A5108091153- High-Energy Particle Collisions Research
- Quantum Chromodynamics and Particle Interactions
- Particle physics theoretical and experimental studies
- Pulsars and Gravitational Waves Research
- Particle Detector Development and Performance
- High-pressure geophysics and materials
- Radiation Detection and Scintillator Technologies
- Nuclear physics research studies
- Gamma-ray bursts and supernovae
- CCD and CMOS Imaging Sensors
- Nuclear reactor physics and engineering
- Cold Atom Physics and Bose-Einstein Condensates
- Geophysics and Sensor Technology
- Statistical Methods and Bayesian Inference
- Markov Chains and Monte Carlo Methods
- Advanced Neural Network Applications
- Network Security and Intrusion Detection
- X-ray Spectroscopy and Fluorescence Analysis
- Stellar, planetary, and galactic studies
- Nuclear Physics and Applications
- Astrophysical Phenomena and Observations
- Dark Matter and Cosmic Phenomena
- Internet Traffic Analysis and Secure E-voting
- ERP Systems Implementation and Impact
- Magnetic Field Sensors Techniques
Institute of Physics, Bhubaneshwar
2015-2024
Homi Bhabha National Institute
2019-2024
Indian Institute of Information Technology Allahabad
2024
Siksha O Anusandhan University
2021
AGH University of Krakow
2018-2019
Brookhaven National Laboratory
2015-2017
Kyoto University
2010
Hokkaido University
2000-2003
Istituto Nazionale di Fisica Nucleare, Sezione di Catania
2001-2002
Justus-Liebig-Universität Gießen
1998
We study the hadron-quark phase transition in interior of neutron stars (NS's). calculate equation state (EOS) hadronic matter using Brueckner-Bethe-Goldstone formalism with realistic two-body and three-body forces, as well a relativistic mean field model. For quark we employ MIT bag model constraining constant by indications coming from recent experimental results obtained at CERN SPS on formation quark-gluon plasma. find necessary to introduce density dependent parameter, corresponding...
Collective flows in heavy-ion collisions from AGS [$(2--11)A$ GeV] to SPS [$(40,158)A$ energies are investigated a nonequilibrium transport model with the nuclear mean field (MF). Sideward $\ensuremath{\langle}{p}_{x}\ensuremath{\rangle}$, directed ${v}_{1}$, and elliptic ${v}_{2}$ systematically studied different assumptions for equation of state (EOS). We find that momentum dependence on MF is important understanding proton collective at energies. Calculated results momentum-dependent...
In the conventional approach to observable $$ n-\overline{n} oscillation through Pati-Salam intermediate gauge symmetry in SO(10), canonical seesaw mechanism is also constrained by breaking scale M R ∼ C ≤ 106 GeV which yields light neutrino masses several orders larger than data. A method evade this difficulty TeV gauged inverse has been recently exploited while predicting experimentally verifiable W ± , Z bosons with a new dominant contribution neutrinoless double beta decay L −W channel...
We discuss the {\it SU}(2) chiral sigma model in context of nuclear matter using a mean field approach at high density. In this we include dynamically generated isoscalar vector and higher-order terms scalar field. With inclusion these, reproduce empirical values saturation density, binding energy, incompressibility. The value incompressibility is chosen according to recently obtained heavy-ion collision data. then apply same dynamical neutron-rich beta equilibrium, related neutron star...
We make a first calculation of eigenfrequencies radial pulsations neutron stars with quark cores in general relativistic formalism given by Chandrasekhar. The equations state used to estimate such have been derived taking proper care the hadron-quark phase transition. hadronic obtained framework Brueckner-Hartree-Fock and mean field theories, whereas equation has within MIT bag model. find that periods oscillation show kink is associated presence mixed region. Also, significant differences...
Eigenfrequencies of radial pulsations "slowly" rotating neutron stars are calculated in a general relativistic formalism given by Chandrasekhar & Friedman. It is found that the square frequencies always decreasing function central density star. The decrease squared frequency sensitive to equation state star matter, and illustrated using realistic models.
We systematically investigate the vacuum stability and nuclear properties in effective chiral model with higher-order terms $\ensuremath{\sigma}$. evaluate parameters by considering saturation of matter as well normal to be globally stable at zero finite baryon densities. find parameter sets giving moderate equations state apply these models nuclei.
A data logger is designed to monitor and record ambient parameters such as temperature, pressure relative humidity along with gas flow rate a function of time. These are required for understanding the characteristics gas-filled detectors Gas Electron Multiplier (GEM) Multi-Wire Proportional Counter (MWPC). The has different microcontrollers been interfaced an ethernet port local LCD unit displaying all measured parameters. In this article, explanation design, hardware, software description...
We present theoretical model comparison with published ALICE results for [Formula: see text]-mesons ([Formula: text], text] and text]) in collisions at = 7 TeV text][Formula: text]TeV. Event generator Heavy-Ion Jet Interaction Generator (HIJING), transport calculation of AMPT calculations from Next-to-Leading Order (NLO)(MNR) Fixed-Order Next-to-Leading-Logarithmic (FONLL) have been used this study. found that HIJING predictions are matching text]-meson cross-sections collisions, while both...
Abstract We perform a comprehensive timing and broadband spectral analysis using an AstroSat observation of the low-mass black hole X-ray binary H 1743–322 during its 2017 outburst. Additionally, we use two Swift/XRT observations, one which is simultaneous with other taken three days earlier, for analysis. The hardness–intensity diagram indicates that outburst was failed one, unlike previous successful in 2016. detect type C quasi-periodic oscillation (QPO) observations at ∼0.4 Hz, whereas...