Crystal growth and magneto-transport of Bi2Se3 single crystals

In this letter, we report on the growth and characterization of bulk Bi2Se3 single crystals. The studied Bi2Se3 crystals are grown by the self-flux method through the solid-state reaction from high-temperature (950 °C) melt of constituent elements and slow cooling (2 °C/h). The resultant crystals are shiny and grown in the [00l] direction, as evidenced from surface XRD. Detailed Reitveld analysis of powder X-ray diffraction (PXRD) of the crystals showed that these are crystallized in the rhombohedral crystal structure with a space group of R3m (D5), and the lattice parameters are a = 4.14 (2), b = 4.14 (2), and c = 28.7010 (7) A° . Temperature versus resistivity (ρ − T ) plots revealed metallic conduction down to 2 K, with typical room temperature resistivity (ρ300 K) of around 0.53 mΩ- cm and residual resistivity (ρ0 K) of 0.12 mΩ-cm. Resistivity under magnetic field [ρ(T )H] measurements exhibited large+ve magneto-resistance right from 2 to 200 K. Isothermal magneto-resistance [ρH] measurements at 2, 100, and 200 K exhibited magneto-resistance (MR) of up to 240 %, 130 %, and 60 %, respectively, at 14 T. Further, the MR plots are nonsaturating and linear with the field at all temperatures. At 2 K, the MR plots showed clear quantum oscillations at above say 10 T applied field. Also, the Kohler plots, i.e., Δρ/ρo versus B/ρ, were seen consolidating on one plot. Interestingly, the studied Bi2Se3 single crystal exhibited the Shubnikov-de Haas (SdH) oscillations at 2 K under different applied magnetic fields ranging from 4 to 14 T

Open data from the third observing run of LIGO, Virgo, KAGRA, and GEO

The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages

Search for gravitational-wave transients associated with magnetar bursts in advanced LIGO and advanced Virgo data from the third observing run

Gravitational waves are expected to be produced from neutron star oscillations associated with magnetar giant f lares and short bursts. We present the results of a search for short-duration (milliseconds to seconds) and longduration (∼100 s) transient gravitational waves from 13 magnetar short bursts observed during Advanced LIGO, Advanced Virgo, and KAGRA’s third observation run. These 13 bursts come from two magnetars, SGR1935 +2154 and SwiftJ1818.0−1607. We also include three other electromagnetic burst events detected by FermiGBM which were identified as likely coming from one or more magnetars, but they have no association with a known magnetar. No magnetar giant flares were detected during the analysis period. We find no evidence of gravitational waves associated with any of these 16 bursts. We place upper limits on the rms of the integrated incident gravitational-wave strain that reach 3.6 × 10−²³ Hz at 100 Hz for the short-duration search and 1.1 ×10−²² Hz at 450 Hz for the long-duration search. For a ringdown signal at 1590 Hz targeted by the short-duration search the limit is set to 2.3 × 10−²² Hz. Using the estimated distance to each magnetar, we derive upper limits upper limits on the emitted gravitational-wave energy of 1.5 × 1044 erg (1.0 × 1044 erg) for SGR 1935+2154 and 9.4 × 10^43 erg (1.3 × 1044 erg) for Swift J1818.0−1607, for the short-duration (long-duration) search. Assuming isotropic emission of electromagnetic radiation of the burst fluences, we constrain the ratio of gravitational-wave energy to electromagnetic energy for bursts from SGR 1935+2154 with the available fluence information. The lowest of these ratios is 4.5 × 103

A joint Fermi-GBM and Swift-BAT analysis of gravitational-wave candidates from the third gravitational-wave observing run

We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers

Constraints on the cosmic expansion history from GWTC–3

We use 47 gravitational wave sources from the Third LIGO–Virgo–Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC–3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34 M⊙, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding ${H}_{0}={68}_{-8}^{+12}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC–1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of ${H}_{0}={68}_{-6}^{+8}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC–1 result and 20% with respect to recent H0 studies using GWTC–2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814

Riccati generalization of self-similar solutions of nonautonomous Gross-Pitaevskii equation

We present a systematic analytical approach to construct a family of self-similar waves, related through a free parameter, in quasi one-dimension Gross-Pitaevskii equation with time-varying parameters. This approach enables us to control the dynamics of dark and bright similaritons, and first- and second- order self-similar rogue waves in Bose-Einstein condensate through the modulation of time dependent trapping potential. The analysis is done for the sech2− type time-varying quadratic trapping potential for two different choices of linear potential

Decision Support System for Research Project Duplication Detection

Not AvailableDecision Support Systems are usually computer applications along with a human component that can sift through large amounts of data and pick between many choices. Among many challenges in front of research managers, checking of duplication of research efforts is a major challenge. Existing systems do provide simple keyword base search wherein one can find similar projects. These systems do not take care of the semantics or sense of the word into consideration. Also, these systems fail to provide results if synonyms of the keywords are used in other research projects. Moreover, if the keywords are matched and are not used in the same sense, it is very much likely that the projects may not be similar. The presented approach in this work uses WordNet Ontology for finding the semantics of the textual information available within the system. Two algorithms viz. Filtered Set and Preferential Coefficient are presented that also take care the structure of the research project proposal. The algorithms are implemented for the PIMS-ICAR database that contains more than 5000 research project documents.Not Availabl

Not Available

Not AvailableAgricultural Statistician Network provides dynamic working linkages among the statisticians with emphasis on research information exchange, resource sharing and optimizing response time for addressing methodology related problems and foster fellow feelings among the group with cost effective communication media. The website is accessible across the world at the address www. iasri.res.in/asn/ and provides an opportunity to enhance the image of organizations and the statisticians at the international platform. It lays emphasis on providing a unified base on various professional activities of the agricultural statisticians. Individual’s research expertise is exposed to the international community thus providing opportunity for global collaboration. System has features like chat, discussion group, notice board, search, online registration and online data management for effective communication. Web site has been designed and developed using standard three-tier architecture. Site has been developed using Active Server Pages (ASP) for server side programming, Hyper Text Markup Language (HTML) and VBScript for client side interface and validation and Microsoft Access for Database management.Not Availabl

Relativistic fine structure and the energy levels of confined multi-electron GaAs quantum dot with hydrogenic impurity within the effective mass approximation in presence of magnetic field

The theory of ground state and excited state energies calculations of multielectron quantum dot with hydrogenic impurity within the effective mass approximation has been given. Results show that ground and excited state energies decrease with dot radius. In the present paper, calculation has been carried out for two electron quantum dot. The effect of magnetic field on first excited state for different values of and has been studied. In addition, the first order relativistic terms such as relativistic correction to the kinetic energy, Darwin and spin-orbit interaction term for first excited state have been investigated. According to the results obtained (i) Relativistic correction to kinetic energy, Darwin and spin-orbit interaction term approaches zero when dot size increases. (ii) The splitting between j=1/2 and j=3/2 due to spin-orbit interaction decreases by increasing dot size. (iii)The splitting between j=1/2 and j=3/2 due to spin-orbit interaction decreases by increasing depth of potential