Maximum TNT Equivalence of Naval Propellants

Swisdak, Jr

doi:10.21236/adp004886

Cited by 10 publications

(12 citation statements)

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“…where δ = ̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅ ̅ 1 + 3 cos 2 θ √ . Conversion formulas between dipole and spherical coordinates can be found in Swisdak (2006).…”

Section: Incorporating Focusing In a Diffusive Transport Modelmentioning

confidence: 99%

Particle Scattering in the Presence of Moderate to Strong Adiabatic Focusing

Florinski

2024

JGR Space Physics

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Starting from the Vlasov‐Boltzmann equation, we derive corrections to the quasi linear Fokker‐Planck pitch angle scattering coefficient caused by a non‐uniformity of the background magnetic field. Integration of the perturbed particle distribution function is performed along a modified unperturbed trajectory that takes into account the effects of focusing and mirroring on pitch angle and gyrophase. We calculate the changes to the quasi‐linear scattering rate owing to a variations in the field strength and the gyrophase drift that affects the resonance between particles and magnetic fluctuations. It is shown that the scattering coefficient has an oscillating behavior in pitch angle when the focusing lengthscale is comparable to the correlation length of the turbulence and the particle's Larmor radius. The applicability of analytic results are demonstrated with a simple model of charged particles trapped in a magnetic field of a planet. It is suggested that the pitch angle diffusion coefficient could become negative for the case of very strong focusing.

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“…where δ = ̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅̅ ̅ 1 + 3 cos 2 θ √ . Conversion formulas between dipole and spherical coordinates can be found in Swisdak (2006).…”

Section: Incorporating Focusing In a Diffusive Transport Modelmentioning

confidence: 99%

Particle Scattering in the Presence of Moderate to Strong Adiabatic Focusing

Florinski

2024

JGR Space Physics

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“…They follow magnetic field lines parameterized by footpoint latitude * q = R r sin 2 0 e q and equatorial extension r eq = η. With a suitable inverse transformation (Swisdak 2006) we can then define the magnetic energy ( )…”

Section: Axisymmetric (2d) Models: Extended Current Sheets Versus Cor...mentioning

confidence: 99%

Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions

Mahlmann

Philippov

Mewes

et al. 2023

ApJL

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The origins of the various outbursts of hard X-rays from magnetars (highly magnetized neutron stars) are still unknown. We identify instabilities in relativistic magnetospheres that can explain a range of X-ray flare luminosities. Crustal surface motions can twist the magnetar magnetosphere by shifting the frozen-in footpoints of magnetic field lines in current-carrying flux bundles. Axisymmetric (2D) magnetospheres exhibit strong eruptive dynamics, i.e., catastrophic lateral instabilities triggered by a critical footpoint displacement of ψ crit ≳ π. In contrast, our new three-dimensional (3D) twist models with finite surface extension capture important non-axisymmetric dynamics of twisted force-free flux bundles in dipolar magnetospheres. Besides the well-established global eruption resulting (as in 2D) from lateral instabilities, such 3D structures can develop helical, kink-like dynamics, and dissipate energy locally (confined eruptions). Up to 25% of the induced twist energy is dissipated and available to power X-ray flares in powerful global eruptions, with most of our models showing an energy release in the range of the most common X-ray outbursts, ≲1043 erg. Such events occur when significant energy builds up while deeply buried in the dipole magnetosphere. Less energetic outbursts likely precede powerful flares, due to intermittent instabilities and confined eruptions of a continuously twisting flux tube. Upon reaching a critical state, global eruptions produce the necessary Poynting-flux-dominated outflows required by models prescribing the fast radio burst production in the magnetar wind—for example, via relativistic magnetic reconnection or shocks.

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“…The photon generated at position ‘S’ propagates along direction n B of the local magnetic field for a corotating observer. The component value of vector n B is easily calculated in magnetic polar coordinates (Swisdak 2006): which can be used to calculate the component value of n B in the laboratory frame by combining it with .…”

Section: The γ–B Absorption Of High‐energy Photons In a Pulsar Magnmentioning

confidence: 99%

“…The photon generated at position 'S' propagates along direction nB of the local magnetic field for a co-rotating observer. The component value of vector nB is easily calculated in magnetic polar coordinates (Swisdak 2006)…”

Section: γ-B Absorption Processes With Detailed Geometrymentioning

confidence: 99%

Low bounds for pulsar γ-ray radiation altitudes

Lee

Wang

et al. 2010

Monthly Notices of the Royal Astronomical Society

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The observational determination of radiation locations can constrain pulsar radiation models. The γ -B process in a strong magnetic field is one of the fundamental physical processes contributing to pulsar radiation mechanisms. Photons generated near a pulsar surface with sufficient energy will be absorbed in the magnetosphere. Considering aberrational, rotational and general relativistic effects, we calculate the γ -B optical depth for γ -ray photons, and we use the derived optical depth to determine the lower bounds of the radiation altitude for photons with given energies. As a case study, we obtain the low bounds of radiation altitude for the Crab pulsar for photons with energies of 5 GeV-1 TeV.

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Maximum TNT Equivalence of Naval Propellants

Cited by 10 publications

References 0 publications

Particle Scattering in the Presence of Moderate to Strong Adiabatic Focusing

Particle Scattering in the Presence of Moderate to Strong Adiabatic Focusing

Three-dimensional Dynamics of Strongly Twisted Magnetar Magnetospheres: Kinking Flux Tubes and Global Eruptions

Low bounds for pulsar γ-ray radiation altitudes

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