Session T1: Poster Session III (14:00 - 17:00)

Periodicity of Mrk 501 in Optical Wavelengths

We present data for Mrk501 from 2009-2016 taken by ROVOR and WMO in Johnson B, V, and R filters. An aperture of radius 5" was used for all data. Photometry was referenced to the same ensemble of stars in all frames. We find strong evidence for a regular light curve matching a sine wave of amplitude around $1 \times 10^{-15} (erg \; s^{-1}cm^{-2}{\AA}^{-1})$ in B, $0.6\times10^{-15}(erg \; s^{-1}cm^{-2}{\AA}^{-1})$ in V, and $0.5\times10^{-15}(erg\; s^{-1}cm^{-2}{\AA}^{-1})$ in R, and with a period of $\sim2000\pm200$ days. Additionally, a linear combination of sine waves having periods of $\sim113\pm3$ days and $\sim70\pm5$ days also show a strong presence in the light curve, both with amplitudes of around $0.25\pm0.03\times10^{-15}(erg\; s^{-1}cm^{-2}{\AA}^{-1})$ in V. These results are consistent with X-ray data and are qualitatively similar to the light curve found for NGC5548 (Bon et al, 2016). We lend these results as potentially bearing further evidence for the presence of a binary super-massive balck hole in Mrk 501.   

Jupiter's X-ray aurora via polar ion precipitation

Jupiter's auroral X-ray emission was first observed by the Einstein X-ray Observatory in 1979 and has since been observed over the past 20 years by the Roentgen satellite, Chandra X-ray Observatory, and XMM-Newton. The strong X-ray emission produces a spectacular 1 GW of total power at the polar caps. There has been extensive research of X-ray production from incident electrons; however, this has not been able to account for the full power of the generated X-rays. The remainder of the X-ray production can be modeled and reproduced into observable results by the precipitation of several MeV oxygen and sulfur ions from the outer magnetosphere into an atmosphere that has been adapted to the auroral conditions. The present research uses a revised model of a hybrid Monte Carlo method with varying oxygen ion energies (10 keV/u -- 5 MeV/u) and updated collision cross-sections to concentrate on the ionization of the atmosphere, generation of secondary electron fluxes and their escape from the atmosphere, and characterization of the H2 Lyman-Werner band emission. Predictions relevant to awaited NASA's Juno results are made: escaping electrons with an energy range of 1 eV to 6 keV, H2 band emission rates of 80 kR, and downward field-aligned currents of at least 2 MA.   

Effect of Inhomogeneous Flow on K-H Turbulence

We study the effect of inhomogeneous flow on the Kelvin-Helmholz instability and turbulence. The inhomogeneous flow includes both flow shear and flow curvature. The effect of flow curvature (second radial derivative of flow) is shown to have significant effect in controlling the turbulence level contrary to the usual prediction that flow shear (first radial derivative of flow) alone controls the turbulence level. The detail result of this simulation will be reported.   

Measuring Ejecta from Inspiralling Binary Neutron Stars using Smoothed-particle Hydrodynamics

Gravitational waves, detectable perturbations in spacetime, can arise from astrophysical systems such as inspiralling binary neutron stars, the remnants of the core collapse of massive stars. In the inspiral process, neutron stars, composed of highly dense nuclear matter, are torn apart by each others gravity and eject matter. Using both gravitational waves and direct observations of ejected matter, we may gain valuable new information about the composition of neutron stars. Using several previously studied test cases, we seek to determine how the amount of ejected matter depends on the physical parameters of these systems. To do this, we use a particle-based hydrodynamics code which can accurately simulate binary neutron star systems with variable equation of state, spin, mass ratio, and eccentricity, and includes the lowest-order effects from gravitational wave emission.   

The Janus Cosmological Model (JCM) : An answer to the missing cosmological antimatter

Cosmological antimatter absence remains unexplained. Twin universes 1967 Sakarov's model suggests an answer: excess of matter and anti-quarks production in our universe is balanced by equivalent excess of antimatter and quark in twin universe. JCM$^{\mathrm{[1]}}$ provides geometrical framework, with a single manifold , two metrics solutions of two coupled field equations, to describe two populations of particles, one with positive energy-mass and the other with negative energy-mass : the `twin matter'. In a quantum point of view, it's a copy of the standard matter but with negative mass and energy. The matter-antimatter duality holds in both sectors. The standard and twin matters do not interact except through the gravitational coupling expressed in field equations. The twin matter is unobservable from matter-made apparatus. Field equations shows that matter and twin matter repel each other. Twin matter surrounding galaxies explains their confinement (dark matter role) and, in the dust universe era, mainly drives the process of expansion of the positive sector, responsible of the observed acceleration (dark energy role). [1]Negative mass hypothesis and the nature of dark energy Mod. Phys. Lett.$ A$ \textbf{29}, 1450182 (2014)   

Quantum Tunneling and the Energy of the Vacuum.

We describe a dynamical mechanism by which a cosmological scalar field in a Higgs-type potential naturally acquires an exponentially small energy density in Planck units. It is assumed that the energy density of the scalar field vanishes in its lowest (symmetric) state, but that the field is presently hung up in the first antisymmetric state. A net energy density of 10$^{\mathrm{-122\thinspace }}$times the Planck density is easily obtained in the simplest two-parameter model with both free parameters of order unity. We discuss the obstacles that lie in the way of exploiting such a mechanism as an explanation for the observed density of dark energy in the universe.   

Dark matter scattering on electrons: Accurate calculations of atomic excitations and implications for the DAMA and XENON experiments

Atoms can become ionised during the scattering of a slow, heavy particle off a bound electron. Such an interaction involving leptophilic WIMP dark matter is a potential explanation for the anomalous 9 sigma annual modulation in the DAMA direct detection experiment. We show that due to non-analytic, cusp-like behavior of Coulomb functions close to the nucleus leads to an effective atomic structure enhancement. Crucially, we also show that electron relativistic effects are important. With this in mind, we perform high-accuracy relativistic calculations of atomic ionisation. We scan the parameter space: the DM mass, the mediator mass, and the effective coupling strength, to determine if there is any region that could potentially explain the DAMA signal. While we find that the modulation fraction of all events with energy deposition above 2 keV in NaI can be quite significant, reaching \textasciitilde 50{\%}, the relevant parts of the parameter space are excluded by the XENON10 and XENON100 experiments. B. M. Roberts, V. V. Flambaum, and G. F. Gribakin, Phys. Rev. Lett. 116, 023201 (2016). B. M. Roberts, V. A. Dzuba, V. V. Flambaum, M. Pospelov, and Y. V. Stadnik, Phys. Rev. D 93 115037 (2016).   

Exploring the MSSM Neutralino Parameter Space using DarkSUSY

Historically, one of the most promising dark matter candidates has been the Neutralino from the Minimal Supersymmetric Standard Model (MSSM). Although Supersymmetry has not been experimentally confirmed, it has been tightly constrained by both accelerator limits and astrophysical bounds. DarkSUSY is a computer code that is based on the MSSM, and which allows for the calculation of Neutralino densities, cross sections, and expected detection rates in both direct and indirect detection experiments. In this work we use DarkSUSY, together with the latest accelerator constraints and astrophysical bounds, to explore parameter space. Beginning with 700,000+ randomly generated models we explore if the MSSM has been experimentally ruled out. Surviving models and interesting regions of surviving parameter space will be presented and discussed.   

Can cold neutrons give hint to understanding nature of dark matter?

The composition of Dark Matter remains a mystery despite numerous searches. We explore an alternative to the WIMP paradigm in which Ordinary Matter and Dark Matter ``Mirror'' sectors are made of the same particles with the Standard Model interactions in each sector, except two sectors do not interact with each other by the Standard Model interactions. They only interact gravitationally and by some BSM mechanisms that can mix neutral components from both sectors. Thus, for example, photons can mix with sterile mirror photons via ``kinetic mixing'' mechanism, neutrinos can oscillate into sterile mirror neutrinos, and neutrons into sterile mirror neutrons. I explore the possibility to search for this Dark ``Mirror'' Sector by looking at mixing between neutron and mirror neutron. This can be done in a cold neutron beam where neutrons can oscillate into mirror neutrons and pass through a neutron absorber and then transform back into ordinary neutrons where they are detected. The regeneration of neutron depends on the magnitude and direction of a magnetic field.   

Putting BayesWave to the Test: Can BayesWave Detect Eccentric Black-Hole Binary Sources?

The mission of the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO) is to detect gravitational waves that are caused by the interaction of massive gravitating bodies such as coalescing black holes and neutron stars. Due to the detection of gravitational waves in the past year, we want to take it a step further and detect gravitational waves from eccentric black hole binary (eBBH) sources. Therefore, we propose BayesWave as the main algorithm for detecting and analyzing eBBH sources. We will explore the efficacy of using BayesWave to detect eBBH sources and discuss future modifications to BayesWave to improve these searches.   

Rapid Realization of the Stochastic Gravitational Wave Signal due to Galactic Mergers

Mergers of massive galaxies often result in a merger between their central supermassive black holes. These merging binaries will generate gravitational waves, all of which add up to create a stochastic gravitational-wave background in the nanohertz range. Full realization of this signal requires generation of a large population of binaries (N$=$10$^{\mathrm{11}})$. Each of these binaries must be assigned a number of relevant parameters, including individual masses. By manipulating the distributions from which individual black holes are drawn, we demonstrate a method which allows generation of the full population in minutes rather than weeks. This forms the basis for analysis requiring multiple realizations of the background, such as constraining the variance of the stochastic signal.   

The PyCBC search for compact binary mergers in the second run of Advanced LIGO

The PyCBC software implements a matched-filter search for gravitational-wave signals associated with mergers of compact binaries. During the first observing run of Advanced LIGO, it played a fundamental role in the discovery of the binary-black-hole merger signals GW150914, GW151226 and LVT151012. In preparation for Advanced LIGO's second run, PyCBC has been modified with the goal of increasing the sensitivity of the search, reducing its computational cost and expanding the explored parameter space. The ability to report signals with a latency of tens of seconds and to perform inference on the parameters of the detected signals has also been introduced. I will give an overview of PyCBC and present the new features and their impact.   

Transition of EMRIs through resonance: higher order corrections in resonant flux enhancement

Extreme mass ratio inspirals (EMRIs) are candidate events for gravitational wave detection in the millihertz range (by detectors like LISA and eLISA). These events involve a stellar-mass black hole, or a similar compact object, descending into the gravitational field of a supermassive black hole, eventually merging with it. Properties of the inspiraling trajectory away from resonance are well known and have been studied extensively, however little is known about the behaviour of these binary systems at resonance, when the radial and lateral frequencies of the orbit become commensurate. There are two resonance models in the literature, the instantaneous frequency function by Gair, Bender, and Yunes, and the standard two timescales approach devised by Flanagan and Hinderer. We argue that the Gair, Bender and Yunes model provides a valid treatment of the resonance problem and extend this solution to higher order in the size of the on-resonance perturbation. The non-linear differential equations which arise in treating resonances are interesting from a mathematical view point. We present our algorithm for perturbative solutions and the results to third order in the infinitesimal parameter, and discuss the scope of this approach.   

Christodoulou Memory of GW150914 - Prospects of Detection in LIGO and Future Detectors

The event GW150914 produced strains of the order $10^{-21}$ in the two instruments comprising the Laser Interferometric Gravitational Wave Observatory (LIGO). The event has been interpreted as originating in a coalescing black hole binary, with individual components of about 30 solar masses each. A striking aspect of the coalescence deduced from the signal is the emission of 3 solar masses of energy in the oscillating gravitational wave. Theory predicts a DC component of the gravitational signal associated with the emission of such large amounts of gravitational wave energy known as the Christodoulou memory. The memory, as a non-linear component of the signal, is expected to be an order of magnitude smaller than the amplitude of the primary AC component of the gravitational waves. We discuss the prospects of detecting the Christodoulou memory in similar future signals, both with LIGO and with other detectors, including future space-based instruments.   

Analysis of Gravitational Signals from Core-Collapse Supernovae (CCSNe) using MatLab

When a massive star runs out of fuel, it collapses under its own weight and rebounds in a powerful supernova explosion, sending, among other things, ripples through space-time, known as gravitational waves (GWs). GWs can be detected by earth-based observatories, such as the Laser Interferometer Gravitational-Wave Observatory (LIGO). Observers must compare the data from GW detectors with theoretical waveforms in order to confirm that the detection of a GW signal from a particular source has occurred. GW predictions for core collapse supernovae (CCSNe) rely on computer simulations. The UTK/ORNL astrophysics group has performed such simulations. Here, I analyze the resulting waveforms, using Matlab, to generate their Fourier transforms, short-time Fourier transforms, energy spectra, evolution of frequencies, and frequency maxima. One product will be a Matlab interface for analyzing and comparing GW predictions based on data from future simulations. This interface will make it easier to analyze waveforms and to share the results with the GW astrophysics community.   

Gravitational Waves from Fallback Accretion in Long Gamma-Ray Bursts

The collapsar scenario for long gamma-ray bursts (GRBs), detailed by fallback accretion onto a nascent neutron star and subsequent collapse to a black hole, presents a promising source of gravitational waves (GWs) in the sensitive band for ground-based GW detectors. Piro $\&$ Thrane (2012) introduced an analytical model for GW emission from fallback accretion in long GRBs, detailing the spin-up of the neutron star and saturation of secular non-axisymmetric instabilities, which sources GW emission until the neutron star collapses to a black hole. We augment this model to consider finite-temperature equations of state, and consequently, realistic mass-radius evolution and maximum neutron star mass. In addition to this, we investigate the plausibility of hybridising this model with a black hole ringdown term to describe the late-time evolution of the system. We outline the analysis to search for such GW signals, and explore their detectability with second-and-third-generation ground-based GW detectors.   

Visualizing and understanding vortex and tendex lines of colliding black holes

Gravitational waves (GWs) are ripples of spacetime. In order to detect and physically study the GW emitted by merging black holes with ground based detectors such as aLIGO, we must accurately predict how the waves look and behave. This requires numerical simulations of black hole (BH) mergers on supercomputers, because all analytical approximations fail near the time of merger. These simulations also reveal how BHs warp space and time. My project focuses on using these simulations to visualize the strongly curved space time in simulations of merging BHs. I have visualized the vortex and tendex lines for a binary BH system, using the Spectral Einstein Code. Vortex lines describe how an observer would be twisted by the curvature, and the tendex lines describe an observer would be stretched at squeezed by it. These lines are analogous to how electric and magnetic field lines describe the electromagnetic forces on an observer. Visualizing these will provide a more intuitive understanding of the nonlinear dynamics of the spacetime of merging BHs. I am exploring how these lines change with time during a simulation, to see whether they vary smoothly in time and how they depend on where they are seeded.   

Neutrino Astrophysics and the Fermi Large Area Telescope

Photohadronic emission models suggest both neutrinos and gamma-ray photons could be produced by accelerated photons in the relativistic jets of blazars. As the background spectrum falls rapidly with increasing energy, individual events with energies of the order of PeV and above are the best candidates in the search for their astrophysical origin. We present results from our search for possible FSRQ counterparts to high energy neutrinos detected by IceCube. We also present strategies implemented for quick Fermi-LAT followup of new IceCube detections.   

Comparative study of carbonaceous meteoritic fragments by micro-Raman spectroscopy and SEM/EDS.

Meteorites provide precious clues about the formation of planets in the solar system. In particular, carbonaceous chondritic meteorites, considered the most primitive surviving materials from the early Solar System, can contribute to understand how planetisimals (the precursors to planets, of 1-100~km in radius) formed from dust (micron-size grains). These relics are mainly composed of chondrules (micro/millimeter-sized inclusions) surrounded by a matrix of microparticles. Here we present a comparative study of the structure and composition of the chondrules and surrounding matrix of different carbonaceous chondritic meteorites using low- and high-resolution micro-Raman spectroscopy and SEM/EDS (Scanning Electron Microscopy/Energy Dispersive X-ray Spectroscopy). We examine how these properties vary in different regions of the chondrules and matrix, capturing details from micrometer to millimeter scales. We compare the structure and composition between different samples, looking for signatures of the physical processes that drove their formation.   

Fourier transform spectroscopy for future planetary missions

Thermal-emission infrared spectroscopy is a powerful tool for exploring the composition, temperature structure, and dynamics of planetary atmospheres; and the temperature of solid surfaces. A host of Fourier transform spectrometers (FTS) such as Mariner IRIS, Voyager IRIS, and Cassini CIRS from NASA Goddard have made and continue to make important new discoveries throughout the solar system. Future FTS instruments will have to be more sensitive (when we concentrate on the colder, outer reaches of the solar system), and less massive and less power-hungry as we cope with decreasing resource allotments for future planetary science instruments. With this in mind, we have developed CIRS-lite, a smaller version of the CIRS FTS for future planetary missions. We discuss the roadmap for making CIRS-lite a viable candidate for future planetary missions, including the recent increased emphasis on ocean worlds (Europa, Encelatus, Titan) and also on smaller payloads such as CubeSats and SmallSats.   

Advanced Ion Mass Spectrometer for Giant Planet Ionosphere, Magnetospheres and Moons

We present our Advanced Ion Mass Spectrometer (AIMS) for outer planet missions which has been under development from various NASA sources (NASA Living with a Star Instrument Development (LWSID), NASA Astrobiology Instrument Development (ASTID), NASA Goddard Internal Research and Development (IRAD)s) to measure elemental, isotopic, and simple molecular composition abundances of 1 V to 25 kV hot ions with wide field-of-view (FOV) in the 1 -- 60 amu mass range at mass resolution M/$\Delta $M $\le $ 60 over a wide dynamic range of particle intensities and penetrating radiation background from the inner magnetospheres of Jupiter and Saturn to the outer magnetospheric boundary regions and the upstream solar wind. This instrument will work for both spinning spacecraft and 3-axis stabilized spacecraft. AIMS will measure the ion velocity distribution functions (VDF) for the individual ion species from which velocity moments will give their ion density, flow velocity and temperature.   

Gamma-Ray Bursts Search with HAWC

The High Altitude Water Cherenkov (HAWC) Gamma-ray observatory is a wide field-of-view observatory sensitive to gamma rays in the 100 GeV - 100 TeV energy range, located in Mexico at an altitude of 4100 m. In the present work we present results on the search for excesses in the rates of signals from the individual photomultiplier tubes (PMTs) using the Time to Digital Converters (TDC) of HAWC. This search is based on the implementation of the Moving Average Ratio Analysis (MARA) focused on the characterization of the different physical phenomena that may give rise to such excesses: noise in the PMTs, atmospheric conditions related with thunderstorms and excesses of astrophysical origin such as variable sources of high energy gamma rays and in particular GRBs. In particular we present an analysis over the HAWC historical data for the search of such excesses and elaborate on the possible physical interpretation of the found excesses.   

Modification to the Calculation of a Two-point Correlation Function

We suggest a modification to the calculation of a two-point correlation function $\xi(s)=\frac{DD(s)-2DR(s)+RR(s)}{RR(s)}$ commonly used in the analysis of large-scale structures in cosmology. Traditionally, it is known that the catalog of random galaxies, for efficient background elimination, has to be at least an order of magnitude larger than the target data catalog. The na\"ive algorithm to calculate the correlation function in the configuration space requires calculating the distances between all possible pairs of galaxies within a reasonable distance scale, which is thereby $O(n^2)$. Hence, the overall computing time is dominated by the calculations of $RR(s)$ and, to a lesser extent, $DR(s)$. The new algorithm discussed here utilizes a probability density distribution of galaxies to eliminate the background. This galaxy distribution is isotropic which implies that it is separable into a function of two angular coordinates $(\alpha, \delta)$ and another function of radial distance represented by the redshift $z$. This allows for a faster computation of $RR(s)$ and $DR(s)$ by simplifying the convolution integrals. We also demonstrate that the new method suggested is statistically more robust than the conventional method.   

Searching for Signals of Merging Primordial Black Hole Binaries

It was recently advocated that the interactions of 30 solar masses primordial black holes composing the dark matter could explain the first ever observed coalescence event of BHs by the LIGO interferometers. We will discuss potential probes for such a scenario. One probe is the measurement of the eccentricities of the inspiralling binary black holes. We will show that PBH binaries are formed on highly eccentric orbits and can then merge on timescales that in some cases are years or less, retaining some eccentricity in the last seconds before the merger, which can be detected by LIGO or future Einstein Telescope by the observation of high frequency gravitational wave modes. In contrast, in massive-stellar-binaries, globular-clusters, or other astrophysical environment of binary black holes, the orbits have very effectively circularized by the time the binary enters the observable LIGO window.Finally we will discuss the possibility of detecting a signal of PBH binaries in the stochastic gravitational wave background with future gravitational wave detectors.   

Common structure-balance between spacetime structure and massenergy structure

According to Einstein field equation, there is a balance between spacetime structure and massenergy structure. nd the paper consider it as a common structurewhich was brought forward by Daqing Cao in 2011 ecause it is general structure in the universe and everything have the same model of structure in their one system. The Jovian planets is spacetime structure of solar system because they are gas-sphere and they have more density of spacetime (spacetime/massenergy) than the density of massenergy (massenergy/spacetime). The terrestrial planets is massenergy structure of solar system because they are rock-ball and they have more density of massenergy than the density of spacetime. That can explain of that the Jovian planets of big mass is far away from sun. With the idea that the wave is spacetime and the wave effect is spacetime structure, the planets have elliptic orbits and the same direction of their revolution. Because sun is like a massenergy center of the massenergy structure and the terrestrial planets, the paper supposes there is a dark sun-a dark hole who has a spacetime center of spacetime structure and influences on the orbits of the Jovian planets. \underline {http://meetings.aps.org/Meeting/APR16/Session/M13.8}   

A Two-Step Integrated Theory of Everything (TOE)

Two opposing TOE visions are my Two-Step (physics/math) and Hawking's single math step. My Two-Step should replace the single step because of the latter's near zero results after a century of attempts. My physics step had 3 goals. First ``Everything'' was defined as 20 interrelated amplified theories (e.g. string, Higgs forces, spontaneous symmetry breaking, particle decays, dark matter, dark energy, stellar black holes) and their intimate physical interrelationships. Amplifications of Higgs forces theory (e.g. matter particles and their associated Higgs forces were one and inseparable, spontaneous symmetry breaking was bidirectional and caused by high temperatures not Higgs forces, and sum of 8 Higgs forces of 8 permanent matter particles was dark energy) were key to my Two-Step TOE. The second goal answered all outstanding physics questions: what were Higgs forces, dark energy, dark matter, stellar black holes, our universe's creation, etc.? The third goal provided correct inputs for the two part second math step, an E8 Lie algebra for particles and an N-body cosmology simulation (work in progress). Scientific advancement occurs only if the two opposing TOEs are openly discussed/debated.   

The cosmological Janus model: comparison with observational data

In 2014 we presented a model based on a system of two coupled field equations to describe two populations of particles, one positive and the other mass of negative mass. The analysis of this system by Newtonian approximation show that the masses of the same signs attract according to Newton's law while the masses of opposite signs repel according to an anti-Newton law. This eliminates the runaway phenomenon. It uses the time-dependent exact solution of this system to build the bolometric magnitude distribution of the red-shift. Comparing the prediction of our model -which requires adjustment with a single parameter- with the data from 740 supernovae highlighting the acceleration of the universe gives an excellent agreement. The comparison is then made with the multi-parametric $\Lambda $ CDM model. (1) J-P. Petit, and G. D'Agostini, Negative mass hypothesis and the nature of dark energy Mod. Phys. Lett.$ A$ \textbf{29}, 1450182 (2014) (2) J.P.Petit et G. D'Agostini~: Cosmological bimetric model with interacting positive andnegative masses and two different speeds of light, in agreement with the observed acceleration of the Universe. Mod. Phys. Let. A Vol. 29, No. 34 (2014 nov. 10th) 1450182   

Constraints on extra dimensions within the framework of the Standard Model Extension

We consider Kaluza-Klein-type extensions of General Relativity in which extra dimensions may be large but do not necessarily have units of length. Additional coordinates of this kind necessarily violate Lorentz symmetry in principle, but whether or not the violations are detectable in practice depends on the dimension-transposing constants that convert them into lengths. We parametrize these violations in terms of coefficients associated with the matter sector of the Standard Model Extension, and show that the associated variation in fundamental quantities, such as rest mass or charge, must occur slowly, on cosmological scales.   

Magnetic Draping as a Possible Solution to Turbulent Heating of the ICM in Kinetic Mode AGN Feedback

Recent x-ray measurements of the Perseus Cluster intracluster medium (ICM) by the Hitomi Mission found a velocity dispersion measure of $\sigma \sim 150$ km/s, indicating a large-scale turbulent energy of approximately 4$\%$ of the thermal energy. If this energy is transferred to small scales via a turbulent cascade and dissipated as heat, radiative cooling can be offset and the cluster can remain in its observed thermal equilibrium. We investigate the role of AGN feedback, specifically the production of turbulence by g-modes generated by the supersonic expansion and buoyant rise of AGN-driven bubbles, in a plane-parallel model of the ICM using 3D ideal MHD simulations. We present results for a magnetic field perpendicular to the gravitational field as well as a helical field. We find that, while magnetic draping is able to better preserve AGN-driven bubbles and excite stronger g-modes, the production of turbulence is still inefficient. This fact is likely due to the magnetic tension force preventing the production of vortices in the ICM plasma. Our work shows that ideal MHD is an insufficient description for the cluster feedback process and we discuss future work such as the inclusion of anisotropic viscosity as a means of simulating high $\beta$ plasma kinetic effects.   

Performance of vegetative and fruits Zn/Cu based electrochemical cell

We have studied the performance of PKL, Aloe Vera, Tomato and Lemon juice electrochemical Cells without load condition for 1:1 Zn/Cu based electrodes. It was studied the variation of Open circuit voltage (Voc), Short current (Isc) and Maximum Power (P$_{\mathrm{max}})$ with the variation of time for PKL, Aloe Vera, Tomato and Lemon juice electrochemical Cells. It was seen from the research observation that the discharge characteristic of the PKL electrochemical cell was more efficient than the other three Aloe Vera, Tomato and Lemon juice electrochemical Cells. Because the Open circuit voltage (Voc), Short current (I$_{\mathrm{sc}})$ and Maximum Power (P$_{\mathrm{max}})$ are more stable and steady than the others three Aloe Vera, Tomato and Lemon juice electrochemical Cells. Furthermore, to enhance the performance we have also studied the secondary salt effect by using the NaCl as an electrolyte with the PKL, Aloe Vera and Lemon juice electrochemical Cells. Most of the results have been tabulated and graphically discussed.   

Verifying the Simulation Hypothesis via Infinite Nested Universe Simulacrum Loops

The simulation hypothesis proposes that local reality exists as a simulacrum within a hypothetical computer's dimension. More specifically, Bostrom's trilemma proposes that the number of simulations an advanced 'posthuman' civilization could produce makes the proposition very likely. In this paper a hypothetical method to verify the simulation hypothesis is discussed using infinite regression applied to a new type of infinite loop. Assign dimension n to any computer in our present reality, where dimension signifies the hierarchical level in nested simulations our reality exists in. A computer simulating known reality would be dimension (n-1), and likewise a computer simulating an artificial reality, such as a video game, would be dimension (n$+$1). In this method, among others, four key assumptions are made about the nature of the original computer dimension n. Summations show that regressing such a reality infinitely will create convergence, implying that the verification of whether local reality is a grand simulation is feasible to detect with adequate compute capability. The action of reaching said convergence point halts the simulation of local reality. Sensitivities to the four assumptions and implications are discussed.   

A Study on the Performance and Electrochemistry of Bryophyllum pinnatum Leaf (BPL) Electrochemical Cell

The study was carried out to investigate on an innovative invention, Pathor Kuchi Leaf (PKL) electrochemical cell, which is fueled with PKL sap of widely available plant called \textit{Bryophyllum pinnatum} as an energy source for use in PKL battery to generate electricity. This battery, a primary source of electricity, has several order of magnitude longer shelf-lives than the traditional Galvanic cell battery, is still under investigation. In this regard, we have conducted some experiments using various instruments including Atomic Absorption Spectrophotometer (AAS), Ultra-Violet Visible spectrophotometer (UV-Vis), pH meter, Ampere-Volt-Ohm Meter (AVO Meter) etc. The AAS, UV-Vis and pH metric analysis data provided that the potential and current were produced as the Zn electrode itself acts as reductant while Cu$^{\mathrm{2+}}$ and H$^{\mathrm{+}}$ ions are behaving as oxidant. The significant influence of secondary salt on current and potential leads to the dissociation of weak organic acids in PKL juice, and subsequent enrichment to the reactant ions by the secondary salt effects. However, the liquid junction potential was not as great as minimized with the opposite transference of organic acid anions and H$^{\mathrm{+\thinspace }}$ions as their dissimilar ionic mobilities. Moreover, the large value of equilibrium constant (K) implies the big change in Gibbs free energy ($\Delta $G), revealed the additional electrical work in presence of PKL sap. This easily fabricated high performance PKL battery can show an excellent promise during the off-peak across the country-side.   

Performance of Electricity Generation from Bryophyllum Leaf for Practical Utilisation

Constructing an affordable cost, environment friendly simplified electrical energy source with Pathor Kuchi Leaf (PKL) for power electrifications which will significantly upgrade the life style of 1.6 billion people especially, who live in rural areas of Bangladesh. However, one fifth of the world's population still lack access to electricity-well, mainly in Sub-Saharan Africa and South Asia (Bangladesh, India, Sri Lanka, Pakistan, Nepal and Bhutan). This innovative technology will meet essential requirements as lighting, telecommunication as well as information access. Electrodes are put into the \textit{Bryophyllum Pinnatum} Leaf (BPL) or Pathor Kuchi Leaf (PKL) sap and they produce substantially sufficient amount of electricity to power energy consumed electronics and electrical appliances. CuSO$_{\mathrm{4}}$.5H$_{\mathrm{2}}$O solution is used as a secondary salt. The role of CuSO$_{\mathrm{4}}$.5H$_{\mathrm{2}}$O solution has been studied. The electrical and chemical properties, a very important factor for PKL electricity generation device have been studied in this research work. The electrical properties are: internal resistance, voltage regulation, energy efficiency, pulse performance, self discharge characteristics, discharge characteristics with load, capacity of the PKL cell, temperature characteristics and life cycle of the PKL cell. The chemical properties are: variation of voltage, current with the variation of [Zn$^{\mathrm{2+}}$], [Cu$^{\mathrm{2+}}$] and time. The performance of the production of the two bi-products (fertilizer and hydrogen gas production) has been studied. Variation of concentration of Zn$^{\mathrm{2+}}$ and Cu$^{\mathrm{2+}}$ with the variation of percentage of the