arXiv subjects

A. K. Srivastava

Publications and source records attributed to A. K. Srivastava.

At least 55 records · Page 3Linked to original sources

arXiv2018

Propagation of MRT Unstable Plasma Spikes in the Inter-planetary Space

We have used the Coronagraphic and Heliospheric Imaging data from Solar TErrestrial RElations Observatory (STEREO) to observe a prominence which is erupted on June 7th, 2011. This prominence is subjected to the morphological evolution of MRT instability from the lower solar corona upto the inter-planetary space. The unstable structures are converted into the bunch of localized plasma spikes due to the turbulent mixing, and propagate in the inter-planetary space upto 1 A.U.

astro-ph.SR↗

arXiv2018

Super Penumbral Chromospheric Flare

We observed a C-class flare at the outer boundary of the super-penumbra of a sunspot. The flare was triggered by an emerging magnetic bipolar region that was obliquely oriented with respect to the super-penumbral fibrils. The flare started due to the low height magnetic reconnection of emerging magnetic flux with super-penumbral field resulting hot multi-temperature plasma flows in the inverse Evershed flow channel and its overlying atmosphere. The inverse Evershed flows in the chromosphere start from super penumbra towards sunspot that end at the outer boundary of the penumbra. The hot plasma flow towards the sunspot in the inverse Evershed channels show about 10 km s$^{-1}$ higher velocity in H$α$ wavelengths compared to the plasma emissions at various temperatures as seen in different AIA filters. Even though these velocities are about seven times higher than the typical inverse-Evershed flow speeds, the flow is diminished at the outer boundary of the sunspot's penumbra. This suggests that the super-penumbral field lines that carry the inverse Evershed flows, are discontinued at the boundary where the penumbral field lines dive into the sun and these two sets of field lines are completely distinct. The discontinuity in the typical magnetic field and plasma properties at the adjoining of these two sets of field lines further leads the discontinuity in the characteristic magnetoacoustic and Alfvén speeds, therefore, stopping the plasma flows further on. The multi-temperature plasma in the inverse Evershed channels exhibits \textbf{possible} longitudinal oscillations initially during the onset of the flare, and later flows towards the sunspot. In the multi-temperature view, the different layers above the flare region have the mixture of supersonic as well as subsonic flows.

astro-ph.SR↗

arXiv2018

C-1.4 Class Flare and An Associated Peculiar Coronal Jet

Using HINODE/XRT, GOES, SDO/AIA observations, we study a compact C-1.4 class flare outside a major sunspot of AR 12178 on 4 October 2014. This flare is associated with a peculiar coronal jet, which is erupted in two stages in the overlying corona above the compact flaring region. At the time of flare maximum, the first stage of the jet eruption occurs above the flare energy release site, and thereafter in the second stage its magneto-plasma system interacts with the overlying distinct magnetic field domain in its vicinity to build further the typical jet plasma column.

astro-ph.SR↗

arXiv2018

Rotating Network Jets in the quiet Sun as Observed by IRIS

Aims. We perform a detailed observational analysis of network jets to understand their kinematics, rotational motion and underlying triggering mechanism(s). We have analyzed the quiet-Sun (QS) data. Methods. IRIS high resolution imaging and spectral observations (SJI: Si iv 1400.0 Å, Raster: Si iv 1393.75 Å) are used to analyze the omnipresent rotating network jets in the transition-region (TR). In addition, we have also used Atmospheric Imaging Assembly (AIA) onboard Solar Dynamic Observation (SDO) observations. Results. The statistical analysis of fifty-one network jets is performed to understand various their mean properties, e.g., apparent speed (140.16+/-39.41 km/s), length (3.16+/-1.18 Mm), lifetimes (105.49+/-51.75 s). The Si iv 1393.75 Åline has secondary component along with its main Gaussian, which is formed due to the high-speed plasma flows (i.e., network jets). The variation of Doppler velocity across these jets (i.e., blue shift on one edge and red shift on the other) signify the presence of inherited rotational motion. The statistical analysis predicts that the mean rotational velocity (i.e., \delV) is 49.56 km/s. The network jets have high angular velocity in comparison to the other class of solar jets. Conclusions. The signature of network jets are inherited in TR spectral lines in terms of the secondary component of the Si iv 1393.75 Åline. The rotational motion of network jets is omnipresent, which is reported firstly for this class of jet-like features. The magnetic reconnection seems to be the most favorable mechanism for the formation of these network jets.

astro-ph.SR↗

arXiv2018

First Evidence of the Frequency Filtering of Magnetoacoustic Waves in the Flaring Star EK Dra

Using the data obtained from XMM-Newton, we show the gradual evolution of two periodicities of ~4500 s and ~2200 s in the decay phase of the flare observed in a solar analog EK Dra. The longer period evolves firstly for first 14 ks, while the shorter period evolves for next 10 ks in the decay phase. We find that these two periodicities are associated with the magnetoacoustic waves triggered in the flaring region. The flaring loop system shows cooling and thus it is subjected to the change in the scale height and the acoustic cut-off period. This serves to filter the longer period magnetoacoustic waves and enables the propagation of the shorter period waves in the later phase of the flare. We provide the first clues of the dynamic behaviour of EK Dra's corona which affects the propagation of waves and causes their filtering.

astro-ph.SR↗

arXiv2018

Evolution of Magnetic Rayleigh-Taylor Instability into the Outer Solar Corona and Low Inter Planetary Space

We analyze the observations from Solar TErrestrial RElations Observatory (STEREO)-A\&B/COR-1 of an eruptive prominence in the intermediate corona on 7 June 2011 at 08:45 UT, which consists of magnetic Rayleigh-Taylor (MRT) unstable plasma segments. Its upper northward segment shows spatio-temporal evolution of MRT instability in form of finger structures upto the outer corona and low inter-planetary space. Using method of Dolei et al.(2014), It is estimated that the density in each bright finger is greater than corresponding dark region lying below of it in the surrounding intermediate corona. The instability is evolved due to wave perturbations that are parallel to the magnetic field at the density interface. We conjecture that the prominence plasma is supported by tension component of the magnetic field against gravity. Using linear stability theory, magnetic field is estimated as 21-40 mG to suppress growth of MRT in the observed finger structures. In the southward plasma segment, a horn-like structure is observed at 11:55 UT in the intermediate corona that also indicates MRT instability. Falling blobs are also observed in both the plasma segments. In the outer corona upto 6-13 solar radii, the mushroom-like plasma structures have been identified in the upper northward MRT unstable plasma segment using STEREO-A/COR-2. These structures most likely grew due to the breaking and twisting of fingers at large spatial scales in weaker magnetic fields. In the lower inter-planetary space upto 20 solar radii, these structures are fragmented into various small-scale localized plasma spikes most likely due to turbulent mixing.

astro-ph.SR↗

arXiv2017

Robust broad spectral photodetection (UV-NIR) and ultra high responsivity investigated in nanosheets and nanowires of Bi2Te3 under harsh nano-milling conditions

Due to miniaturization of device dimensions, the next generations photodetector based devices are expected to be fabricated from robust nanostructured materials. Hence there is an utmost requirement of investigating exotic optoelectronic properties of nanodevices fabricated from new novel materials and testing their performances at harsh conditions. The recent advances on 2D layered materials indicate exciting progress on broad spectral photodetection (BSP) but still there is a great demand for fabricating ultra-high performance photodetectors made from single material sensing broad electromagnetic spectrum since the detection range 325 nm to 1550 nm is not covered by the conventional Si or InGaAs photodetectors. Alternatively, Bi2Te3 is a layered material, possesses exciting optoelectronic, thermoelectric, plasmonics properties. Here we report robust photoconductivity measurements on Bi2Te3 nanosheets and nanowires demonstrating BSP from UV to NIR. The nanosheets of Bi2Te3 show the best ultra-high photoresponsivity (~74 A/W at 1550 nm ). Further these nanosheets when transform into nanowires using harsh FIB milling conditions exhibit about one order enhancement in the photoresponsivity without affecting the performance of the device even after 4 months of storage at ambient conditions. An ultra-high photoresponsivity and BSP indicate exciting robust nature of topological insulator based nanodevices for optoelectronic applications.

cond-mat.mtrl-sci↗

arXiv2017

X-ray photoelectron spectroscopy, Magnetotransport and Magnetization study of Nb2PdS5 superconductor

In the present report, we investigate various properties of the Nb2PdS5 superconductor. Scanning electron microscopy displayed slabs like laminar growth of Nb2PdS5while X-ray photoelectron spectroscopy exhibited the hybridization of Sulphur (2p) with both Palladium (3d)and Niobium (3d). High field (140kOe) magneto-transport measurements revealed that superconductivity (Tc onset =7K and Tc R = 0 = 6.2K) of the studied Nb2PdS5material is quite robust against magnetic field with the upper critical field (Hc2) outside the Pauli paramagnetic limit. Thermally activated flux flow (TAFF) of the compound showed that resistivity curves follow Arrhenius behaviour. The activation energy for Nb2PdS5 is found to decrease from 15.15meV at 10kOe to 2.35meV at 140kOe. Seemingly, the single vortex pinning is dominant in low field regions, while collective pinning is dominant in high field region. The temperature dependence of AC susceptibility confirmed the Tc at 6K, further varying amplitude and frequency showed well coupled granular nature of superconductivity. The lower critical field (Hc1) is extracted from DC magnetisation measurements at various T below Tc. It is found that Hc1(T) of Nb2PdS5 material seemingly follows the multiband nature of superconductivity.

cond-mat.supr-con↗

arXiv2017

A Study of a long duration B9 flare-CME event and associated piston-driven shock

We present and discuss here the observations of a small long duration GOES B- class flare associated with a quiescent filament eruption, a global EUV wave and a CME on 2011 May 11. The event was well observed by the Solar Dynamics Observatory (SDO), GONG Hα, STEREO and HiRAS spectrograph. As the fil- ament erupted, ahead of the filament we observed the propagation of EIT wave fronts, as well as two flare ribbons on both sides of the polarity inversion line (PIL) on the solar surface. The observations show the co-existence of two types of EUV waves, i.e., a fast and a slow one. A type II radio burst with up to the third harmonic component was also associated with this event. The evolution of pho- tospheric magnetic field showed flux emergence and cancellation at the filament site before its eruption.

astro-ph.SR↗

arXiv2017

Magnetic swirls and associated fast magnetoacoustic kink waves in a solar chromospheric flux tube

We perform numerical simulations of impulsively generated magnetic swirls in an isolated flux tube which is rooted in the solar photosphere. These swirls are triggered by an initial pulse in a horizontal component of the velocity. The initial pulse is launched either: (a) centrally, within the localized magnetic flux tube; or (b) off-central, in the ambient medium. The evolution and dynamics of the flux tube is described by three-dimensional, ideal magnetohydrodynamic equations. These equations are numerically solved to reveal that in case (a) dipole-like swirls associated with the fast magnetoacoustic kink and $m=1$ Alfvén waves are generated. In case (b), the fast magnetoacoustic kink and $m=0$ Alfvén modes are excited. In both these cases, the excited fast magnetoacoustic kink and Alfvén waves consist of similar flow pattern and magnetic shells are also generated with clockwise and counter-clockwise rotating plasma within them, which can be the proxy of dipole-shaped chromospheric swirls. The complex dynamics of vortices and wave perturbations reveals the channelling of sufficient amount of energy to fulfill energy losses in the chromosphere ($\sim$ 10$^{4}$ W m$^{-1}$) and in the corona ($\sim$ 10$^{2}$ W m$^{-1}$). Some of these numerical findings are reminiscent of signatures in recent observational data.

astro-ph.SR↗

arXiv2017

Fabrication of plasmonic surface relief gratings for the application of band-pass filter in UV-Visible spectral range

The measured experimental results of optical diffraction of 10, 5 and 3.4 micrometer period plasmonic surface relief grating are presented for the application of band-pass filter in visible spectral range. Conventional scanning electron microscopic (SEM) is used to fabricate the grating structures on the silver halide based film (substrate) by exposing the electron beam in raster scan fashion. Morphological characterization of the gratings is performed by atomic force microscopy (AFM) shows that the period, height and profile depends on the line per frame, beam spot, single line dwell time, beam current, and accelerating voltage of the electron beam. Optical transmission spectra of 10 micrometer period grating shows a well-defined localized surface plasmon resonance (LSPR) dip at ~366 nm wavelength corresponding to gelatin embedded silver nanoparticles of the grating structure. As the period of the grating reduces LSPR dip becomes prominent. The maximum first order diffraction efficiency (DE) and bandwidth for 10 micrometer period grating are observed as 4% and 400 nm in 350 nm to 800 nm wavelength range respectively. The DE and bandwidth are reduced up to 0.03% and 100 nm for 3.4 micrometer period grating. The profile of DE is significantly flat within the diffraction bandwidth for each of the gratings. An assessment of the particular role of LSPR absorption and varied grating period in the development of the profile of first order DE v/s wavelength are studied. Fabrication of such nano-scale structures in a large area using conventional SEM and silver halide based films may provide the simple and efficient technique for various optical devices applications.

physics.app-ph↗

arXiv2017

Active Longitude and Coronal Mass Ejection Occurrences

The spatial inhomogeneity of the distribution of coronal mass ejection (CME) occurrences in the solar atmosphere could provide a tool to estimate the longitudinal position of the most probable CME-capable active regions in the Sun. The anomaly in the longitudinal distribution of active regions themselves is often referred to as active longitude (AL). In order to reveal the connection between the AL and CME spatial occurrences, here we investigate the morphological properties of active regions. The first morphological property studied is the separateness parameter, which is able to characterize the probability of the occurrence of an energetic event, such as a solar flare or CME. The second morphological property is the sunspot tilt angle. The tilt angle of sunspot groups allows us to estimate the helicity of active regions. The increased helicity leads to a more complex buildup of the magnetic structure and also can cause CME eruption. We found that the most complex active regions appear near the AL and that the AL itself is associated with the most tilted active regions. Therefore, the number of CME occurrences is higher within the AL. The origin of the fast CMEs is also found to be associated with this region. We concluded that the source of the most probably CME-capable active regions is at the AL. By applying this method, we can potentially forecast a flare and/or CME source several Carrington rotations in advance. This finding also provides new information for solar dynamo modeling.

astro-ph.SR↗

arXiv2017

Flux free growth of superconducting FeSe single crystals

We report flux free growth of superconducting FeSe single crystals by an easy and versatile high temperature melt and slow cooling method for first time. The room temperature XRD on the surface of the piece of such obtained crystals showed single 101 plane of Beta-FeSe tetragonal phase. The bulk powder XRD, being obtained by crushing the part of crystal chunk showed majority tetragonal and minority FeSe hexagonal crystalline phases. Detailed HRTEM images along with SAED (selected area electron diffraction) showed the abundance of both majority and minority FeSe phases. Both transport (RT) and magnetization (MT) exhibited superconductivity at below around 10K. Interestingly, the magnetization signal of these crystals is dominated by the magnetism of minority magnetic phase, and hence the isothermal magnetization (MH) at 4K was seen to be ferromagnetic (FM) like. Transport (R-T) measurements under magnetic field showed superconductivity onset at below 12K, and R = 0 (Tc) at 9K. Superconducting transition temperature (Tc) decreases with applied field to around 6K at 7Tesla, with dTc/dH of 0.4K/Tesla, giving rise to an Hc2 value of around 50 Tesla, 30 Tesla and 20 Tesla for Rn = 90, 50 and 10 percent respectively. FeSe single crystal activation energy is calculated from Thermally Activated Flux Flow (TAFF) model which is found to decreases with field.

cond-mat.supr-con↗

arXiv2017

Superconductivity at 5.5 K in Nb2PdSe5 compound

We report superconductivity in as synthesized Nb2PdSe5, which is similar to recently discovered Nb2PdS5 compound having very high upper critical field, clearly above the Pauli paramagnetic limit [Sci. Rep. 3, 1446 (2013)]. A bulk polycrystalline Nb2PdSe5 sample is synthesized by solid state reaction route in phase pure structure. The structural characterization has been done by X ray diffraction, followed by Rietveld refinements, which revealed that Nb2PdSe5 sample is crystallized in monoclinic structure with in space group C2/m. Structural analysis revealed the formation of sharing of one dimensional PdSe2 chains. Electrical and magnetic measurements confirmed superconductivity in Nb2PdSe5 compound at 5.5K. Detailed magneto-resistance results, exhibited the value of upper critical field to be around 8.2Tesla. The estimated Hc2(0) is within Pauli Paramagnetic limit, which is unlike the Nb2PdS5.

cond-mat.supr-con↗

arXiv2016

Observation of quantum oscillations in FIB fabricated nanowires of topological insulator (Bi2Se3)

Since last few years, research based on topological insulators (TI) is in great interests due to intrinsic exotic fundamental properties and future potential applications such as quantum computers or spintronics. The fabrication of TI nanodevices and study on their transport properties mostly focused on high quality crystalline nanowires or nanoribbons. Here we report robust approach of Bi2Se3 nanowire formation from deposited flakes using ion beam milling method. The fabricated Bi2Se3 nanowire devices have been employed to investigate the robustness of topological surface state (TSS) to gallium ion doping and any deformation in the material due to fabrication tools. We report the quantum oscillations in magnetoresistance curves under the parallel magnetic field. The resistance versus magnetic field curves have been studied and compared with Aharonov-Bohm (AB) interference effects which further demonstrate the transport through TSS. The fabrication route and observed electronic transport properties indicate clear quantum oscillations and can be exploited further in studying the exotic electronic properties associated with TI based nanodevices.

cond-mat.mtrl-sci↗

arXiv2016

Transverse oscillations in a coronal loop triggered by a jet

We detect and analyse transverse oscillations in a coronal loop, lying at the south east limb of the Sun as seen from the \textit{Atmospheric Imaging Assembly} (AIA) onboard \textit{Solar Dynamics Observatory} (SDO). The jet is believed to trigger transverse oscillations in the coronal loop. The jet originates from a region close to the coronal loop on 19$^{\rm th}$ September 2014 at 02:01:35 UT. The length of the loop is estimated to be between 377-539~Mm. Only one complete oscillation is detected with an average period of about $32\pm5$~min. Using MHD seismologic inversion techniques, we estimate the magnetic field inside the coronal loop to be between $2.68 -4.5$~G. The velocity of the hot and cool components of the jet is estimated to be 168~km~s$^{-1}$ and 43~km~s$^{-1}$, respectively. The energy density of the jet is found to be greater than the energy density of the oscillating coronal loop. Therefore, we conclude that the jet {triggered} transverse oscillations in the coronal loop. To our knowledge, this is the first coronal loop seismology study using the properties of a jet propagation {to trigger} oscillations.

astro-ph.SR↗

arXiv2016

Simultaneous longitudinal and transverse oscillation in an active filament

We report on the co-existence of longitudinal and transverse oscillations in an active filament. On March 15$^{th}$ 2013, a M1.1 class flare was observed in the active region AR 11692. A CME was found to be associated with the flare. {The CME generated a shock wave that triggered the oscillations in a nearby filament}, situated at the south-west of the active region as observed from National Solar Observatory (NSO)\textit{Global Oscillation Network Group}(GONG) H$α$ images. In this work we report the longitudinal oscillations in the two ends of the filament, co-existing with the transverse oscillations. We propose a scenario in which {an} incoming shock wave hits the filament obliquely and triggers both longitudinal and transverse oscillations. Using the observed parameters, we estimate the lower limit of the magnetic field strength. We use simple pendulum model with gravity as the restoring force to estimate the radius of curvature. We also calculate the mass accretion rate which causes the filament motions to damp quite fast.

astro-ph.SR↗

arXiv2016

Blowout Jets and Impulsive Eruptive Flare in a Bald-Patch Topology

Context: A subclass of broad EUV and X-ray jets, called blowout jets, have become a topic of research since they could be the link between standard collimated jets and CMEs.} Aim: Our aim is to understand the origin of a series of broad jets, some accompanied by flares and associated with narrow and jet-like CMEs. Methods: We analyze observations of a series of recurrent broad jets observed in AR 10484 on 21-24 October 2003. In particular, one of them occurred simultaneously with an M2.4 flare on 23 October at 02:41 UT (SOLA2003-10-23). Both events were observed by ARIES H-alpha Solar Tower-Telescope, TRACE, SOHO, and RHESSI instruments. The flare was very impulsive and followed by a narrow CME. A local force-free model of AR 10484 is the basis to compute its topology. We find bald patches (BPs) at the flare site. This BP topology is present for at least two days before. Large-scale field lines, associated with the BPs, represent open loops. This is confirmed by a global PFSS model. Following the brightest leading edge of the H-alpha and EUV jet emission, we can temporarily associate it with a narrow CME. Results: Considering their characteristics, the observed broad jets appear to be of the blowout class. As the most plausible scenario, we propose that magnetic reconnection could occur at the BP separatrices forced by the destabilization of a continuously reformed flux rope underlying them. The reconnection process could bring the cool flux-rope material into the reconnected open field lines driving the series of recurrent blowout jets and accompanying CMEs. Conclusions: Based on a model of the coronal field, we compute the AR 10484 topology at the location where flaring and blowout jets occurred from 21 to 24 October 2003. This topology can consistently explain the origin of these events.

astro-ph.SR↗