Emanuele Cazzola

On the electron dynamics during island coalescence in asymmetric magnetic reconnection

We present an analysis of the electron dynamics during rapid island merging in asymmetric magnetic reconnection. We consider a doubly periodic system with two asymmetric transitions. The upper layer is an asymmetric Harris sheet of finite width perturbed initially to promote a single reconnection site. The lower layer is a tangential discontinuity that promotes the formation of many X-points, separated by rapidly merging islands. Across both layers, the magnetic field and the density have a strong jump, but the pressure is held constant. Our analysis focuses on the consequences of electron energization during island coalescence. We focus first on the parallel and perpendicular components of the electron temperature to establish the presence of possible anisotropies and non-gyrotropies. Thanks to the direct comparison between the two different layers simulated, we can distinguish three main types of behavior characteristic of three different regions of interest. The first type represents the regions where traditional asymmetric reconnections take place without involving island merging. The second type of regions instead shows reconnection events between two merging islands. Finally, the third regions identify the regions between two diverging island and where typical signature of reconnection is not observed. Electrons in these latter regions additionally show a flat-top distribution resulting from the saturation of a two-stream instability generated by the two interacting electron beams from the two nearest reconnection points. Finally, the analysis of agyrotropy shows the presence of a distinct double structure laying all over the lower side facing the higher magnetic field region. This structure becomes quadrupolar in the proximity of the regions of the third type. The distinguishing features found for the three types of regions investigated provide clear indicators to the recently launched Magnetospheric Multiscale NASA mission for investigating magnetopause reconnection involving multiple islands.

MAGNETIC NULL POINTS IN KINETIC SIMULATIONS OF SPACE PLASMAS

We present a systematic attempt to study magnetic null points and the associated magnetic energy conversion in kinetic Particle-in-Cell simulations of various plasma configurations. We address three-dimensional simulations performed with the semi-implicit kinetic electromagnetic code iPic3D in different setups: variations of a Harris current sheet, dipolar and quadrupolar magnetospheres interacting with the solar wind; and a relaxing turbulent configuration with multiple null points. Spiral nulls are more likely created in space plasmas: in all our simulations except lunar magnetic anomaly and quadrupolar mini-magnetosphere the number of spiral nulls prevails over the number of radial nulls by a factor of 3-9. We show that often magnetic nulls do not indicate the regions of intensive energy dissipation. Energy dissipation events caused by topological bifurcations at radial nulls are rather rare and short-lived. The so-called X-lines formed by the radial nulls in the Harris current sheet and lunar magnetic anomaly simulations are rather stable and do not exhibit any energy dissipation. Energy dissipation is more powerful in the vicinity of spiral nulls enclosed by magnetic flux ropes with strong currents at their axes (their cross-sections resemble 2D magnetic islands). These null lines reminiscent of Z-pinches efficiently dissipate magnetic energy due to secondary instabilities such as the two-stream or kinking instability, accompanied by changes in magnetic topology. Current enhancements accompanied by spiral nulls may signal magnetic energy conversion sites in the observational data.

On the Electron Agyrotropy during Rapid Asymmetric Magnetic Island Coalescence in Presence of a Guide Field

We present an analysis of the properties of the electron velocity distribution during island coalescence in asymmetric reconnection with and without guide field. In a previous study, three main domains were identified, in the case without guide field, as X, D, and M regions featuring different reconnection evolutions. These regions are also identified here in the case with guide field. We study the departure from isotropic and gyrotropic behavior by means of different robust detection algorithms proposed in the literature. While in the case without guide field these metrics show an overall agreement, when the guide field is present, a discrepancy in the agyrotropy within some relevant regions is observed, such as at the separatrices and inside magnetic islands. Moreover, in light of the new observations from the Multiscale MagnetoSpheric mission, an analysis of the electron velocity phase-space in these domains is presented.

Reconnection Separatrix: Simulations and Spacecraft Measurements

In this chapter, we review the progress in understanding the processes near the separatrices during magnetic reconnection. The results are obtained from numerical simulation and spacecraft measurement. The reconnection separatrices represent the surface (cross curve in two-dimensional regime) separating the reconnected magnetic field lines from the reconnecting lines, and thereby connect to the reconnection X-line. The average properties of the particle distribution and physical processes in the separatrix region are summarized. Recent studies confirm that various instabilities occur in the separatrix region and lead to a complex interplay and affecting the plasma in this region. The microphysics in the separatrix region should play an important role in reconnection dynamics. Furthermore, electrons are accelerated up to 100 keV before they enter into the electron diffusion region: a significant part of energy conversion takes place in the separatrix region during reconnection.

On magnetic reconnection as promising driver for future plasma propulsion systems

This work presents a more detailed analysis of the process of magnetic reconnection as a promising ion beam accelerator mechanism with possible applications in laboratory plasmas and, more importantly, in the plasma propulsion field. In a previous work, an introductory study on this subject was already carried out, yet under the adoption of relevant approximations, such as the limitation to 2.5D simulations and especially the use of hydrogen plasma as a propellant, whose element is rarely considered in the real scenario. Also, the analysis mainly focussed on studying the physical content of the outcomes, by leaving out the analysis of more important engineering quantities, such as the mass flow and thrust effectively reached out of such systems. In this work, we intend to fill these gaps in order to provide further insights into the great potentiality of a future technology based on magnetic reconnection. Additionally, one of the possibly limiting features was the inevitable symmetric outflow produced by the reconnection process. Among all the possible adoptable solutions, we propose here a solution based on the particle behavior undertaken for entering the reconnection region according to the initial density profile. We demonstrate that a noticeable net thrust value can be achieved by setting up a longitudinal asymmetric density profile with a relevant drop gradient.This work presents a more detailed analysis of the process of magnetic reconnection as a promising ion beam accelerator mechanism with possible applications in laboratory plasmas and, more importantly, in the plasma propulsion field. In a previous work, an introductory study on this subject was already carried out, yet under the adoption of relevant approximations, such as the limitation to 2.5D simulations and especially the use of hydrogen plasma as a propellant, whose element is rarely considered in the real scenario. Also, the analysis mainly focussed on studying the physical content of the outcomes, by leaving out the analysis of more important engineering quantities, such as the mass flow and thrust effectively reached out of such systems. In this work, we intend to fill these gaps in order to provide further insights into the great potentiality of a future technology based on magnetic reconnection. Additionally, one of the possibly limiting features was the inevitable symmetric outflow produced by ...

Web-based description of the space radiation environment using the bethe–bloch model

Space weather is a rapidly growing area not only in scientific and engineering applications but also in physics education and in the interest of the public. We focus especially on space radiation and its impact on space exploration. The topic is highly interdisciplinary bringing together fundamental concepts of nuclear physics with aspects of radiation protection and space science. We present a new approach to presenting the topic by developing a web-based tool that combines some of the fundamental concepts from these two fields in a single tool that can be developed in the context of advanced secondary or undergraduate university education. We present DREADCode, an outreach or teaching tool to asses rapidly the current conditions of the radiation field in space. DREADCode uses the available data feeds from a number of ongoing space missions to produce a first order approximation of the dose an astronaut would receive during a mission of exploration in deep space. DREADcode is based on a intuitive GUI interface available online from the European Space Weather Portal. The core of the radiation transport computation to produce the radiation dose from the observed fluence of radiation observed by the spacecraft fleet considered is based on a relatively simple approximation: the Bethe-Block equation. DREADCode assumes also a simplified geometry and material configuration for the shields used to compute the dose. The approach is approximate and it sacrifices some important physics on the altar of a rapid execution time allowing a real time operation scenario. There is no intention here to produce an operational tool for use in the space science and engineering. Rather we present an educational tool at undergraduate level that uses modern web-based and programming methods to learn some of the most important concepts in the application of radiation protection to space weather problems.