Implications of a "Fast Radio Burst" from a Galactic Magnetar

A luminous radio burst was recently detected in temporal coincidence with a hard X-ray flare from the Galactic magnetar SGR 1935+2154 with a time and frequency structure consistent with cosmological fast radio bursts (FRB) and a fluence within a factor of $\lesssim 10$ of the least energetic extragalactic FRB previously detected. Although active magnetars are commonly invoked FRB sources, several distinct mechanisms have been proposed for generating the radio emission which make different predictions for the accompanying higher frequency radiation. We show that the properties of the coincident radio and X-ray flares from SGR 1935+2154, including their approximate simultaneity and relative fluence $E_{\rm radio}/E_{\rm X} \sim 10^{-5}$, as well as the duration and spectrum of the X-ray emission, are consistent with extant predictions for the synchrotron maser shock model. Rather than arising from the inner magnetosphere, the X-rays are generated by (incoherent) synchrotron radiation from thermal electrons heated at the same shocks which produce the coherent maser emission. Although the rate of SGR 1935+2154-like bursts in the local universe is not sufficient to contribute appreciably to the extragalactic FRB rate, the inclusion of an additional population of more active magnetars with stronger magnetic fields than the Galactic population can explain both the FRB rate as well as the repeating fraction, however only if the population of active magnetars are born at a rate that is at least two-orders of magnitude lower than that of SGR 1935+2154-like magnetars. This may imply that the more active magnetar sources are not younger magnetars formed in a similar way to the Milky Way population (e.g. via ordinary supernovae), but instead through more exotic channels such as superluminous supernovae, accretion-induced collapse or neutron star mergers.Comment: 21 pages, 9 figures; submitted to ApJL; comments welcome

Separation of Benzene and n-Hexane Using a Liquid Membrane Technique

The separation of a mixture of benzene and n-hexane was studied using a liquid membrane technique. Sparkleen^ detergent was used as the surfactant and heavy mineral oil was used as the solvent to receive the permeate. The effects of the following variables on the separation factor were investigated: 1. The relative proportion of benzene and n-hexane in the original mixture. 2 . Surfactant concentration. 3 . Quantity of surfactant solution. 4. Amount of solvent. 5 . Contact time with solvent. The effect of each variable was studied by varying the values of that variable while holding other variables constant. It was found that both the separation factor and the permeate composition vary with the feed composition. Under the experimental conditions employed in the present study, the average value of the separation factor for 0.1 to 0.9 mole fraction of benzene in the feed was found to be approximately 6. Under the experimental conditions employed in the present study, the separation factor was found to be low for the volumes of solvent less than 180 c.c. The separation factor was found to be about constant for the volumes of solvent between 180 and 250 c.c. Beyond 250 c.c. , the separation factor was again found to be low. For low values of concentration of surfactant and contact times with solvent, the separation factor was found to be low. As the values of these variables were increased the separation factor increased and reached a maximum and for large values of these variables, the separation factor again decreased. From the study of the variation of separation factor with the quantity of surfactant solution, it was found that the separation factor was independent of the quantity of surfactant solution beyond a certain volume of surfactant solution. For volumes less than this minimum, the separation factor was lower, but increased as the volume increased. A rough estimate of the theoretical and experimental error involved in the present study has been made. The relative advantages and disadvantages of the separation by liquid membrane were also discussed

Switched Control of Electron Nuclear Spin Systems

In this article, we study control of electron-nuclear spin dynamics at magnetic field strengths where the Larmor frequency of the nucleus is comparable to the hyperfine coupling strength. The quantization axis for the nuclear spin differs from the static B_0 field direction and depends on the state of the electron spin. The quantization axis can be switched by flipping the state of electron spin, allowing for universal control on nuclear spin states. We show that by performing a sequence of flips (each followed by a suitable delay), we can perform any desired rotation on the nuclear spins, which can also be conditioned on the state of the electron spin. These operations, combined with electron spin rotations can be used to synthesize any unitary transformation on the coupled electron-nuclear spin system. We discuss how these methods can be used for design of experiments for transfer of polarization from the electron to the nuclear spins

Radio Nebul\ae\ from Hyper-Accreting X-ray Binaries as Common Envelope Precursors and Persistent Counterparts of Fast Radio Bursts

Roche lobe overflow from a donor star onto a black hole or neutron star binary companion can evolve to a phase of unstable runaway mass-transfer, lasting as short as hundreds of orbits ($\lesssim 10^{2}$ yr for a giant donor), and eventually culminating in a common envelope event. The highly super-Eddington accretion rates achieved during this brief phase ($\dot{M} \gtrsim 10^{5}\dot{M}_{\rm Edd})$ are accompanied by intense mass-loss in disk winds, analogous but even more extreme than ultra-luminous X-ray (ULX) sources in the nearby universe. Also in analogy with observed ULX, this expanding outflow will inflate an energetic `bubble' of plasma into the circumbinary medium. Embedded within this bubble is a nebula of relativistic electrons heated at the termination shock of the faster $v \gtrsim 0.1 c$ wind/jet from the inner accretion flow. We present a time-dependent, one-zone model for the synchrotron radio emission and other observable properties of such ULX `hyper-nebulae'. If ULX jets are sources of repeating fast radio bursts (FRB), as recently proposed, such hyper-nebulae could generate persistent radio emission and contribute large and time-variable rotation measure to the bursts, consistent with those seen from FRB 20121102 and FRB 190520B. ULX hyper-nebulae can be discovered independent of an FRB association in radio surveys such as VLASS, as off-nuclear point-sources whose fluxes can evolve significantly on timescales as short as years, possibly presaging energetic transients from common envelope mergers.Comment: 27 pages, 9 figures, 1 table; accepted for publication in Ap

Quantitative analysis of pedestrian counterflow in a cellular automaton model

Pedestrian dynamics exhibits various collective phenomena. Here we study bidirectional pedestrian flow in a floor field cellular automaton model. Under certain conditions, lane formation is observed. Although it has often been studied qualitatively, e.g., as a test for the realism of a model, there are almost no quantitative results, neither empirically nor theoretically. As basis for a quantitative analysis we introduce an order parameter which is adopted from the analysis of colloidal suspensions. This allows to determine a phase diagram for the system where four different states (free flow, disorder, lanes, gridlock) can be distinguished. Although the number of lanes formed is fluctuating, lanes are characterized by a typical density. It is found that the basic floor field model overestimates the tendency towards a gridlock compared to experimental bounds. Therefore an anticipation mechanism is introduced which reduces the jamming probability.Comment: 11 pages, 12 figures, accepted for publication in Phys. Rev.