arXiv subjects

Raj Kumar

Publications and source records attributed to Raj Kumar.

At least 19 recordsLinked to original sources

arXiv2026

X-ray spectral and temporal evolution of atoll source 4U 1820-30 with AstroSat: detection of high frequency quasi-periodic oscillation

AstroSat/LAXPC and SXT observed the persistent neutron star low-mass X-ray binary 4U 1820-30 between 2016 and 2022. During these observations, the hardness-intensity diagram (HID) and color-color diagram (CCD) indicated that the source was in the banana state. We divided the CCD into 11 segments for spectral and timing analyses. For each segment in the CCD, we modeled the spectral data using two distinct approaches over the 0.7-20.0 keV band. A combination of a multi-color-disk component with an inner disk temperature of around 0.6 keV and Comptonized emission from the boundary layer (BL)/ hot corona provided the best description of the X-ray spectral data of this source. The truncation radius was found to be in the range of $\sim$ 19-40 km. The Comptonized component has an optical depth in the range of $\sim 7 - 13$ with electron temperature in the range of $\sim 2.5 - 3.8$ keV. The optical depth of the corona varies significantly along the position on the CCD, while $\sim$ 80\% of the X-ray flux comes from the Comptonized component. We discuss possible physical scenarios to explain the relationship between the spectral evolution and motion of the source along the CCD. The timing analysis revealed kHz QPOs peaks at $\sim 710$ Hz and $\sim 740$ Hz in the lower left banana branch. An energy-dependent study indicates that these QPOs are stronger in the high-energy band.

astro-ph.HE↗

arXiv2026

Competing decay modes and stability analysis of superheavy nuclei with Z = 120 using relativistic mean-field approach

We systematically study the competition between {\alpha}-decay and spontaneous fission in even-even superheavy nuclei with (Z=120) and 256 \leq A \leq 304 within the preformed cluster-decay model using microscopic inputs from relativistic mean-field calculations with the NL3 parameter set. The {\alpha}-decay half-lives are obtained from WKB barrier penetration with empirically determined preformation factors, self-consistent Q_{\alpha} values from RMF, and nuclear interaction potentials constructed using both M3Y and relativistic R3Y nucleon-nucleon forces, and are benchmarked against standard semi-empirical formulas. Our results predict reduced spontaneous fission probabilities and extended {\alpha}-decay chains toward the fermium region for isotopes with 296 \leq A \leq 304, with enhanced stability reflected in maxima of log_{10} T_{1/2} around neutron numbers N \approx 166-182. In particular, the nuclei 296,298,300,302,304_{120} are identified as the most favorable candidates for survival against fission, demonstrating the crucial role of shell effects, deformation, and pairing correlations and providing quantitative guidance for future experimental searches of Z=120 nuclei.

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arXiv2025

Influence of effective interactions and nuclear densities on the dynamics of heavy-ion fusion

The study aims to explore the mechanism of heavy-ion fusion using various effective nucleon-nucleon (NN) interactions and nuclear density distributions. The nuclear potentials are obtained by folding the relativistic effective NN interaction (R3Y) with densities derived from the relativistic mean-field (RMF) approach. The RMF formalism with the NL3$^*$ parameter set and the relativistic-Hartree-Bogoliubov (RHB) approach with the DDME2 parameter set are used to obtain the medium-independent R3Y and density-dependent R3Y (DDR3Y) NN potentials. The results of these relativistic interactions are compared with the Reid and Paris M3Y NN interactions and their density-dependent versions. Nuclear potentials are used to calculate the fusion barrier characteristics and cross-sections within the $\ell$-summed Wong model for $^{16}$O+$^{144}$Sm, $^{48}$Ca+$^{208}$Pb, $^{16}$O+$^{154}$Sm, and $^{48}$Ca+$^{238}$U reactions. The relativistic R3Y and DDR3Y NN potentials provide higher cross-sections than both the Reid and Paris versions. The inclusion of in-medium effects in all interactions results in more repulsive potentials, leading to higher fusion barriers and reduced cross-sections. The impact of nuclear shape degrees of freedom is included for $^{16}$O+$^{154}$Sm and $^{48}$Ca+$^{238}$U reactions involving deformed targets. Results using RMF-NL3$^*$ densities are also compared with those from the two-parameter Fermi (2pF) formula for $^{16}$O+$^{154}$Sm, showing higher cross-sections with RMF densities. A comparison of calculated cross-sections with experimental data shows that the R3Y NN potential with RMF-NL3$^*$ densities provides good agreement for reactions involving both spherical and deformed nuclei.

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arXiv2025

Exploring the role of low-lying intrinsic degrees of freedom and their impact on fusion cross-sections

The present work focuses on examining the low-lying intrinsic degrees of freedom and their impact on fusion dynamics. Fusion cross-sections were calculated using the coupled-channel code CCFULL for four specific reactions: $^{18}$O+$^{74}$Ge, $^{18}$O+$^{148}$Nd, $^{18}$O+$^{182}$W, and $^{18}$O+$^{186}$W, all conducted at energies below the Coulomb barrier across various energy levels. Vibrational and rotational features were studied concerning energy to distinguish their respective effects on fusion properties. The results indicate that the theoretical calculations for the nuclei $^{74}$Ge, $^{148}$Nd, $^{182}$W and $^{186}$W closely match the experimental data, particularly for the $2^+$ excited states. While slight discrepancies are observed for other excited states ($4^+$ and $6^+$), overall agreement remains significant. Additionally, the study reveals that hexadecapole deformation with different magnitudes have significant influences on the fusion cross-section. In cases where $\beta_4$ has a positive value, rotational levels beyond $6^+$ have minimal impact on the cross-section, resulting in a notable difference in the contribution of sequential channels. In contrast, for negative $\beta_4$ values, rotational energy levels up to the $2^+$ state substantially affect the fusion characteristics. Furthermore, the analysis extends to the estimation of the relative change ($\Delta\sigma_{fus}$) between the excited states and the ground state, both with and without considering coupling terms.

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arXiv2025

Study of Solar Energetic Particles: their Source Regions, Flares and CMEs during Solar Cycles 23-24

In this work, we examine the association between solar active regions and 152 solar flares, coronal mass ejections, and solar energetic particle (SEP) events over solar cycles 23-24 (1997-2017). The CDAW center's GOES data in the energy channel >10 MeV (Major SEPs; solar proton events) with flux >= 10 pfu was used for our investigation. For the associated activities, we have analyzed the data from space born satellites namely: SOHO/LASCO and SDO/AIA. We found a moderate correlation (55 %) between SXR flux and sunspot area i.e., active regions with larger sunspot areas generally generate larger flares. We found that most of the SEPs are originated from the magnetically complex active regions i.e., hale class beta-gamma-delta and beta. Very few events were associated with unipolar active regions. Stronger GOES X-ray is linked to more impulsive events, as evidenced by the negative correlation (-0.40) between X-ray flux and SEP duration. In the active region beta-gamma-delta, the highest average SEP intensity (2051 pfu) was detected. In the data set used, only 10 % SEPs are found impulsive in nature, while the remaining 90 % are gradual in nature. All the impulsive events had SEP intensity less than 100 pfu and most of the CMEs associated with these events were decelerated CMEs. We discovered that the majority of faster CMEs are linked to the most complex magnetic active regions. This indicates that high speed CMEs are produced by magnetically complex active regions. We discovered that 58 SEP events in our data set are linked to accelerated CMEs, while 82 are linked to decelerated CMEs. The highest average CME width is found corresponding to magnetically most complex active regions beta-delta, gamma-delta, alpha-gamma-delta and beta-gamma-delta, which shows that large CMEs are the consequences of magnetically complex active regions.

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arXiv2025

Spectro-Polarimetric Study of Weakly Magnetized Neutron Star X-ray binary GX 349+2

We report the first spectro-polarimetric investigation of the bright Z-type source GX 349+2 using simultaneous observations of \textit{IXPE}, \textit{NuSTAR} and \textit{Swift/XRT}. The source exhibited significant polarization in the 2-8 keV energy range during the flaring branch (FB) and normal branch (NB). The estimated polarization degree (PD) and polarization angle (PA) for FB are $1.74 \pm 0.52\%$ ($3.3\sigma$) and $19.4 \pm 8.9^\circ$, respectively; while for NB, PD and PA are $0.8 \pm 0.22\%$ ($3.6\sigma$) and $35.4 \pm 7.9^\circ$, respectively. The energy-resolved polarization for NB revealed an increase in PD from $0.78\pm0.2\%$ ($3.6\sigma$) to $1.32\pm0.40\%$ ($3.3\sigma$) and a change in PA from $17.9\pm8.1^\circ$, and $53.2\pm8.6^\circ$, in the energy range of 2-4 and 4-8 keV, respectively. Using the simultaneous observations of \textit{Swift/XRT} and \textit{NuSTAR}, we investigated the spectral properties of the source during NB, and the Western model well explained it. The spectra also depicted a strong and broad Fe K$\alpha$ line. However, spectro-polarimetric analyses carried out by \textit{IXPE} align closely with model-independent polarimetric results. We discuss results obtained from the polarimetric studies in the context of various coronal geometries, and we confirm the slab-like geometry in the NB for GX 349+2.

astro-ph.HE↗

arXiv2025

Variability study of classical supergiant X-ray binary 4U 1907+09 using NuSTAR

We investigate the X-ray variability of the supergiant X-ray binary 4U 1907+09 using the new NuSTAR observation of 2024. The source had a relatively stable flux level during previous NuSTAR observations, but the flux varied significantly during the current one. The light curve exhibits dips (off-state) and flares (on-state). The phase-coherent timing analysis during the on-state yields a pulse period of $443.99(4)~\mathrm{s}$, showing the pulsar's continued spin-down. The pulse profiles show an asymmetric double-peaked structure with a phase separation of 0.47 between the two peaks. A cyclotron resonance scattering feature (CRSF) is also detected at $\sim 17.6~\mathrm{keV}$, along with its harmonic at $\sim 38~\mathrm{keV}$, persisting across all flux states. Flux-resolved spectroscopy reveals that the CRSF remains constant despite a 25-fold change in flux. The spectral parameters like photon index and e-fold energy are out of phase with the pulse shape, whereas cutoff energy is in phase with the pulse shape. The source's luminosity during the on-state is $2.85 \times 10^{35}~\mathrm{erg~s^{-1}}$, consistent with a "pencil" beam radiation pattern expected at this flux level from a collisionless gas-mediated shock. These results offer further insights into the accretion dynamics and magnetic field geometry of this system.

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arXiv2024

Very High-energy Gamma-Ray Episodic Activity of Radio Galaxy NGC 1275 in 2022-2023 Measured with MACE

The radio galaxy NGC 1275, located at the central region of Perseus cluster, is a well-known very high-energy (VHE) gamma-ray emitter. The Major Atmospheric Cherenkov Experiment Telescope has detected two distinct episodes of VHE (E > 80 GeV) gamma-ray emission from NGC 1275 during 2022 December and 2023 January. The second outburst, observed on 2023 January 10, was the more intense of the two, with flux reaching 58$\%$ of the Crab Nebula flux above 80 GeV. The differential energy spectrum measured between 80 GeV and 1.5 TeV can be described by a power law with a spectral index of $\Gamma = - 2.90 \pm 0.16_{stat}$ for both flaring events. The broadband spectral energy distribution derived from these flares, along with quasisimultaneous low-energy counterparts, suggests that the observed gamma-ray emission can be explained using a homogeneous single-zone synchrotron self-Compton model. The physical parameters derived from this model for both flaring states are similar. The intermediate state observed between two flaring episodes is explained by a lower Doppler factor or magnetic field, which subsequently returned to its previous value during the high-activity state observed on 2023 January 10.

astro-ph.HE↗

arXiv2024

Exploring the effect of positive Q-value neutron transfer in coupled-channels calculations using microscopic nuclear potentials

We investigated the effect of the degree of freedom of neutron transfer on the cross section of heavy-ion fusion reactions, using the relativistic mean-field formalism within the coupled channel approach (CCFULL). We obtain the microscopic nuclear interaction potential in terms of the density distributions for the targets and projectiles with the NL3$^*$ parameter set and corresponding R3Y nucleon-nucleon potential. The present analysis includes the $^{18}$O-induced reactions, for which experimental fusion cross-section is available around the Coulomb barrier. It is evident from the results that including vibrational and/or rotational degrees of freedom enhances the fusion cross-section at energies below the barrier. However, fusion hindrance persists in this energy region. To address this, we incorporated the two-neutron $(2n)$ transfer channels in the Coupled Channel calculation. A comparison with the Woods-Saxon potential (WS) shows that the R3Y nucleon-nucleon (NN) potential, with intrinsic degrees of freedom, is superior to it, especially at energies below the barrier. This superiority can be attributed to the observed higher barrier heights and lower cross-section of the WS potential compared to the relativistic R3Y NN potential for the considered reaction systems. Consequently, we employed the relativistic mean-field formalism to estimate fusion characteristics for the unknown $^{18}$O-induced reactions, namely $^{18}$O + $^{62}${Ni}, $^{18}$O + $^{70,72,76}${Ge}, $^{18}$O + $^{144,150}${Nd}, and $^{18}$O + $^{144,148,152,154}${Sm}. Our analysis highlights the significant role of positive $Q$-value neutron transfer in enhancing the sub-barrier fusion cross-section for the $^{18}$O + $^{148}${Nd} reaction with the R3Y NN potential. However, the effect of this transfer channel for the other considered reactions is comparatively less pronounced.

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arXiv2024

Role of nuclear deformation and orientation about symmetry axis of target nucleus on heavy-ion fusion dynamics

Nuclear shape and orientation degrees of freedom are incorporated into the calculation of the double-folding nuclear potential within the relativistic mean-field (RMF) formalism. The quadrupole deformations ($\beta_2$), nuclear densities and the effective nucleon-nucleon (NN) interaction potential are obtained using the RMF approach for the Hybrid, NL3$^*$ and NL3 parameterizations. The calculated quadrupole deformations are included in the target densities through the nuclear radius. The deformation and orientation-dependent microscopic nuclear potentials are further employed to obtain fusion barrier characteristics and cross-sections for 12 even-even heavy-ion reactions with doubly magic spherical $^{16}$O and $^{48}$Ca as projectiles along with deformed targets from different mass regions. The results obtained for the relativistic R3Y NN potential are compared with those of the Reid version of the non-relativistic M3Y NN potential as well as with the available experimental data. A decrease in the barrier height and increase in the cross-section is observed upon the inclusion of target quadrupole deformations in the nuclear density distributions at the target orientation angles, $\theta_2\le58^\circ$ for the R3Y NN potential and at $\theta_2\le60^\circ$ for the M3Y NN potential. On comparing the $\theta_2$-integrated cross-section calculated using M3Y and R3Y NN potentials with spherical and deformed densities, one observes that the deformed densities and the relativistic R3Y NN potential obtained for the Hybrid parameter set provide better agreement with the available experimental data for all the considered reactions. Moreover, the modifications in the characteristics of the fusion barrier and hence in the cross-section with the inclusion of nuclear shape degrees of freedom and orientations are found to become more prominent in reactions forming heavier compound nuclei.

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arXiv2024

Persistence of the N = 50 shell closure over the isotopic chains of Sc, Ti, V and Cr nuclei using relativistic energy density functional

The analytical expression of the density-dependent binding energy per nucleon for the relativistic mean field (RMF), also known as the relativistic energy density functional (Relativistic-EDF), is used to obtain the isospin-dependent symmetry energy and its components for the isotopic chain of Sc, Ti, V, and Cr nuclei. The procedure of the coherent density fluctuation model is employed to formulate the Relativistic-EDF and Brueckner energy density functional (Brueckner-EDF) at local density. A few signatures of shell and/or sub-shell closure are observed in the symmetry energy and its components, i.e., surface and volume symmetry energy, far from the beta-stable region for odd-A Sc and V, and even-even Ti and Cr nuclei with non-linear NL3 and G3 parameter sets. A comparison is made with the results obtained from Relativistic-EDF and Brueckner-EDF with both NL3 and G3 for the considered isotopic chains. We find Relativistic-EDF outperforms the Brueckner-EDF in predicting the shell and/or sub-shell closure of neutron-rich isotopes at N = 50 for these atomic nuclei. Moreover, a relative comparison has been made for the results obtained with the non-linear NL3 and G3 parameter sets.

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arXiv2024

Black hole spin estimation of XTE J2012+381 using simultaneous observations of Swift/XRT and NuSTAR

A sufficiently precise measurement of black hole spin is required to carry out quantitative tests of the Kerr metric and to understand several phenomena related to astrophysical black holes. After 24 years, XTE J2012+381 again underwent an outburst in December 2022. In this work, we focused on the measurement of spin and mass of black hole candidate XTE J2012+381 using broadband spectral analysis of X-ray data from \emph{Swift/XRT} and \emph{NuSTAR}. By using the relxillCp model, the spin and inclination of the source were found to be $0.883_{-0.061}^{+0.033}$ and $46.2_{-2.0}^{+3.7}$ degrees, respectively for high disk density ($i.e.\;10^{20}\;\mathrm{cm}^{-3}$). We further test our results for lamp post geometry using the relxilllpCp model. The spin and inclination of the source were found to be $0.892_{-0.044}^{+0.020}$ and $43.1_{-1.2}^{+1.4}$ degrees, respectively. Then "continuum-fitting" method was used for the soft state to estimate the mass of BH and found to be $7.95_{-3.25}^{+7.65}\;\mathrm{M}_{\odot}$ and $7.48_{-2.75}^{+5.80}\;\mathrm{M}_{\odot}$ for the spin and inclination estimated from the relxillCp and relxilllpCp model respectively. We used a distance of 5.4 kpc as measured by Gaia using the parallax method. This study also addresses the issue of supersolar iron abundance in XTE J2012+381 by using \texttt{reflionx} based reflection model and found high disk density for the source.

astro-ph.HE↗

arXiv2024

Nuclear incompressibility and its enduring impact on fusion cross-section

The fusion mechanism of reactions involving even-even $^{112-124}$Sn, doubly magic $^{132}$Sn, $^{208}$Pb as targets, and $^{64}$Ni as the projectile is explored within the relativistic mean field (RMF) formalism. The main aim of choosing these nuclei is to explore the correlation between the nuclear incompressibility and the fusion cross-section. The nucleus-nucleus interaction potential is calculated by folding the axially deformed nuclear densities and the relativistic R3Y nucleon-nucleon (NN) potential obtained for the nonlinear sets of NL3$^*$, hybrid, and NL1, which yield different values for various characteristics of nuclear matter at saturation. The fusion barrier characteristics obtained for different RMF parameterizations are further used to calculate the cross-section within the $\ell$-summed Wong model. We found a decrease in the barrier height and consequently, an increase in the cross-section with a decrease in the incompressibility for all sets of parameters considered. The calculated cross section is satisfactorily consistent with the available experimental data for $^{64}$Ni+$^{208}$Pb system. In contrast, the nuclear potentials obtained for NL3$^*$ and the hybrid parameter sets underestimate the cross-section at below-barrier energies for $^{64}$Ni+$^{112-124,132}$Sn reactions. This discrepancy between the experimental data and the theoretical results for $^{64}$Ni+$^{112-124,132}$Sn reactions can be correlated with the soft behaviour of the Sn isotopes. The compressible nature of Sn-isotopes is inferred to lower the barrier height, which further leads to enhancement of the experimental fusion and/or capture cross-section at below-barrier energies. Thus, the NL1 parameter set with a comparatively soft equation of state (EoS) is observed to be a better choice to describe the sub-barrier nuclear fusion dynamics of reactions involving the Sn-isotopes.

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arXiv2024

Implementation of the microscopic nuclear potential in the coupled channels calculations to study the fusion dynamics of Oxygen based reactions

In the present work, we have incorporated the microscopic relativistic nuclear potential obtained from recently developed relativistic R3Y NN potential in the coupled channels code CCFULL to study the fusion dynamics. The R3Y NN-potential and the densities of interacting nuclei are obtained for the relativistic mean-field approach for the NL3$^*$ parameter set. It is to be noted that the R3Y NN potential can be expressed in terms of masses of the mesons and their couplings by considering the meson degrees of freedom within the relativistic mean field, which has a form similar to the widely used M3Y potential. We focused on the fusion cross-sections for $Oxygen$-based reactions with targets from different mass regions of the periodic table i.e. $^{16}$O + $^{24}$Mg, $^{18}$O + $^{24}$Mg, $^{16}$O + $^{148}$Sm, $^{16}$O + $^{176}$Hf, $^{16}$O + $^{176}$Yb, $^{16}$O + $^{182}$W, and $^{16}$O + $^{186}$W. A comparison is also made with the ones calculated using the nuclear potential obtained from the traditional Woods-Saxon potential and the widely used M3Y NN potential within CCFULL. The coupled channel calculations are performed with shape and rotational degrees of freedom to examine the fusion enhancement at below-barrier energies. It is observed from the calculations that the fusion cross-sections obtained using R3Y NN potential with rotational degrees of freedom are found to be more consistent with the experimental data than those for the M3Y and Woods-Saxon potentials mainly at below barrier energies.

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arXiv2024

Relativistic mean-field study of alpha decay in superheavy isotopes with 100 \texorpdfstring{$\leq$ Z $\leq$}-120

The $\alpha$-decay half-lives of superheavy nuclei with $100 \leq Z \leq 120$ are comprehensively analyzed using the axially deformed relativistic mean field (RMF) formalism for the NL3$^*$ parameter set. We employ RMF binding energies to determine the $\alpha$-decay energies and make a comparison with both the available experimental data and the theoretical results obtained from the global nuclear mass model WS4. The four distinct formulae, specifically the modified scaling law Brown, modified Viola-Seaborg, Yibin {\it et al.} formula, and its modified form are used to calculate the decay half-lives and examine the numerical correlation between the half-life ($T_{1/2}$) for each $\alpha$-decay energy. We notice that $T_{1/2}$ is significantly dependent on the decay formula in terms of isospin asymmetry and decay energy. We also noticed that modified scaling law Brown formula estimates of half-lives agreed comparatively better with the experiment as compared to others. Moreover, the present investigation provides significant information on the stability of the superheavy island considered for ongoing and/or future experiments.

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arXiv2024

Relativistic energy density functional from momentum space to coordinate space within a coherent density fluctuation model

In this theoretical study, we have derived a simplified analytical expression for the binding energy per nucleon as a function of density and isospin asymmetry within the relativistic mean-field model. We have generated a new parameterization for the density-dependent DD-ME2 parameter set using the Relativistic-Hartree-Bogoliubov approach. Moreover, this work attempts to revisit the prior polynomial fitting in [Phy. Rev. C 103, 024305 (2021)] for the non-linear NL3 force parameter to provide a simplified set of equations for the energy density functional which is used for calculating the surface properties of finite nuclei. The current study improves the existing fitting procedure by effectively proposing a simpler model that provides comparably precise results while lowering the computational expense. To study the surface properties of finite nuclei with these parameterizations, we have adopted the coherent density fluctuation model, which effectively translates the quantities of nuclear matter from momentum space to coordinate space at local density. The isospin properties, such as symmetry energy and its surface and volume components, slope parameter, finite nuclear incompressibility, and surface incompressibility for even-even nuclei, are calculated for different mass regions. Moreover, we have studied the effect of density, weight function, and choice of relativistic force parameters on the surface properties. The consequence of this work will help to determine the properties of nuclei along the nuclear landscape and can facilitate an improved understanding of the island of stability, heavy-ion collision, and nucleosynthesis, among others.

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arXiv2024

Study of type-B QPOs observed in black hole X-ray binary Swift J1728.9-3613

We report the detection of type-B quasi-periodic oscillation (QPO) of the black hole X-ray binary Swift J1728.9-3613 observed by NICER during the 2019 outburst. A type- B QPO was observed for the first two days and it disappeared as flux increased, but again appeared at $\sim$ 7.70 Hz when flux was dramatically decreased. The source was found in the soft-intermediate state during these observations. We further studied the energy dependence of the QPO. We found that QPO was observed only for a higher energy range implying that the origin of QPO is possibly due to the corona emitting higher energy photons by the inverse Compton process. The variation of spectral parameters can be explained with the disk truncation model. The fractional rms found to be monotonically increased with energy. The phase lag spectrum followed the U-shaped curve. The rms and phase lag spectrum are modelled and explained with the single-component comptonization model vkompthdk.

astro-ph.HE↗

arXiv2023

Reply to the "Comment on `Effect of density and nucleon-nucleon potential on the fusion cross section within the relativistic mean field formalism'"

In reply to the Comment made by M. V. Chushnyakova et al. on our paper [Phys. Rev. C 101, 044603 (2020)], we argue that the calculations, results and conclusions of our paper remain valid. We have shown here the calculations for one reaction using the deformed densities and the R3Y nucleon-nucleon potential obtained within the relativistic mean-field (RMF) formalism. Suitable clarications and justifications are given to address all the points raised in the Comment.

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