetic field comparable to that of Jupiter, the equatorial DZ, which is confined by the magnetic field and corotates with the planet, contributes at least half of the transit signal. For even stronger fields, the gas escaping in the mid-latitude WZ is found to have a smaller contribution to the transit depth than the equatorial DZ. Transmission spectra computed from the simulations are compared to Hubble Space Telescope Space Telescope Imaging Spectrograph and Advanced Camera for Surveys data for HD 209458b and HD 189733b, and the range of model parameters consistent with the data is found. The central result of this paper is that the transit depth increases strongly with magnetic field strength when the hydrogen ionization layer is magnetically dominated, for dipole magnetic field B {sub 0} ≳ 10 G. Hence transit depth is sensitive to magnetic field strength, in addition to standard quantities such as the ratio of thermal to gravitational binding energies. Another effect of the magnetic field is that the planet loses angular momentum orders of magnitude faster than in the non-magnetic case, because the magnetic field greatly increases the lever arm for wind braking of the planet's rotation. Spin-down timescales for magnetized models of HD 209458b that agree with the observed transit depth can be as short as ≅ 30 Myr, which is much shorter than the age of the system.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

Axion induced oscillating electric dipole moments

In this study, the axion electromagnetic anomaly induces an oscillating electric dipole for any magnetic dipole. This is a low energy theorem which is a consequence of the space-time dependent cosmic background field of the axion. The electron will acquire an oscillating electric dipole of frequency m a</> and strength ~ 10 -32 e-cm, within four orders of magnitude of the present standard model DC limit, and two orders of magnitude above the nucleon, assuming standard axion model and dark matter parameters. This may suggest sensitive new experimental venues for the axion dark matter search.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2018

A Comprehensive Comparison of Relativistic Particle Integrators

We compare relativistic particle integrators commonly used in plasma physics, showing several test cases relevant for astrophysics. Three explicit particle pushers are considered, namely, the Boris, Vay, and Higuera–Cary schemes. We also present a new relativistic fully implicit particle integrator that is energy conserving. Furthermore, a method based on the relativistic guiding center approximation is included. The algorithms are described such that they can be readily implemented in magnetohydrodynamics codes or Particle-in-Cell codes. Here, our comparison focuses on the strengths and key features of the particle integrators. We test the conservation of invariants of motion and the accuracy of particle drift dynamics in highly relativistic, mildly relativistic, and non-relativistic settings. The methods are compared in idealized test cases, i.e., without considering feedback onto the electrodynamic fields, collisions, pair creation, or radiation. The test cases include uniform electric and magnetic fields, ${\boldsymbol{E}}\times {\boldsymbol{B}}$ fields, force-free fields, and setups relevant for high-energy astrophysics, e.g., a magnetic mirror, a magnetic dipole, and a magnetic null. These tests have direct relevance for particle acceleration in shocks and in magnetic reconnection.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

Fabrication and test of model superconducting inflector for g-2 at FNAL

The new FNAL g-2 experiment is based on the muon storage ring previously used at BNL. The 1.45 T dipole magnetic field in the storage ring is required to have very high (1 ppm) homogeneity. The muon beam injected into the ring must be transported through the magnet yoke and the main superconducting coil cryostat with minimal distortions. The old inflector magnet shielded the main dipole fringe field inside the muon transport beam pipe, with an outer NbTi superconducting screen, and did not disturb the field in the area of circulating beam. Nevertheless, this magnet had coils with closed ends in which a large fraction of muon beam particles were lost. A new magnet is envisioned utilizing the same cross section as the original with open ends for improved beam transport. A model magnet has been wound utilizing 3d printed parts to verify the magnetic behavior of the magnet at room temperature and validate winding of the complicated geometry required for the magnet ends. Finally, room temperature magnetic measurements have been performed and confirm the magnetic design

43 PARTICLE ACCELERATORS↗