arXiv subjects

S. Ganesh

Publications and source records attributed to S. Ganesh.

At least 19 recordsLinked to original sources

arXiv2026

Activity and composition of periodic comets 67P/Churyumov-Gerasimenko and 103P/Hartley 2 at two different perihelion passages

Through photometry and spectroscopy, we studied the evolution of the activity and chemical composition of comet 67P during its 2025 and 2021 perihelion passages and of comet 103P during its 2010 and 2023 passages. For each comet, we aim to compare their behavior from one apparition to another. We used the TRAPPIST telescopes to monitor the comets using broadband and narrowband filters. From the broadband images, we produced light curves and computed color indices for each passage, and we derived the activity slopes. We used a Haser model to compute the production rates of five gaseous species (CN, C2, C3, OH, and NH) and derived the proxy parameter Afrho for dust activity. We also observed both comets in spectroscopy during their most recent apparition using the Himalayan Chandra Telescope and compared the spectroscopic data to our results obtained through photometry. For both comets, our analysis of coma colors does not reveal any significant change from one passage to the other, indicating that the properties of the released dust grains are similar. Our values of the color indices are consistent with the mean values for Jupiter-family comets. We measured a slight increase in the gas and dust activities of comet 67P between 2015 and 2021, probably due to the small change in the comet's orbit that led the perihelion distance to decrease from 1.24 au for the first apparition to 1.21 au for the second one. Regarding 103P, we unambiguously measured a decrease (of at least 50\%) in the gas and dust activities between 2010 and 2023, showing a different behavior for this young, active comet. We find a typical chemical composition for both comets and detect no variation of the C2-to-CN production rate ratios and dust-to-gas ratios from one passage to the other, indicating constant compositions, even if the level of activity has changed for 103P.

astro-ph.EP↗

arXiv2025

Ionic emissions and activity evolution in comet C/2020 F3 (NEOWISE): Insights from long-slit spectroscopy and photometry

Comet C/2020 F3 (NEOWISE) was the brightest comet in the northern hemisphere since C/1995 O1 (Hale-Bopp), providing a unique opportunity to study its composition and spatial distribution of emissions. We conducted narrow-band photometry and long-slit low-resolution spectroscopy to monitor the comet's activity and compositional evolution over several weeks post-perihelion. Narrow-band images (OH, NH, CN, C$_2$, C$_3$, BC, GC, RC) and broad-band images (B, V, Rc, Ic) were acquired with TRAPPIST-North between 22 July and 10 September 2020 to derive production rates, mixing ratios, and dust proxy (Af$\rho$). A long-slit spectrum obtained on 24 July 2020 with HFOSC on the 2-m HCT was used to analyse emission profiles along the sunward and anti-sunward directions. We report production rates and mixing ratios of OH, NH, CN, C$_2$, C$_3$, and NH$_2$, and derive the water production rate using forbidden oxygen line flux. Ionic emissions from N$_2^+$, CO$^+$, CO$_2^+$, and H$_2$O$^+$ were detected at 4$\times$10$^4$ to 1$\times$10$^5$ km from the nucleus in the tailward direction. The average N$_2^+$/CO$^+$ ratio was found to be (3.0 $\pm$ 1.0)$\times$10$^{-2}$, refined to (4.8 $\pm$ 2.4)$\times$10$^{-2}$ using fluorescence modeling. The CO$_2^+$/CO$^+$ ratio was measured to be 1.34 $\pm$ 0.21. These results suggest the comet likely formed in the cold mid-to-outer solar nebula (approx. 50-70 K). Additionally, the average rotation period was estimated as 7.28 $\pm$ 0.79 hours, with a CN outflow velocity of 2.40 $\pm$ 0.25 km/s

astro-ph.EP↗

arXiv2025

Many body gravity and the bullet cluster

Many body gravity (MBG) is an alternate theory of gravity, which has been able to explain the galaxy rotation curves, the radial acceleration relation (RAR) and the wide binary stars (WBS). The genesis of MBG is a novel theory, which models systems with thermal gradients, by recasting the variation in the temperature as a variation in the metric. Merging the above concept with Einstein's gravity, leads to the theory of thermal gravity in 5-D space-time-temperature. Thermal gravity when generalized for partially thermalized systems, results in the theory of many body gravity. The bullet cluster is supposed to be a smoking gun evidence for the presence of dark matter. However, this work demonstrates that the MBG theory can explain the weak gravitational lensing effect of the bullet cluster, without the need for yet undiscovered baryonic matter or dark matter.

gr-qc↗

arXiv2024

Constraints on Triton atmospheric evolution from occultations: 1989-2022

Context - Around the year 2000, Triton's south pole experienced an extreme summer solstice that occurs every about 650 years, when the subsolar latitude reached about 50{\deg}. Bracketing this epoch, a few occultations probed Triton's atmosphere in 1989, 1995, 1997, 2008 and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of Triton's atmospheric pressure which is presented here. Aims- The goal is to constrain the Volatile Transport Models (VTMs) of Triton's atmosphere that is basically in vapor pressure equilibrium with the nitrogen ice at its surface. Methods - Fits to the occultation light curves yield Triton's atmospheric pressure at the reference radius 1400 km, from which the surface pressure is induced. Results - The fits provide a pressure p_1400= 1.211 +/- 0.039 microbar at radius 1400 km (47 km altitude), from which a surface pressure of p_surf= 14.54 +/- 0.47 microbar is induced (1-sigma error bars). To within error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p_1400 = 1.18 +/- 0.03 microbar and p_surf= 14.1 +/- 0.4 microbar, respectively. Based on recent models of Triton's volatile cycles, the overall evolution over the last 30 years of the surface pressure is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton could explain the relatively constant pressure between 2017 and 2022.

astro-ph.EP↗

arXiv2023

Absolute frequency measurements on the $5s5p^{3}$P$_{0}\to5s6d^{3}$D$_{1}$ transition in strontium

We report the first absolute frequency measurements for the $5s5p^{3}$P$_{0}\to5s6d^{3}$D$_{1}$ transition at 394 nm for all the stable strontium isotopes by utilizing repumping induced spectroscopy in a magneto-optical trap. Absolute transition frequency is measured to be 760524409251(25) kHz for $^{88}$Sr.With reference to $^{88}$Sr, the isotope shifts are measured to be 91052(35), 54600(33), and 51641(28) kHz for $^{84}$Sr, $^{86}$Sr, and $^{87}$Sr, respectively. We calculate the hyperfine constants A and B for the fermionic isotope $^{87}$Sr at kHz level. Furthermore, we perform King plot analysis by combining isotope shifts on the 689-nm transition to our data.

physics.atom-ph↗

arXiv2023

5-D thermal field theory, Einstein field equations and spontaneous symmetry breaking

It has been shown previously, that the spatial thermal variation of a thermal medium can be recast as a variation in the Euclidean metric. It is now extended to temporal variations in temperature, for a non-relativistic thermal bath, which remains in local thermal equilibrium. This is achieved by examining the thermal field theory in a five-dimensional space-time-temperature. The bulk thermodynamic quantity, namely the energy density, is calculated for a neutral scalar field with a time-dependent Hamiltonian. Furthermore, the concept of recasting thermal variations as a variation in the metric is extended to thermal systems in a gravitational field. The Einstein field equations, in the 5-D space-time-temperature, is determined. It is shown that the resulting Ricci scalar can lead to spontaneous symmetry breaking, leading to the Higgs mechanism. In essence, the asymmetry in the distribution of temperature in space-time can translate to spontaneous symmetry breaking of particle fields, in a very strong gravitational field.

hep-th↗

arXiv2022

Quantum theory, thermal gradients and the curved Euclidean space

The Euclidean space, obtained by the analytical continuation of time, to an imaginary time, is used to model thermal systems. In this work, it is taken a step further to systems with spatial thermal variation, by developing an equivalence between the spatial variation of temperature in a thermal bath and the curvature of the Euclidean space. The variation in temperature is recast as a variation in the metric, leading to a curved Euclidean space. The equivalence is substantiated by analyzing the Polyakov loop, the partition function and the periodicity of the correlation function. The bulk thermodynamic properties like the energy, entropy and the Helmholtz free energy are calculated from the partition function, for small metric perturbations, for a neutral scalar field. The Dirac equation for an external Dirac spinor, traversing in a thermal bath with spatial thermal gradients, is solved in the curved Euclidean space. The fundamental behavior exhibited by the Dirac spinor eigenstate, may provide a possible mechanism to validate the theory, at a more basal level, than examining only bulk thermodynamic properties. Furthermore, in order to verify the equivalence at the level of classical mechanics, the geodesic equation is analyzed in a classical backdrop. The mathematical apparatus is borrowed from the physics of quantum theory in a gravity-induced space-time curvature. As spatial thermal variations are obtainable at QCD or QED energies, it may be feasible for the proposed formulation to be validated experimentally.

hep-th↗

arXiv2021

Bottomonium suppression in PbPb collision at energies available at the CERN large hadron collider

We had been gradually working towards building a comprehensive quarkonia suppression formalism to explain all 3 dependencies of quarkonium suppression obtained from heavy-ion collision experiments. We present here the improved version of quarkonia suppression framework. It assumes bottomonia produced in the early stage which dissociates due to color screening, gluonic dissociation, and collisional damping in addition to the shadowing as an initial state effect. The QGP medium formed in the collisions is assumed to evolve under ($3+1$)-dimensional relativistic viscous hydrodynamics which is modeled using ECHO-QGP. This replaces the Bjorken's hydrodynamics which we had used in our earlier work where we determined the centrality and transverse momentum dependent suppression. The correlated bottom quark and bottom anti-quark could recombine in the plasma. A rate equation is employed, whose solution gives the final number of bottomonium after dissociation and recombination under $(3+1)$-dimensional expansion of the QGP medium. The Shadowing effect, which is the dominant Cold Nuclear Matter effect at LHC energies, has now been modified by employing the most recent parton distribution functions obtained from CT14 global analysis and shadowing factors from EPPS16. Using this improved formalism we determine the centrality, transverse momentum, and rapidity, dependencies of bottomonium suppression for $Υ(1S)$, and $Υ(2S)$ at the LHC's energies of $2.76$ TeV and $5.02$ TeV. We find a fairly good agreement between theoretically calculated survival probability and the measured nuclear modification factor($R_{AA}$) at the two energies.

hep-ph↗

arXiv2020

Asteroseismology of sz lyn using multi-band high time resolution photometry from ground and space

We report the analysis of high temporal resolution ground and space based photometric observations of SZ Lyncis, a binary star one of whose components is a high amplitude $δ$ Scuti. UBVR photometric observations were obtained from Mt. Abu Infrared Observatory and Fairborn Observatory; archival observations from the WASP project were also included. Furthermore, the continuous, high quality light curve from the TESS project was extensively used for the analysis. The well resolved light curve from TESS reveals the presence of 23 frequencies with four independent modes, 13 harmonics of the main pulsation frequency of 8.296943$\pm$0.000002 d$^{-1}$ and their combinations. The frequency 8.296 d$^{-1}$ is identified as the fundamental radial mode by amplitude ratio method and using the estimated pulsation constant. The frequencies 14.535 d$^{-1}$, 32.620 d$^{-1}$ and 4.584 d$^{-1}$ are newly discovered for SZ Lyn. Out of these three, 14.535 d$^{-1}$ and 32.620 d$^{-1}$ are identified as non-radial lower order p-modes and 4.584 d$^{-1}$ could be an indication of a g-mode in a $δ$ Scuti star. As a result of frequency determination and mode identification, the physical parameters of SZ Lyn were revised by optimizations of stellar pulsation models with the observed frequencies. The theoretical models correspond to 7500 K $\le $T$_{\rm eff}$ $\le$ 7800 K, log(g)=3.81$\pm$0.06. The mass of SZ Lyn was estimated to be close to 1.7--2.0 M$_\odot$ using evolutionary sequences. The period-density relation estimates a mean density $ρ$ of 0.1054$\pm$0.0016 g cm$^{-3}$

astro-ph.SR↗

arXiv2020

Effect of temperature gradient on heavy quark anti-quark potential using gravity dual model

Thermal systems have traditionally been modeled via Euclideanized space by analytical continuation of time to an imaginary time. We extend the concept to static thermal gradients by recasting the temperature variation as a variation in the Euclidean metric. We apply this prescription to determine the Quark anti-Quark potential in a system with thermal gradient. A naturally occurring QCD medium with thermal gradients is a Quark Gluon Plasma (QGP). However, the QGP evolves in time. Hence, we use a quasi-stationary approximation, which is applicable only if the rate of time evolution is slow. The application of our proposal to a Quark anti-Quark potential in QGP can be seen as a step towards a more exact theory which would incorporate time varying thermal gradients. The effect of a static temperature gradient on the Quark anti-Quark potential is analyzed using a gravity dual model. A non-uniform black string metric is developed, by perturbing the Schwarzchild metric, which allows to incorporate the temperature gradient in the dual AdS space. Finally, an expression for the Quark anti-Quark potential, in the presence of a static temperature gradient, is derived.

hep-ph↗

arXiv2020

A proposal for exploring quantum theory in curved spacetime in lab

Gravity curves spacetime. In regions where the de Broglie wavelength is very small compared to the curvature of spacetime, the wave equations in flat spacetime can be generalized to curved spacetime. The validity of the formulation when the de Broglie wavelength becomes comparable to the curvature is an open question. To test these formulations experimentally, huge energy of the order of the Planck mass would be required. Euclideanized spacetime is used to model thermal systems. In this work, an equivalence between spatial variation of temperature in thermal baths and curvature of Euclideanized spacetime is propounded. The variation in temperature is recast as a variation in the metric. The Dirac equation is then solved in this curved Euclideanized spacetime. The curvature in Euclideanized spacetime can be obtained in Chromodynamic or Electromagnetic scale energies. If this equivalence is correct, it could provide a platform to experimentally explore quantum mechanics in curved spacetime.

hep-th↗

arXiv2019

Centrality and transverse momentum dependent suppression of $Υ(1S)$ and $Υ(2S)$ in p$-$Pb and Pb$-$Pb collisions at the CERN Large Hadron Collider

Deconfined QCD matter in heavy-ion collisions has been a topic of paramount interest for many years. Quarkonia suppression in heavy-ion collisions at the Relativistic Heavy Ion Collider (RHIC) and Large Hadron Collider (LHC) experiments indicate the quark-gluon plasma (QGP) formation in such collisions. Recent experiments at LHC has given some indications of hot matter effect in asymmetric p$-$Pb nuclear collisions. Here, we employ a theoretical model to investigate the bottomonium suppression in Pb$-$Pb at $\sqrt{s_{NN}}=2.76$, $5.02$ TeV, and in p$-$Pb at $\sqrt{s_{NN}}=5.02$ TeV center-of-mass energies under a QGP formation scenario. Our present formulation is based on a unified model consisting of suppression due to color screening, gluonic dissociation along with the collisional damping. Regeneration due to correlated $Q\bar Q$ pairs has also been taken into account in the current work. We obtain here the net bottomonium suppression in terms of survival probability under the combined effect of suppression plus regeneration in the deconfined QGP medium. We mainly concentrate here on the centrality, $N_\text{part}$ and transverse momentum, $(p_{t})$ dependence of $Υ(1S)$ and $ Υ(2S)$ states suppression in Pb$-$Pb and p$-$Pb collisions at mid-rapidity. We compare our model predictions for $Υ(1S)$ and $Υ(2S)$ suppression to the corresponding experimental data obtained at the LHC. We find that the experimental observations on $p_t$ and $N_\text{part}$ dependent suppression agree reasonably well with our model predictions.

hep-ph↗

arXiv2018

Optical variability in IBL S5 0716+714 during the 2013-2015 outburst

With an aim to explore optical variability at diverse timescales in BL Lac source S5 0716+714, it was observed for 46 nights during 2013 January 14 to 2015 June 01 when it underwent two major outbursts. The observations were made using the 1.2-m Mount Abu InfraRed Observatory telescope mounted with a CCD camera. On 29 nights, the source was monitored for more than two hours, resulting in 6256 data points in R-band, to check for the intra-night variability. Observations in B, V and I bands with 159, 214, and 177 data points, respectively, along with daily averaged R-band data are used to address inter-night and long-term variability and the color behavior of S5 0716+71. The study suggests that the source shows significant intra-night variability with a duty cycle of more than 31% and night-to-night variations. The average brightness magnitudes in B, V, R & I bands were found to be 14.42(0.02), 14.02(0.01), 13.22(0.01) & 13.02(0.03), respectively, while S5 0716+714 was historically brightest with R = 11.68 mag on 2015 January 18, indicating that source was in relatively high state during this period. A mild bluer when brighter behavior, typical of BL Lacs, supports the shock-in-jet model. We notice larger amplitudes of variation when the source was relatively brighter. Based on the shortest time scale of variability and causality argument, upper bound on the size of the emission region is estimated to be 9:32x 10^{14} cm and the mass of the black hole to be 5.6 x10^8Ms.

astro-ph.GA↗

arXiv2018

$ψ(2S)$ enhancement in p-Pb collision as an indication of QGP formation at the LHC

Proton-nucleus collisions serve as an important baseline for the understanding and interpretation of the nucleus-nucleus collisions. These collisions have been employed to characterize the cold nuclear matter effects at SPS and RHIC energies for the past several years, as it was thought that Quark-Gluon Plasma (QGP) is not formed in such collisions. However, at the Large Hadron Collider (LHC), there seems a possibility that QGP is formed during proton-lead (p$-$Pb) collisions. In this work, we have derived an expression for gluon induced excitation of $J/ψ$ to $ψ(2S)$, using pNRQCD, and show that the relative enhancement of $ψ(2S)$ vis a vis $J/ψ$, especially at high $p_T$, gives further indication that the QGP is indeed formed in p$-$Pb collisions at the most central collisions at LHC energy. $J/ψ$ and $ψ(2S)$ suppression effects seen at ALICE are also qualitatively explained.

hep-ph↗

arXiv2017

Efficient and Secure Routing Protocol for WSN-A Thesis

Advances in Wireless Sensor Network (WSN) have provided the availability of small and low-cost sensors with the capability of sensing various types of physical and environmental conditions, data processing, and wireless communication. Since WSN protocols are application specific, the focus has been given to the routing protocols that might differ depending on the application and network architecture. In this work, novel routing protocols have been proposed which is a cluster-based security protocol is named as Efficient and Secure Routing Protocol (ESRP) for WSN. The goal of ESRP is to provide an energy efficient routing solution with dynamic security features for clustered WSN. During the network formation, a node which is connected to a Personal Computer (PC) has been selected as a sink node. Once the sensor nodes were deployed, the sink node logically segregates the other nodes in a cluster structure and subsequently creates a WSN. This centralized cluster formation method is used to reduce the node level processing burden and avoid multiple communications. In order to ensure reliable data delivery, various security features have been incorporated in the proposed protocol such as Modified Zero-Knowledge Protocol (MZKP), Promiscuous hearing method, Trapping of adversaries and Mine detection. One of the unique features of this ESRP is that it can dynamically decide about the selection of these security methods, based on the residual energy of nodes.

cs.NI↗

arXiv2017

Multi-wavelength study of flaring activity in HBL 1ES 1959+650 during 2015-16

We present the results from a multiwavelength study of the flaring activity in HBL, 1ES 1959+650, during January 2015-June 2016. The source underwent significant flux enhancements showing two major outbursts (March 2015 and October 2015) in optical, UV, X-rays and gamma-rays. Normally, HBLs are not very active but 1ES 1959+650 has shown exceptional outburst activity across the whole electromagnetic spectrum (EMS). We used the data from Fermi-LAT, Swift-XRT & UVOT and optical data from Mt. Abu InfraRed Observatory (MIRO) along with archival data from Steward Observatory to look for possible connections between emissions at different energies and the nature of variability during flaring state. During October 2015 outburst, thirteen nights of optical follow-up observations showed brightest and the faintest nightly averaged V-band magnitudes as 14.45(0.03) and 14.85(0.02), respectively. In optical, the source showed a hint of optical intra-night variability during the outburst. A significant short-term variability in optical during MJD 57344 to MJD 57365 and in gamma-rays during MJD 57360 and MJD 57365 was also noticed. Multiwavelength study suggests the flaring activity at all frequencies to be correlated in general, albeit with diverse flare durations. We estimated the strength of the magnetic field as 4.21 G using the time-lag between optical and UV bands as synchrotron cooling time scale (2.34 hrs). The upper limits on the sizes of both the emission regions, gamma-ray and optical, are estimated to be of the order of 10^16cm using shortest variability time scales. The quasi-simultaneous flux enhancements in 15 GHz and VHE gamma-ray emissions indicates to a fresh injection of plasma into the jet, which interacts with a standing sub-mm core resulting in co-spatial emissions across the EMS. The complex and prolonged behavior of the second outburst in October 2015 is discussed in detail.

astro-ph.GA↗

arXiv2017

Study of the plutino object (208996) 2003 AZ84 from stellar occultations: size, shape and topographic features

We present results derived from four stellar occultations by the plutino object (208996) 2003~AZ$_{84}$, detected at January 8, 2011 (single-chord event), February 3, 2012 (multi-chord), December 2, 2013 (single-chord) and November 15, 2014 (multi-chord). Our observations rule out an oblate spheroid solution for 2003~AZ$_{84}$'s shape. Instead, assuming hydrostatic equilibrium, we find that a Jacobi triaxial solution with semi axes $(470 \pm 20) \times (383 \pm 10) \times (245 \pm 8)$~km % axis ratios $b/a= 0.82 \pm 0.05$ and $c/a= 0.52 \pm 0.02$, can better account for all our occultation observations. Combining these dimensions with the rotation period of the body (6.75~h) and the amplitude of its rotation light curve, we derive a density $ρ=0.87 \pm 0.01$~g~cm$^{-3}$ a geometric albedo $p_V= 0.097 \pm 0.009$. A grazing chord observed during the 2014 occultation reveals a topographic feature along 2003~AZ$_{84}$'s limb, that can be interpreted as an abrupt chasm of width $\sim 23$~km and depth $> 8$~km or a smooth depression of width $\sim 80$~km and depth $\sim 13$~km (or an intermediate feature between those two extremes).

astro-ph.EP↗

arXiv2017

Optical intra-day variability in 3C 66A: 10 years of observations

We present results based on the observations of the blazar 3C 66A from 2005 November 06 to 2016 February 14 in the BVR and I broadbands using 1.2m telescope of the Mt. Abu InfraRed Observatory (MIRO). The source was observed on 160 nights out of which on 89 nights it was monitored for more than 1 hr to check for the presence of any intra-day variability (IDV). The blazar 3C 66A exhibited significant variations in the optical flux on short and long term time scales. However, unlike highly variable S5 0716+71, it showed IDV duty cycle of about 8% only. Our statistical studies suggest the IDV time scales ranging from $\sim$ 37 min to about 3.12 hours and, in one case, a possibility of the quasi-periodic variations with characteristic timescale of $\sim$ 1.4 hrs. The IDV amplitudes in R$-$band were found to vary from 0.03 mag to as much as 0.6 mag, with larger amplitude of variation when the source was relatively fainter. The typical rate of the flux variation was estimated to be $\sim$0.07 mag hr$^{-1}$ in both, the rising and the falling phases. However, the rates of the brightness variation as high as 1.38 mag/hr were also detected. The shortest timescale of the variation, 37 min, sets an upper limit of $6.92 \times 10^{14}$ cm on the size of the emission region and about $3.7 \times 10^8\ \mathrm{M}_{\odot}$ as an estimate of the mass of the black hole, assuming the origin of the rapid optical variability is in close vicinity of the central SMBH. The long-term study suggests a mild bluer-when-brighter behavior, typical for BL Lacs.

astro-ph.GA↗