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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 1,081 records · Page 60
All sourcesNASA NTRSDOE OSTI
DOE OSTI2017

Single-ion properties of the S eff = 1 2 XY antiferromagnetic pyrochlores Na A ' Co 2 F 7 ( A ' = Ca 2 + , Sr 2 + )

The antiferromagnetic pyrochlore material NaCaCo 2 F 7 is a thermal spin liquid over a broad temperature range (≈140 K down to T F =2.4 K), in which magnetic correlations between Co 2+ dipole moments explore a continuous manifold of antiferromagnetic XY states. The thermal spin liquid is interrupted by spin freezing at a temperature that is ~2% of the mean-field interaction strength, leading to short-range static XY clusters with distinctive relaxation dynamics. Here we report the low-energy inelastic neutron scattering response from the related compound NaSrCo 2 F 7 , confirming that it hosts the same static and dynamic spin correlations as NaCaCo 2 F 7 . We then present the single-ion levels of Co 2+ in these materials as measured by inelastic neutron scattering. An intermediate spin-orbit coupling model applied to an ensemble of trigonally distorted octahedral crystal fields accounts for the observed transitions. The single-ion ground state of Co 2+ is a Kramers doublet with a strongly XY-like g tensor ( gxy/gz ~3). The local disorder inherent from the mixed pyrochlore A sites (Na + /Ca 2+ and Na + /Sr 2+ ) is evident in these measurements as exaggerated broadening of some of the levels. A simple model that reproduces the salient features of the single-ion spectrum produces approximately 8.4% and 4.1% variation in the z and xy components of the g tensor, respectively. In conclusion, this study confirms that an S eff = 1/2 model with XY antiferromagnetic exchange and weak exchange disorder serves as a basic starting point in understanding the low-temperature magnetic behavior of these strongly frustrated magnets.

36 MATERIALS SCIENCE↗
NASA NTRS1976

An evaluation of recent quantitative magnetospheric magnetic field models

Magnetospheric field models involving dipole tilt effects are discussed, with particular reference to defined magnetopause models and boundary surface models. The models are compared with observations and with each other whenever possible. It is shown that models containing only contributions from magnetopause and tail current systems are capable of reproducing the observed quiet time field just in a qualitative way. The best quantitative agreement between models and observations take place when currents distributed in the inner magnetosphere are added to the magnetopause and tail current systems. One region in which all the models fall short is the region around the polar cusp. Obtaining physically reasonable gradients should have high priority in the development of future models.

Walker, R. J.↗
DOE OSTI2017

Mode Change of a Gamma-Ray Pulsar, PSR J2021+4026

A glitch of a pulsar is known as a sudden increase in the spin frequency and spin-down rate (frequency time derivative), and it can be caused by a sudden release of the stress built up in the solid crust of the star or pinned vortices in the superfluid interior. PSR J2021+4026 is the first pulsar that shows a significant change in the gamma-ray flux and pulse profile at the glitch that occurred around 2011 October 16. We report the results of timing and spectral analysis of PSR J2021+4026 using ∼8 yr Fermi Large Area Telescope data. We find that the pulsar stayed at a high spin-down rate (∼4% higher than the pre-glitch value) and a low gamma-ray state (∼18% lower) for about 3 yr after the glitch. Around 2014 December, the spin-down rate and gamma-ray flux gradually returned to pre-glitch values within a timescale of a few months. The phase-resolved spectra and pulse profiles after the relaxation are also consistent with those before the glitch. The observed long-term evolution of the spin-down rate and the gamma-ray flux indicates that the glitch triggered a mode change in the global magnetosphere. We speculate that the glitch changed the local magnetic field structure around the polar cap and/or the inclination angle of the dipole axis, leading to a change in the electric current circulating in the magnetosphere.

79 ASTRONOMY AND ASTROPHYSICS↗
NASA NTRS1985

The magnetic and thermodynamical structure of a coronal hole

A nonpolytropic model of a polar coronal hole of 2-5 solar radii constructed. The main assumptions are: (1) the magnetic structure of the sun can be described by a combination of dipole-like and radial fields; (2) in the magnetically dominated region rho(nu sq/2) much less than B sq/8 pi the influence of the outflow on the magnetic structure is negligible. The magnetic and thermodynamic structures are obtained by solving the force balance equation for plasma with the observationally derived electron density. Profiles of velocities in the acceleration regime are presented and the influence of the outflow on the thermodynamic structure of the solar corona above the polar region is discussed.

Osherovich, V. A.↗
DOE OSTI2018

Magnetorotational Mechanism of the Explosion of Core-Collapse Supernovae

The idea of the magnetorotational explosion mechanism is that the energy of rotation of the neutron star formed in the course of a collapse is transformed into the energy of an expanding shock wave by means of a magnetic field. In the two-dimensional case, the time of this transformation depends weakly on the initial strength of the poloidal magnetic field because of the development of a magnetorotational instability. Differential rotation leads to the twisting and growth of the toroidal magnetic-field component, which becomes much stronger than the poloidal component. As a result, the development of the instability and an exponential growth of all field components occur. The explosion topology depends on the structure of the magnetic field. In the case where the initial configuration of the magnetic field is close to a dipole configuration, the ejection of matter has a jet character, whereas, in the case of a quadrupole configuration, there arises an equatorial ejection. In either case, the energy release is sufficient for explaining the observed average energy of supernova explosion. Neutrinos are emitted as the collapse and the formation of a rapidly rotating neutron star proceeds. In addition, neutrino radiation arises in the process of magnetorotational explosion owing to additional rotational-energy losses. If the mass of a newborn neutron star exceeds the mass limit for a nonrotating neutron star, then subsequent gradual energy losses may later lead to the formation of a black hole. In that case, the energy carried away by a repeated flash of neutrino radiation increases substantially. In order to explain an interval of 4.5 hours between the two observed neutrino signals from SN 1987A, it is necessary to assume a weakening of the magnetorotional instability and a small initial magnetic field (10{sup 9}−10{sup 10} G) in the newly formed rotating neutron star. The existence of a black hole in the SN 1987A remnant could explain the absence of any visible pointlike source at the center of the explosion.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

Measurement of higher-order multipole amplitudes in ψ ( 3686 ) → γ χ c 1 , 2 with χ c 1 , 2 → γ J / ψ and search for the transition η c ( 2 S ) → γ J / ψ

Using 106 ×10 6 ψ (3686) events collected with the BESIII detector, we measure multipole amplitudes for the decay ψ (3686) → γχ c1,2 → γγ J/ψ beyond the dominant electric-dipole amplitudes. The normalized magnetic-quadrupole (M2) amplitude for ψ (3686) → γχ c1,2 → γγ J/ψ and the normalized electric-octupole amplitudes for ψ ( 3686 ) → γχ c2 , χ c2 → γJ/ψ are determined. The M2 amplitudes for ψ (3686) → γ χ c1 and χ c1,2 → γ J / ψ are found to differ significantly from zero and are consistent with theoretical predictions. We also obtain the ratios of M2 contributions of ψ ( 3686 ) and J /ψ decays to χ c1,2 , b$1\atop{2}$/ b$2\atop{2}$ = 1.35 ± 0.72 and a$1\atop{2}$/a$2\atop{2}$ = 0.617 ± 0.083 , which agree well with theoretical expectations. By considering the multipole contributions of χ c 1 , 2 , we measure the product branching fractions for the cascade decays ψ ( 3686 ) → γχ c0,1,2 → γγJ/ψ and search for the process η c (2S) → γJ/ψ through ψ ( 3686 ) → γη c (2S). The product branching fraction for ψ (3686) → γχ c0 → γγJ/ψ is 3σ larger than published measurements, while those of ψ (3686) → γχ c1,2 → γγJ/ψ are consistent. In conclusion, no significant signal for the decay ψ ( 3686 ) → γη c (2S) → γγJ/ψ is observed, and the upper limit of the product branching fraction at the 90% confidence level is determined.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2020

Compact, Achromatic Non-scaling FFAG Accelerator for HEP, Commercial and Medical Applications (CRADA FRA-2008-0005 Final Report)

Proton and light-ion accelerators have many research and medical applications, but the current state of technology in accelerators severely limits their widespread use: (1) synchrotrons have an intrinsic low duty cycle and become quite large for light ions; and (2) cyclotrons do not have energy variability and require complex superconducting magnets for high energy. A new concept in non-scaling Fixed-Field Alternating-Gradient (FFAGs) has been invented that incorporates both the energy variability of the synchrotron and the high duty cycle of the cyclotron. The concept uses normal-conducting, combined-function magnets that apply only constant (dipole) and linear-gradient (quadrupole) fields to stabilize the accelerator. This project will develop an optimized design for a new non-scaling and cost-effective innovation in FFAG accelerators. The accelerator design will have optics that can stably accelerate protons to 250 MeV (or higher) and carbon ions to =200 MeV, an energy considered ideal for radiation therapy. Phase I will optimize, fully simulate, and demonstrate the feasibility of this accelerator. Commercial Applications and other Benefits as described by the awardee: The fixed-field acceleration concept should eliminate some of the most pronounced technical difficulties, expense, maintenance, and required expertise faced in conventional proton and light-ion accelerators. In addition to the application for high energy physics, these accelerators should have application in cancer treatment, radiopharmaceuticals, and medical isotope production, and materials science.

43 PARTICLE ACCELERATORS↗
NASA NTRS1975

Jupiter revisited - First results from the University of Chicago charged particle experiment on Pioneer 11

The data obtained by Pioneer 11 confirmed results from Pioneer 10 and provided new information for an understanding of the physics of the Jovian magnetosphere. Attention is given to the significance of Pioneer 11 data in relation to two fundamentally different models which have been proposed to account for the variations in the electron flux observed in Jupiter's outer magnetosphere. Proton flux characteristics are considered, taking into account the intensity profiles of energetic particles trapped in the dipole region of Jupiter's magnetic field.

Simpson, J. A.↗
NASA NTRS1976

Magnetospheric whistler ducts observed by ISIS satellites

The latitudinal width of the magnetospheric whistler duct has been estimated by the first and final invariant latitudes of whistler echoes and the conservation of the magnetic flux for the centered dipole field, using 105 whistler echoes in ISIS VLF data received at Kashima, Japan for 1972-1973. The latitudinal distribution of whistler duct occurrence shows a maximum at invariant latitudes of 40-45 degrees near the maximum occurrence latitude of ground whistlers. The radial width of magnetospheric whistler duct in the geomagnetically equatorial plane increases with invariant latitude of the geomagnetic flux tube in which whistlers propagate.

Ondoh, T.↗
NASA NTRS1976

High resolution spectral analyses of the Jovian decametric radiation. I - Burst morphology and drift rates

Morphological analyses of high-resolution spectral recordings of Jovian decametric radiation show a regime of phenomena not seen at lower resolutions. Observed emissions range from narrow-band (50 kHz) simple quasi-periodic bursts to wide-band emissions (extending over a 500-kHz passband) exhibiting complex structural detail. Assuming gyroemission from electrons in a dipole field for which the magnetic moment is 10 Gauss Jupiter-radius-cubed, drift-rate measurements of the bursts indicate that the source size is of the order of 600 km and its location is near 1.3 Jupiter radii at a colatitude of 27.3 deg. The measurements suggest that the emitting electrons belong to a population having a very specific equatorial pitch angle near 3.5 deg. This study concludes that it may be possible to verify gyroemission as the mechanism responsible for the decametric radiation.

Krausche, D. S.↗
NASA NTRS1979

Model magnetosphere of Mercury

A three-dimensional quantitative model of Mercury's magnetosphere based on Mariner 10 data is presented. The model assumes that the Mercury surface magnetic field consists of a dipole, a quadrupole, and an octupole. The dipole moment is determined, noting that the intensity of the quadrupole moment is 45% of the dipole, and that of the octupole moment is 29% of the dipole. The model meets four critical tests: (1) it produces the smallest residuals, (2) it can reproduce the crossing of a tail current sheet by Mariner 10, (3) all planetary field lines are confined inside the model magnetosphere, and (4) the size of the model agrees with the magnetopause crossings observed from Mariner 10. In addition, the plasma characteristics and regions of quiet and disturbed signatures observed from Mariner 10 are discussed.

Whang, Y. C.↗
NASA NTRS1981

The coronal and interplanetary current sheet in early 1976

A comparison of Helios 1 and 2 observations of the interplanetary sector pattern in early 1976 with the maximum brightness curves in the K coronameter data at 1.5 solar radii shows that the latter may be identified with the footprints of the sector boundary surface to an accuracy of about 10 deg. The sector boundary surface probably extended to about 15 deg in the Northern Hemisphere and to about 30 deg in the Southern Hemisphere, with little change between 1.5 solar radii and 1 AU. The surface was warped appreciably from a single titled plane (a dipole configuration) suggesting a significant magnetic quadrupole contribution.

Burlaga, L. F.↗
NASA NTRS1981

Scaling from Jupiter to pulsar and the acceleration of cosmic ray particles by pulsars

The total energy output per second from the 73 known pulsars is estimated. By following the principle of similitude (Rayleigh, 1915), an expression is derived for the energy generated by a rotating magnetized celestial body, and the dipole moment of the body is related linearly with its angular momentum. The scaling constant of the two equations combined is determined, and then checked by comparing the deduced masses of the 73 pulsars with the theoretical limits for neutron stars. By using the scaling constant and deduced pulsar masses, the rates of acceleration of high-energy particles by pulsars, thence the energy output from pulsars, can be estimated. Results show that the Crab pulsar outshines all the others combined.

Fan, Y. C.↗
NASA NTRS1984

Oscillating dynamo magnetic field in the presence of an external nondynamo field - The influence of a solar primordial field

Dynamo magnetic fields are self-excited and, once started, can perpetrate themselves with no outside source of magnetic flux, as long as the necessary fluid motions persist. Such dynamo fields behave completely independently of the field's overall polarity. In the presence of an external field of separate origin this polarity symmetry of the dynamo states is broken; the dynamo states become asymmetric with respect to polarity. In this paper a calculation is performed of the characteristics of a spherical shell dynamo in the presence of a fossil magnetic field penetrating into the dynamo from below. The asymmetric periodic states are found as a function of the strength of underlying fossil field. Applying these results to the sun, there appears to be no evidence of any intense large-scale primordial magnetic flux, having either dipole-like or quadrupole-like symmetry about the sun's equator, penetrating into the convection zone from the sun's radiative core. Indeed, the calculations indicate, even on the basis of the presently crude observations, that any such primordial field must have an intensity smaller than a few gauss.

Boyer, D. W.↗
NASA NTRS1992

Neptune's non-thermal radio emissions - Phenomenology and source locations

During the inbound and the outbound leg of Voyager 2's encounter with Neptune, the Planetary Radio Astronomy (PRA) experiment aboard the spacecraft detected short radio bursts at frequencies within the range of about 500-1300 kHz, and broad-banded smoothly varying emission patterns within the frequency range from about 40-800 kHz. Both emissions can be described in terms of a period of 16.1 hours determining Neptune's rotation period. Furthermore, just near closest approach, a narrow-banded smoothly varying radio component was observed occurring between 600 and 800 kHz. After giving a brief overview about some general characteristics of Neptune's nonthermal radio emission, the source locations of Neptune's emission components are determined, using an offset tilted dipole model for Neptune's magnetic field. Assuming that the emission originates near the electron gyrofrequency a geometrical beaming model is developed in order to fit the observed emission episodes.

Rabl, Gerald K. F.↗