Who Builds the Motherland?

I was born in 2002 into a middle-class Jewish family, in a very Jewish town. The town was our Zion, our Mini-Israel, our bubble. It prided itself on being a sleepy town where any American can feel safe and comfortable. At the best of times, the town felt like a family; everyone knew your name and many children born in the town decided to live the rest of their adult lives there. It was a place where the support of Israel was of utmost importance. Although everyone prided themselves on the security, there was always this unease that our human rights could be taken away by those others that outnumbered us. After all, it only took two years from Hitler\u27s rise to power to his passing of the Nuremberg laws. With this fear of history repeating itself, every Jew in the bubble, whether they be Reform or Orthodox, Ashkenazi or Sephardic, talked of the grandeur of the Israeli state. Because no matter how slim the odds may seem that the worst-case scenario could happen, any chance that it could happen again was unacceptable for the descendants of the victims of the Holocaust. [excerpt

Origin of spontaneous violation of the Lorentz symmetry: Vortices in the cosmos

By carefully studying the (1,0)+(0,1) representation space for massive particles we point to the existence of certain inherent tachyonic dispersion relations: E^2= p^2-m^2. We put forward an interpretation that exploits these ``negative mass squared'' solutions; rotational invariance is spontaneously broken. Relevance of these results to the vortices in the cosmos is pointed out. NOTE: Just as "negative energy solutions'' of Dirac equation are re-interpreted as antiparticles, similarly the possibility exists for re-interpreting the tachyonic dispersion relations of all (j,0)+(0,j) representation spaces via spontaneous Lorentz symmetry breaking. In Mod. Phys. Lett. A8:2623-2630,1993 we exhibited this explicitly for the j=1 representation space. The interest in this old subject has grown markedly in recent years as is evident from numerous theoretical and phenomenological works on the subject. With this observation, we make this replacement of our paper fourteen years after its initial publication. The Abstract and main text remain unaltered. The title is changed to reflect the underlying physics more closely.Comment: This is an exact copy of the published paper with an extended bibliography and a revised title. A brief note is added to point out a systematic way to spontaneously break Lorentz symmetr

The planetary nebula IC 5148 and its ionized halo

Many round or nearly roundish Planetary Nebulae (PNe) show multiple shells and halo structures during their evolutionary stage near the maximum temperature of their central star. Controversial debate is currently ongoing if these structures are recombination halos, as suggested by hydrodynamic modelling efforts, or ionized material. Recently we discovered a halo with even somewhat unusual structures around the sparsely studied PN IC~5148 and present for the first time spectroscopy going out to the halo of such a PN.} resolution spectroscopy is used to derive dust chemistry and mineralogy. We investigate the spatial distribution of material and its ionization state from the center of the nebula up to the very outskirts of the halo. We obtained long-slit low resolution spectroscopy (FORS2@VLT) of the nebula in two position angles, which we used to investigate the nebular structure and its halo in the optical range from 450 to 880\,nm. In addition we used medium resolution spectra taken with X-SHOOTER@VLT ranging from 320 nm to 2.4 mu to derive atmospheric parameters for the central star. We obtained the distance and position in the Galaxy from various methods combined with GAIA DR2 data. We also applied Cloudy models to the nebula in order to derive physical parameters of the various regions. We obtained spatially resolved structures and detailed descriptions of the outrunning shock front and a set of unusual halo structures denoted to further shock. The halo structures appears clearly as hot ionized material. Furthermore we derived a reliable photometric value for the central star at a GAIA distance of D=1.3kpc. Considering the large distance $z=1.0$\,kpc from the galactic plane together to its non-circular motion in the galaxy and, a metallicity only slightly below that of typical disk PNe, most likely IC 5148 originates from a thick disk population star.Comment: 12 pages, 17 figures, accepted for publication in Astronomy & Astrophysic

Where should MMS look for electron diffusion regions?

A great possible achievement for the MMS mission would be crossing electron diffusion regions (EDR). EDR are regions in proximity of reconnection sites where electrons decouple from field lines, breaking the frozen in condition. Decades of research on reconnection have produced a widely shared map of where EDRs are. We expect reconnection to take place around a so called x-point formed by the intersection of the separatrices dividing inflowing from outflowing plasma. The EDR forms around this x-point as a small electron scale box nested inside a larger ion diffusion region. But this point of view is based on a 2D mentality. We have recently proposed that once the problem is considered in full 3D, secondary reconnection events can form [Lapenta et al., Nature Physics, 11, 690, 2015] in the outflow regions even far downstream from the primary reconnection site. We revisit here this new idea confirming that even using additional indicators of reconnection and even considering longer periods and wider distances the conclusion remains true: secondary reconnection sites form downstream of a reconnection outflow causing a sort of chain reaction of cascading reconnection sites. If we are right, MMS will have an interesting journey even when not crossing necessarily the primary site. The chances are greatly increased that even if missing a primary site during an orbit, MMS could stumble instead on one of these secondary sites.Comment: submitted to the Astronum 2015 Conference Proceeding

Solar radio emission

Active areas of both observational and theoretical research in which rapid progress is being made are discussed. These include: (1) the dynamic spectrum or frequency versus time plot; (2) physical mechanisms in the development of various types of bursts; (3) microwave type 1, 2, 3, and moving type 4 bursts; (4) bursts caused by trapped electrons; (5) physics of type 3bursts; (6) the physics of type 2 bursts and their related shocks; (7) the physics of both stationary and moving traps and associated type 1 and moving type 4 bursts; and (8) the status of the field of solar radio emission

Kodaira-Spencer formality of products of complex manifolds

We shall say that a complex manifold $X$ is emph{Kodaira-Spencer formal} if its Kodaira-Spencer differential graded Lie algebra $A^{0,*}_X(Theta_X)$ is formal; if this happen, then the deformation theory of $X$ is completely determined by the graded Lie algebra $H^*(X,Theta_X)$ and the base space of the semiuniversal deformation is a quadratic singularity.. Determine when a complex manifold is Kodaira-Spencer formal is generally difficult and we actually know only a limited class of cases where this happen. Among such examples we have Riemann surfaces, projective spaces, holomorphic Poisson manifolds with surjective anchor map $H^*(X,Omega^1_X) o H^*(X,Theta_X)$ and every compact K"{a}hler manifold with trivial or torsion canonical bundle. In this short note we investigate the behavior of this property under finite products. Let $X,Y$ be compact complex manifolds; we prove that whenever $X$ and $Y$ are K"{a}hler, then $X imes Y$ is Kodaira-Spencer formal if and only if the same holds for $X$ and $Y$. A revisit of a classical example by Douady shows that the above result fails if the K"{a}hler assumption is droppe

Characterizing the Hofstadter butterfly's outline with Chern numbers

In this work, we report original properties inherent to independent particles subjected to a magnetic field by emphasizing the existence of regular structures in the energy spectrum's outline. We show that this fractal curve, the well-known Hofstadter butterfly's outline, is associated to a specific sequence of Chern numbers that correspond to the quantized transverse conductivity. Indeed the topological invariant that characterizes the fundamental energy band depicts successive stairways as the magnetic flux varies. Moreover each stairway is shown to be labeled by another Chern number which measures the charge transported under displacement of the periodic potential. We put forward the universal character of these properties by comparing the results obtained for the square and the honeycomb geometries.Comment: Accepted for publication in J. Phys. B (Jan 2009

Gas bubble dynamics in soft materials

Epstein and Plesset's seminal work on the rate of gas bubble dissolution and growth in a simple liquid is generalized to render it applicable to a gas bubble embedded in a soft elastic medium. Both the underlying diffusion equation and the expression for the gas bubble pressure were modified to allow for the non-zero shear modulus of the elastic medium. The extension of the diffusion equation results in a trivial shift (by an additive constant) in the value of the diffusion coefficient, and does not change the form of the rate equations. But the use of a Generalized Young-Laplace equation for the bubble pressure resulted in significant differences on the dynamics of bubble dissolution and growth, relative to a simple liquid medium. Depending on whether the salient parameters (solute concentration, initial bubble radius, surface tension, and shear modulus) lead to bubble growth or dissolution, the effect of allowing for a non-zero shear modulus in the Generalized Young-Laplace equation is to speed up the rate of bubble growth, or to reduce the rate of bubble dissolution, respectively. The relation to previous work on visco-elastic materials is discussed, as is the connection of this work to the problem of Decompression Sickness (specifically, "the bends"). Examples of tissues to which our expressions can be applied are provided. Also, a new phenomenon is predicted whereby, for some parameter values, a bubble can be metastable and persist for long times, or it may grow, when embedded in a homogeneous under-saturated soft elastic medium.Comment: 18 pages, 4 figures, 1 table, (Included also "Supplementary information": 2 pages, 1 table

Quenching of the beam-plasma instability by 3-D spectra of large scale density fluctuations

A model is presented to explain the highly variable yet low level of Langmuir waves measured in situ by spacecraft when electron beams associated with Type III solar bursts are passing by; the low level of excited waves allows the propagation of such streams from the Sun to well past 1 AU without catastrophic energy losses. The model is based, first, on the existence of large scale density fluctuations that are able to efficiently diffuse small k beam unstable Langmuir waves in phase space, and, second, on the presence of a significantly isotropic nonthermal tail in the distribution function of the background electron population, which is capable of stabilizing larger k modes. The strength of the model lies in its ability to predict various levels of Langmuir waves depending on the parameters. This feature is consistent with the high variability actually observed in the measurements