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Electrospinning with various machine configurations is being used to produce polymer nanofibers with different rates of output. The use of polymers with high viscosity and the encapsulation of nanoparticles for achieving functionalities are some of the limitations of the existing methods. A profiled multi-pin electrospinning (PMES) setup is demonstrated in this work that overcomes the limitations in the needle and needleless electrospinning like needle clogging, particle settling, and uncontrolled/uneven Taylor cone formation, the requirement of very high voltage and uncontrolled distribution of nanoparticles in nanofibers. The key feature of the current setup is the use of profiled pin arrangement that aids in the formation of spherical shape polymer droplet and hence ensures uniform Taylor cone formation throughout the fiber production process. With a 10 wt% of Polyvinyl Alcohol (PVA) polymer solution and at an applied voltage of 30 kV, the production rate was observed as 1.690 g/h and average fiber diameter obtained was 160.5 ± 48.9 nm for PVA and 124.9 ± 49.8 nm for Cellulose acetate (CA) respectively. Moreover, the setup also provides the added advantage of using high viscosity polymer solutions in electrospinning. This approach is expected to increase the range of multifunctional electrospun nanofiber applications.

Imitating Dolphin fish-like movement is productive method for enhancing their hydrodynamic capabilities. This work aims to analyze and understand the oscillations of tail fluke of Dolphin, which can be used as a propulsive mechanism for underwater fish robots and vehicles. The objective of the work is to achieve the desired oscillating amplitude by simulating the NACA 0012 profile using computational models and Set up the swimming movement of the dolphin, imitating a fish like model. Computational techniques were employed to examine the propulsive capabilities of the oscillating hydrofoil, inspired by the dolphin's biological propulsion. The evolutionary of fluid pattern in the field surrounding both Dolphin fish model and the NACA0012 hydrofoil, from initial motion to cruising, was established, and the hydrodynamic impact was subsequently studied. An user-defined function (UDF) was developed to create a dynamic mesh interface with CFD code ANSYS FLUENT for establishing the oscillations of Dolphin tail across the flow field. Influencing hydrodynamic coefficients such as lift and drag coefficients at different frequencies were also obtained. The findings shown that when the acceleration of the Dolphin fish model increases, the time averaged drag force coefficient drops because The wake field's vortex disperses to have some beneficial effects and pressure of water surrounding the fish head intensifies to produce a large resistance force. Simulation results show a 98% agreement at lower frequency and speed levels but a 5% deviation at higher frequency and speed due to turbulence effects in both models. It was established that the vortex superposition enhances the Dolphin fish like model rather than lowering its positive impacts. The Strouhal number, which is obtained by the fluid field's evolution rule, can be linked to the Kármán vortex street span with reverse.

Repowering one of the old Indian wind farms located at a potential wind site is discussed. Various options of repowering have been suggested and compared based on annual energy production and levelised cost of generation. Economic performance indices of repowering in the current wind power policy scenario have been evaluated and the feasibility is discussed. The study infers that partial repowering could be economically more attractive than total repowering, whereas total repowering of old wind farms located at potential sites would be essential to meet renewable energy targets of a nation like India.

This study was carried out to evaluate the influence of high voltage polarity on a newly designed multi-pin upward electrospinning spinneret to produce poly (vinyl alcohol) nanofibers. Two different high voltage polarity configurations were applied to the spinneret and collector, namely collector charging configuration (configuration-1) and spinneret charging configuration (configuration-2). The outcomes demonstrated that the collector charging configuration is better in case of upward multi-pin electrospinning setup, to their conservative framework in terms of stable Taylor cone formation, smaller fiber diameter and less bead formation. Electrical field profile in the electrospinning zone was investigated using finite element modelling for both the configurations. No difference in electric field intensity norm (|E|) was observed near the tip of the pins for both the polarities (configurations). Although having the same magnitude, the dominant electrical field component, Ez for configuration -1 is found to be of opposite sign to that of configuration -2. The electrostatic simulations also suggested that all the pins were not at the same potential and that there was a minor difference in pin potentials. Also, optimizations of pin length to reduce the potential differences between the pins were theoretically estimated through COMSOL3D simulation software.

In this paper, mixed flow impeller is investigated to reduce the secondary flow loss and attain uniform flow at impeller exit by changing the wrap angle in the trailing edge (called as stacking condition). The 3D inverse design methodology is adopted for the blade profile generation using ADT Turbo suite software. The internal flow analysis of the base design is evaluated using commercial computational fluid dynamics (CFD). A single stage proto type model is tested and the experimental results have strong agreement with numerical analysis results. Further the impeller is designed with different wrap angle at the trailing edge of the hub and shroud region. The pump performance curve is obtained from numerical analysis for the optimized impellers from the ADT Turbo suite and compared with the base design. The wrap angle between 8 ̊ - 15̊ degree in hub region has the less secondary flow losses compared to the stacking in the shroud region. Higher wrap angle above 17 ̊ degree increases the diffusion ratio which in turn induces non-uniform flow at the impeller exit and also increases instability.

The Square Kilometre Array (SKA) Observatory is a next-generation radio astronomy facility that has recently entered into the construction phase, after successful completion of the design and prototyping phases during 2013–2021. Planned to be operational by the end of this decade, the SKA is expected to revolutionise astronomy by allowing cutting edge explorations in an extremely wide range of science areas, while driving the growth of many important new state-of-the-art technologies. There are more than 10 countries currently participating in the international consortium to build this facility, which will be co-located in Australia and South Africa with the global headquarters in the United Kingdom. Indian scientists and engineers have played a significant role since the beginning: from the definition of the SKA concept and its science case, to some important aspects of the design of the instrument and the prototyping activities. India is now getting ready to join the construction phase of the SKA with a well defined proposal for technical activities spanning a few different areas of work. Along with this, Indian astronomers are busy refining their science case for the SKA and preparing in different ways to be ready for front line science with the facility as and when it is commissioned. All these activities are coordinated by the SKA India consortium, which currently has a membership of more than 20 institutions across the country. In this paper, we describe the current status of the SKA project, and focus on India’s role—past contributions, ongoing activities and future plans.

The low-frequency radio telescope of the Square Kilometre Array (SKA) is being built by the international radio astronomical community to (i) have orders of magnitude higher sensitivity and (ii) be able to map the sky several hundred times faster, than any other existing facilities over the frequency range of 50–350 MHz. The sensitivity of a radio telescope array is in general, dependent upon the number of electromagnetic sensors used to receive the sky signal. The total number of them is further constrained by the effects of mutual coupling between the sensor elements, allowable grating lobes in their radiation patterns, etc. The operating frequency band is governed by the desired spatial and spectral responses, acceptable sidelobe and backlobe levels, radiation efficiency, polarization purity and calibratability of sensors’ response. This paper presents a brief review of several broadband antennas considered as potential candidates by various engineering groups across the globe, for the low-frequency radio telescope of SKA covering the frequency range of 50–350 MHz, on the basis of their suitability for conducting primary scientific objectives.

Type III solar radio bursts are the Sun’s most intense and frequent nonthermal radio emissions. They involve two critical problems in astrophysics, plasma physics, and space physics: how collective processes produce nonthermal radiation and how magnetic reconnection occurs and changes magnetic energy into kinetic energy. Here magnetic reconnection events are identified definitively in Solar Dynamics Observatory UV-EUV data, with strong upward and downward pairs of jets, current sheets, and cusp-like geometries on top of time-varying magnetic loops, and strong outflows along pairs of open magnetic field lines. Type III bursts imaged by the Murchison Widefield Array and detected by the Learmonth radiospectrograph and STEREO B spacecraft are demonstrated to be in very good temporal and spatial coincidence with specific reconnection events and with bursts of X-rays detected by the RHESSI spacecraft. The reconnection sites are low, near heights of 5–10 Mm. These images and event timings provide the long-desired direct evidence that semi-relativistic electrons energized in magnetic reconnection regions produce type III radio bursts. Not all the observed reconnection events produce X-ray events or coronal or interplanetary type III bursts; thus different special conditions exist for electrons leaving reconnection regions to produce observable radio, EUV, UV, and X-ray bursts.

Backed by advances in digital electronics, signal processing, computation and storage technologies, aperture arrays, which had strongly influenced the design of telescopes in the early years of radio astronomy, have made a comeback. Amid all these developments, an international effort to design and build the world’s largest radio telescope, the Square Kilometre Array (SKA), is ongoing. With its vast collecting area of 1  km 2 , the SKA is envisaged to provide unsurpassed sensitivity and leverage technological advances to implement a complex receiver to provide a large field of view through multiple beams on the sky. Many pathfinders and precursor aperture array telescopes for the SKA, operating in the frequency range of 10–300 MHz, have been constructed and operationalized to obtain valuable feedback on scientific, instrumental and functional aspects. This review article looks explicitly into the progression of digital-receiver architecture from the Murchison Widefield Array (precursor) to the SKA1-Low. It highlights the technological advances in analog-to-digital converters (ADCs), field-programmable gate arrays (FPGAs) and central processing unit–graphics processing unit (CPU–GPU) hybrid platforms around which complex digital signal processing systems implement efficient channelizers, beamformers and correlators. The article concludes with a preview of the design of a new generation signal processing platform based on radio frequency system-on-chip (RFSoC).

Probing the Universe with atomic hydrogen 21 cm emission is a fascinating and challenging work in astronomy. Radio telescopes play a vital role in detecting and imaging these faint signals. Powerful radio telescopes are complex to construct and operate. We have built a simple, low-cost 21 cm radio telescope primarily for educational training purposes. The design uses a custom horn antenna, ready-to-use radio-frequency components, and a software-defined radio module. The telescope operates efficiently from a rooftop in a city environment. Using this telescope, we have conducted observations and successfully detected the 21 cm line emissions from the different directions of our galactic plane. Based on the Doppler-shift observed in these measurements, we have successfully derived the Galactic rotation velocity (rotation curve) in those directions. The paper presents the details of the telescope construction, 21 cm observation, and the Galactic rotation curve derivation.