arXiv subjects

Pawan Kumar

Publications and source records attributed to Pawan Kumar.

At least 145 records · Page 8Linked to original sources

arXiv2020

Radiation Forces Constrain the FRB Mechanism

We provide constraints on Fast Radio Burst (FRB) models by careful considerations of radiation forces associated with these powerful transients. We find that the induced-Compton scatterings of the coherent radiation by electrons/positrons accelerate particles to very large Lorentz factors (LF) in and around the source of this radiation. This severely restricts those models for FRBs that invoke relativistic shocks and maser type instabilities at distances less than about $10^{13}$ cm of the neutron star. Radiation traveling upstream, in these models, forces particles to move away from the shock with a LF larger than the LF of the shock front. This suspends the photon generation process after it has been operating for less than ~0.1 ms (observer frame duration). We show that masers operating in shocks at distances larger than $10^{13}$ cm cannot simultaneously account for the burst duration of 1 ms or more and the observed ~1 GHz frequencies of FRBs without requiring an excessive energy budget ($10^{46}$ erg); the energy is not calculated by imposing any efficiency consideration, or other details, for the maser mechanism, but is entirely the result of ensuring that particle acceleration by induced-Compton forces upstream of the shock front does not choke off the maser process. For the source to operate more or less continuously for a few ms, it should be embedded in a strong magnetic field - cyclotron frequency $\gg$ wave frequency - so that radiation forces do not disperse the plasma and shut-off the engine.

astro-ph.HE↗

arXiv2020

Role of individual components of two-nucleon interaction in nuclear matrix elements of $2νββ$ and $0νββ$ of $^\textbf{48}$Ca: Beyond the closure approximation

In the present work, we examine the role of central (C), spin-orbit (SO) and tensor (T) components of two-nucleon interaction in the nuclear matrix elements (NMEs) of the two-neutrino double beta decay ($2νββ$) and the light neutrino-exchange mechanism of neutrinoless double beta decay ($0νββ$) of $^{48}$Ca in closure approximation and nonclosure approach. The NMEs are calculated in the nuclear shell-model framework using two-nucleon effective interaction GXPF1A used for $pf$ shell. The decomposition of the shell model two-nucleon interaction into its individual components is performed using the spin-tensor decomposition (STD). The NMEs for $2νββ$ are calculated in running nonclosure method. The NMEs for $0νββ$ are calculated with four different methods, namely, closure, running closure, running nonclosure, and mixed method. Results show that the magnitude of NMEs for $2νββ$ decreases about 7\% with the C+SO component of the interaction as compared to the C component. The magnitude of NMEs is further decreased about 9\% by adding T component to the C+SO component. The NMEs of $0νββ$ calculated in running nonclosure method are enhanced by about 8-10\%, 8-10\%, and 9-12\%, respectively, as compared to corresponding NMEs calculated in running closure method with C, C+SO components and total (C+SO+T) GXPF1A interaction for different SRC parametrization. For both $2νββ$ and $0νββ$, the NMEs calculated with C+SO component is in opposite phase with the NMEs calculated with C component and the total GXPF1A interaction.

nucl-th↗

arXiv2020

Direct Visualisation of Out-of-Equilibrium Structural Transformations in Atomically-Thin Chalcogenides

Two-dimensional (2D) transition metal dichalcogenides (TMDCs) have been the subject of sustained research interest due to their extraordinary electronic and optical properties. They also exhibit a wide range of structural phases because of the different orientations that the atoms can have within a single layer, or due to the ways that different layers can stack. Here we report the first study of direct-visualization of structural transformations in atomically-thin layers under highly non-equilibrium thermodynamic conditions. We probe these transformations at the atomic scale using real-time, aberration corrected scanning transmission electron microscopy and observe strong dependence of the resulting structures and phases on both heating rate and temperature. A fast heating rate (25 C/sec) yields highly ordered crystalline hexagonal islands of sizes of less than 20 nm which are composed of a mixture of 2H and 3R phases. However, a slow heating rate (25 C/min) yields nanocrystalline and sub-stoichiometric amorphous regions. These differences are explained by different rates of sulfur evaporation and redeposition. The use of non-equilibrium heating rates to achieve highly crystalline and quantum-confined features from 2D atomic layers present a new route to synthesize atomically-thin, laterally confined nanostrucutres and opens new avenues for investigating fundamental electronic phenomena in confined dimensions.

cond-mat.mtrl-sci↗

arXiv2019

Deep Attentive Ranking Networks for Learning to Order Sentences

We present an attention-based ranking framework for learning to order sentences given a paragraph. Our framework is built on a bidirectional sentence encoder and a self-attention based transformer network to obtain an input order invariant representation of paragraphs. Moreover, it allows seamless training using a variety of ranking based loss functions, such as pointwise, pairwise, and listwise ranking. We apply our framework on two tasks: Sentence Ordering and Order Discrimination. Our framework outperforms various state-of-the-art methods on these tasks on a variety of evaluation metrics. We also show that it achieves better results when using pairwise and listwise ranking losses, rather than the pointwise ranking loss, which suggests that incorporating relative positions of two or more sentences in the loss function contributes to better learning.

cs.CL↗

arXiv2019

Linear polarization in gamma-ray burst prompt emission

Despite being hard to measure, GRB prompt $γ$-ray emission polarization is a valuable probe of the dominant emission mechanism and the outflow's composition and angular structure. During the prompt emission the outflow is ultra-relativistic with Lorentz factors $Γ\gg1$. We describe in detail the linear polarization properties of various emission mechanisms: synchrotron radiation from different magnetic field structures (ordered: toroidal $B_{\rm tor}$ or radial $B_\parallel$, and random: normal to the radial direction $B_\perp$), Compton drag, and photospheric emission. We calculate the polarization for different GRB jet angular structures (e.g. top-hat, Gaussian, power-law) and viewing angles $θ_{\rm obs}$. Synchrotron with $B_\perp$ can produce large polarizations, up to $25\%\lesssimΠ\lesssim45\%$, for a top-hat jet but only for lines of sight just outside the jet's sharp edge. The same also holds for Compton drag, albeit with a slightly higher overall $Π$. Moreover, we demonstrate how $Γ$-variations during the GRB or smoother jet edges would significantly reduce $Π$. We construct a semi-analytic model for non-dissipative photospheric emission from structured jets. Such emission can produce up to $Π\lesssim15\%$ with reasonably high fluences, but this requires steep gradients in $Γ(θ)$. A polarization of $50\%\lesssimΠ\lesssim65\%$ can robustly be produced only by synchrotron emission from a transverse magnetic field ordered on angles $\gtrsim\!1/Γ$ around our line of sight (like a global toroidal field). Therefore, such a model would be strongly favored even by a single secure measurement within this range. We find that such a model would also be favored if $Π\gtrsim20\%$ is measured in most GRBs within a large enough sample, by deriving the polarization distribution for our different emission and jet models.

astro-ph.HE↗

arXiv2019

On the Use of Fast Radio Burst Dispersion Measures as Distance Measures

Fast radio bursts appear to be cosmological signals whose frequency-time structure provides a dispersion measure. The dispersion measure is a convolution of the cosmic distance element and the electron density, and contains the possibility of using these events as new cosmological distance measures. We explore the challenges of extracting the distance in a robust manner, and give quantitative estimates for the systematics control needed for fast radio bursts to become a competitive distance probe. The methodology can also be applied to assessing their use for mapping electron density fluctuations or helium reionization.

astro-ph.CO↗

arXiv2019

Explaining GRB prompt emission with sub-photospheric dissipation and Comptonization

Even though the observed spectra for GRB prompt emission is well constrained, no single radiation mechanism can robustly explain its distinct non-thermal nature. Here we explore the radiation mechanism with the photospheric emission model using our Monte Carlo Radiative Transfer (MCRaT) code. We study the sub-photospheric Comptonization of fast cooled synchrotron photons while the Maxwellian electrons and mono-energetic protons are accelerated to relativistic energies by repeated dissipation events. Unlike previous simulations, we implement a realistic photon to electron number ratio $N_γ/N_{e} \sim 10^5$ consistent with the observed radiative efficiency of a few percent. We show that it is necessary to have a critical number of episodic energy injection events $N_{rh,cr} \sim {\rm few}\ 10{\rm s}-100$ in the jet in addition to the electron-proton Coulomb coupling in order to inject sufficient energy $E_{inj,cr} \sim 2500-4000\ m_e c^2$ per electron and produce an output photon spectrum consistent with observations. The observed GRB spectrum can be generated when the electrons are repeatedly accelerated to highly relativistic energies $γ_{e,in} \sim {\rm few}\ 10{\rm s}-100$ in a jet with bulk Lorentz factor $Γ\sim 30-100$, starting out from moderate optical depths $τ_{in} \sim 20-40$. The shape of the photon spectrum is independent of the initial photon energy distribution and baryonic energy content of the jet and hence independent of the emission mechanism, as expected for photospheric emission.

astro-ph.HE↗

arXiv2019

Role of Neutron Transfer in Sub-Barrier Fusion

Fusion excitation function of $^{35}$Cl + $^{130}$Te system is measured in the energy range around the Coulomb barrier and analyzed in the framework of the coupled-channels approach. The role of projectile deformation, nuclear structure, and the couplings of inelastic excitations and positive Q$-$value neutron transfer channels in sub-barrier fusion are investigated through the comparison of reduced fusion excitation functions of $^{35,37}$Cl +$^{130}$Te systems. The reduced fusion excitation function of $^{35}$Cl + $^{130}$Te system shows substantial enhancement over $^{37}$Cl + $^{130}$Te system in sub-barrier energy region which is attributed to the presence of positive Q-value neutron transfer channels in $^{35}$Cl + $^{130}$Te system. Findings of this work strongly suggest the importance of +2$n$ - transfer coupling in sub-barrier fusion apart from the simple inclusion of inelastic excitations of interacting partners, and are in stark contrast with the results presented by Kohley \textit{et al.}, [Phys. Rev. Lett. 107, 202701 (2011)].

nucl-ex↗

arXiv2019

The Emission Mechanism of Gamma-Ray Bursts: Identification via Optical-IR Slope Measurements

There is no consensus on the emission mechanism of $γ$-ray bursts (GRBs). A synchrotron model can produce $γ$-ray spectra with the empirical Band function form, from a piece-wise two-power-law electron energy distribution (2EPLS). This model predicts that for the same $γ$-ray spectrum, optical emission can be very different in $f_ν$ log slope, and in flux relative to $γ$-rays,depending on model parameter values. The model only allows a small set of $f_ν$ log slopes in the optical -thereby allowing a clear path to verification or falsification. Measurements of prompt GRB emission in the optical thus far give no useful information about the spectral shape within the band, and therefore cannot be used to evaluate such predictions. We describe an experiment that responds to GRB alerts with a fast-slewing telescope, with 3+ simultaneous, high-time resolution cameras. Three channels measure two slopes in order to evaluate the model. We propose cross-correlation of $γ$ and OIR light curves to verify that GRB are single-component dominated, or to quantify additional contributions. Previous CCD measurements have limited-time resolution due to read noise. Electron-multiplied CCDS (EMCCDs) can be used to greatly reduce read noise allowing exposure times of a few hundred ms. Our Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) utilizes a 70 cm telescope that can point in $\le$ 8 s, with 3 optical channels. The NUTTelA-TAO is expected to measure 3-8 GRB/yr, and verify/refute the 2EPLS model with just a few bright GRBs. A space-based experiment with an IR channel would make improved measurements of the self-absorption frequency and physical conditions within the GRB jet. Additional science includes detection of dust evaporation due to GRBs, a tool to study progenitor environment dust.

astro-ph.HE↗

arXiv2019

Thermal Expansion Coefficient and Phonon Dynamics in Coexisting Allotropes of Monolayer WS2 Probed by Raman Scattering

We report a comprehensive temperature dependent Raman measurements on three different phases of monolayer WS2 from 4K to 330K in a wide spectral range. Our studies revels the anomalous nature of the first as well as the higher order combination modes reflected in the disappearance of the few modes and anomalous temperature evaluation of the phonon self-energy parameters attributed to the detuning of resonance condition and development of strain due to thermal expansion mismatch with the underlying substrate. Our detailed temperature dependence studies also decipher the ambiguity about assignment of the two modes in literature near ~ 297 cm-1 and 325 cm-1. Mode near 297 cm-1 is assigned as first order Raman mode, which is forbidden in the backscattering geometry and 325 cm-1 is assigned to the combination of and mode. We also estimated thermal expansion coefficient by systematically disentangling the substrate effect in the temperature range of 4K to 330K and probed its temperature dependence in 1H, 1T and 1T' phases.

cond-mat.mtrl-sci↗

arXiv2019

Mergers of black hole-neutron star binaries and rates of associated electromagnetic counterparts

Black hole-neutron star (BHNS) binaries are amongst promising candidates for the joint detection of electromagnetic (EM) signals with gravitational waves (GWs) and are expected to be detected in the near future. Here we study the effect of the BHNS binary parameters on the merger ejecta properties and associated EM signals. We estimate the remnant disk and unbound ejecta masses for BH mass and spin distributions motivated from the observations of transient low-mass X-ray binaries (LMXBs) and specific NS equation of state (EoS). The amount of r-process elements synthesised in BHNS mergers is estimated to be a factor of $\sim 10^{2}-10^{4}$ smaller than BNS mergers, due to the smaller dynamical ejecta and merger rates for the former. We compute the EM luminosities and light curves for the early- and late-time emissions from the ultra-relativistic jet, sub-relativistic dynamical ejecta and wind, and the mildly-relativistic cocoon for typical ejecta parameters. We then evaluate the low-latency EM follow-up rates of the GW triggers in terms of the GW detection rate $\dot{N}_{GW}$ for current telescope sensitivities and typical BHNS binary parameters to find that most of the EM counterparts are detectable for high BH spin, small BH mass and stiffer NS EoS when NS disruption is significant. Based on the relative detection rates for given binary parameters, we find the ease of EM follow-up to be: ejecta afterglow $>$ cocoon afterglow $\gtrsim$ jet prompt $>$ ejecta macronova $>$ cocoon prompt $>$ jet afterglow $>>$ wind macronova $>>$ wind afterglow.

astro-ph.HE↗

arXiv2019

Catching Element Formation In The Act

Gamma-ray astronomy explores the most energetic photons in nature to address some of the most pressing puzzles in contemporary astrophysics. It encompasses a wide range of objects and phenomena: stars, supernovae, novae, neutron stars, stellar-mass black holes, nucleosynthesis, the interstellar medium, cosmic rays and relativistic-particle acceleration, and the evolution of galaxies. MeV gamma-rays provide a unique probe of nuclear processes in astronomy, directly measuring radioactive decay, nuclear de-excitation, and positron annihilation. The substantial information carried by gamma-ray photons allows us to see deeper into these objects, the bulk of the power is often emitted at gamma-ray energies, and radioactivity provides a natural physical clock that adds unique information. New science will be driven by time-domain population studies at gamma-ray energies. This science is enabled by next-generation gamma-ray instruments with one to two orders of magnitude better sensitivity, larger sky coverage, and faster cadence than all previous gamma-ray instruments. This transformative capability permits: (a) the accurate identification of the gamma-ray emitting objects and correlations with observations taken at other wavelengths and with other messengers; (b) construction of new gamma-ray maps of the Milky Way and other nearby galaxies where extended regions are distinguished from point sources; and (c) considerable serendipitous science of scarce events -- nearby neutron star mergers, for example. Advances in technology push the performance of new gamma-ray instruments to address a wide set of astrophysical questions.

astro-ph.HE↗

arXiv2019

Nanoparticles modulate contact angle hysteresis in electrowetting

The pinning of the contact line adversely influences the electrowetting performance of sessile liquid droplets. In this paper, we report the electrowetting hysteresis characteristics of 100 mM aq. KCl sessile liquid droplet placed on a hydrophobic PDMS surface. The effect of nanoparticles on the contact angle hysteresis under the imposed electric potential is further investigated. This study reveals that the contact angle hysteresis decreases beyond a certain threshold value of nanoparticles concentration. Therefore, nanoparticle suspension in the liquid droplet can be used to enhance or suppress the electrowetting hysteresis and consequentially rate of heat transfer during hot spot cooling.

cond-mat.soft↗

arXiv2018

Fast radio burst source properties from polarization measurements

Recent polarization measurements of fast radio bursts (FRBs) provide new insights on these enigmatic sources. We show that the nearly 100% linear polarization and small variation of the polarization position angles (PAs) of multiple bursts from the same source suggest that the radiation is produced near the surface of a strongly magnetized neutron star. As the emitted radiation travels through the magnetosphere, the electric vector of the X-mode wave adiabatically rotates and stays perpendicular to the local magnetic field direction. The PA freezes at a radius where the plasma density becomes too small to be able to turn the electric vector. At the freeze-out radius, the electric field is perpendicular to the magnetic dipole moment of the neutron star projected in the plane of the sky, independent of the radiation mechanism or the orientation of the magnetic field in the emission region. We discuss a number of predictions of the model. The variation of PAs from repeating FRBs should follow the rotational period of the underlying neutron star (but the burst occurrence may not be periodic). Measuring this period will provide crucial support for the neutron star nature of the progenitors of FRBs. For FRB 121102, the small range of PA variation means that the magnetic inclination angle is less than about 20 degrees and that the observer's line of sight is outside the magnetic inclination cone. Other repeating FRBs may have a different range of PA variation from that of FRB 121102, depending on the magnetic inclination and the observer's viewing angle.

astro-ph.HE↗

arXiv2018

Electrowetting of a nano-suspension on a soft solid

The wetting of solid surfaces can be manoeuvred by altering the energy balance at the interfacial region. While electric field acts favourably to spread a droplet on a rigid surface, this tendency may be significantly suppressed over soft surfaces, considering a part of the interfacial energy being utilized to deform the solid elastically by capillary forces. Here, we bring out a unique mechanism by virtue of which addition of nano-particles to the droplet brings in a favourable recovery of the electro-spreading characteristics of a soft surface, by realizing an alteration in the effective dielectric constant of the interfacial region. Our experiments further demonstrate that this mechanism ceases to be operative beyond a threshold volume fraction of the particle suspension, due to inevitable contact line pinning. We also develop a theory to explain our experimental observations. Our findings provide a non-contact mechanism for meniscus spreading and droplet control, bearing far-reaching implications in biology and engineering.

cond-mat.soft↗

arXiv2018

The maximum luminosity of fast radio bursts

Under the assumption that fast radio bursts (FRBs) are from coherent curvature emission powered by the dissipation of magnetic energy in the magnetosphere of neutron stars, we predict a maximum isotropic equivalent luminosity of (~2x10^{47} erg/s) min(ρ^2, Bρ^{4/3}ν^{-2/3}), where ρ is the curvature radius of the magnetic field lines near the source region in units of 10 km, B is the local magnetic field strength in units of 10^{16} G, and ν is the FRB wave frequency in units of GHz. This is because the electric field responsible for accelerating the radiating particles becomes close to the quantum critical field strength and is then quickly shielded by Schwinger pairs within a nano-second. Future observations should be able to confirm this cut-off luminosity and hence provide a unique probe of the source location and magnetic field strength. We discuss how the maximum luminosity affects the observed flux distributions for repeating bursts from the same object and for the entire FRB population.

astro-ph.HE↗

arXiv2018

Polymer morphology and interfacial charge transfer dominate over energy-dependent scattering in organic-inorganic thermoelectrics

Hybrid (organic-inorganic) materials have emerged as a promising class of thermoelectric materials, achieving power factors exceeding those of either constituent. The mechanism of this enhancement is still under debate, and pinpointing the underlying physics has proven difficult. In this work, we combine transport measurements with theoretical simulations and first principles calculations on a prototypical PEDOT:PSS-Te(Cux) nanowire hybrid material system to understand the effect of templating and charge redistribution on the thermoelectric performance. Further, we apply the recently developed Kang-Snyder charge transport model to show that scattering of holes in the hybrid system, defined by the energy-dependent scattering parameter, remains the same as in the host polymer matrix; performance is instead dictated by polymer morphology manifested in an energy-independent transport coefficient. We build upon this language to explain thermoelectric behavior in a variety of PEDOT and P3HT based hybrids acting as a guide for future work in multiphase materials.

cond-mat.mtrl-sci↗

arXiv2018

On the Missing Energy Puzzle of Tidal Disruption Events

For the majority of the tidal disruption event (TDE) candidates, the observed energy in the optical/near-UV bands is of order 10^{51} erg. We show that this observed energy is smaller than the minimum bolometric energy for the radiative inefficient accretion flow model by a factor of 10-100. We argue that this discrepancy is because the majority of the energy released is in the extreme-UV (EUV) band and/or in the form of relativistic jets beamed away from the Earth. The EUV scenario is supported by existing mid-infrared data and should be further tested by future dust reverberation observations. The jet scenario is disfavored by the radio observations of ASASSN-14li but may still be viable for other TDE candidates. We also provide evidence that, at least for some TDEs, most of the missing energy (in the EUV and/or in the form of jets) is released within a few times the orbital period of the most tightly bound material, which means (1) the circularization of the fallback stream may occur rapidly, and (2) the luminosity of the accretion flow or the jet power may not be capped near the Eddington level when the fallback rate is super-Eddington. For most other TDEs, this energy-release timescale is currently not strongly constrained.

astro-ph.HE↗