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Laurence J. November

Publications and source records attributed to Laurence J. November.

3 recordsLinked to original sources

Zero-Point Forces in Acoustic Waves

By the acousto-optic effect, an acoustic plane wave produces a 1D index-of-refraction or permittivity wave variation through a medium. But adjacent material planes of alternating permittivity should interact due to the zero-point (ZP) field to produce internal forces, roughly like the Casimir effect in a stack of regularly spaced discrete conducting plates. The ZP force in a smoothly varying 1D permittivity wave is modeled and found to consist mainly of bulk repulsive and double-wavenumber harmonics. It is stronger than the Casimir ZP attractive force in the corresponding discrete alternating-layer stack at all physically meaningful repetition scales, extends to larger scales, falling off universally only as the inverse square of the wavelength, and shows no temperature sensitivity. Thus, at its extremes, a standing acoustic wave exhibits a bulk expansive ZP pressure through the material volume, but as it passes through its null the ZP pressure vanishes, giving a body stress modulated at twice the acoustic wave frequency. But such repeated tensing in a piezo material is a usual energy-harvesting scenario, suggesting that ZP energy transfer may occur naturally with standing acoustic waves in a piezo medium. A voltage effect is predicted for biphonon lattice vibrations in piezo crystals with the possibility of 'crystal power', the extraction of electrical ZP energy across the crystal volume.

physics.gen-ph↗

The Astrophysical Corona as the Minimum Atmosphere Surrounding Embedded Non-Force-Free Flux Tubes

The equilibrium of current-carrying magnetic fields (e.g. flux tubes) embedded in a large-scale background field is developed and discussed in the astrophysical context. Embedded non-force-free current-carrying fields require a minimum surrounding atmosphere, which by direct pressure balance has a gas pressure everywhere proportional to the background magnetic pressure. Formally, the MHD equations, with flows and gravity as part of a wide class of physical processes, separate into independent local and global relations representing an equilibrium solution for embedded current-carrying fields. The local pressure relation for the embedded field is a 3D Grad-Shafranov equation with finite-sheath solutions. The global relation reproduces the ambient MHD pressure equation without the embedded fields, but instead with the constraint that the ambient gas and magnetic pressures vary in proportion, as with the direct pressure balance. A coupled gas pressure in magnetically dominant regimes necessitates refilling outflows in a depleted atmosphere (actualized by flux-tube Lorentz forces) providing a compressively heated equilibrium corona with a specific global distribution of density, temperature, and steady accelerated outflow, all defined by the large-scale background magnetic field. Magnetic footpoint compression and twisting in a high-gas-pressure field-forming region (e.g. convection zone) outside, as below, the magnetically dominant regime, can introduce and sustain non-force-free embedded fields, thereby providing the energy for the coronal atmosphere. Such coronae may be relevant on very different astrophysical scales: around the sun and stars, and ranging from planets, to neutron stars, black holes, and spiral galaxies. Predicted coronal temperatures are corroborated.

astro-ph.SR↗

Magnetohydrostatic atmospheres

We show that the atmospheric and magnetic height variations are coupled in general MHS equilibria with gravity when isolated thin non-force-free flux tubes are present. In gas-dominated environments, as in stellar photospheres, flux tubes must expand rapidly with height to maintain pressure balance with the cool surroundings. But in magnetically dominated environments, as in stellar coronae, the large-scale background magnetic field determines the average spreading of embedded flux tubes, and rigidly held flux tubes {\it require} a specific surrounding atmosphere with a unique temperature profile for equilibrium. The solar static equilibrium atmosphere exhibits correct transition-region properties and the accepted base coronal temperature for the sun's main magnetic spherical harmonic. Steady flows contribute to the overall pressure, so equilibria with accelerated wind outflows are possible as well. Flux tubes reflect a mathematical degeneracy in the form of non-force-free fields, which leads to coupling in general equilibrium conditions. The equilibrium state characterizes the system average in usual circumstances and dynamics tend to maintain the MHS atmosphere. Outflows are produced everywhere external to rigidly held flux tubes that refill a depleted or cool atmosphere to the equilibrium gas profile, heating the gas compressively.

astro-ph↗