ELECTRONIC PAPER TECHNOLOGY

ABSTRACT E-Paper or electronic paper or electronic ink is a revolutionary material that is I INTRODUCTION In 1970s, the first electronic paper was developed at Xerox's Palo Alto Research centre by Nick Sheridon. Gyricon was the first electronic paper, consisted of small, statically charged balls that were white on one side and black on the other. The text was altered by the presence of an electric field, causes the balls up or down. Joseph Jacobson was developed another type of electronic paper in 1990s, who soon after co-founded the corporation E Ink which formed a business with Philips Components. After two years, two companies are carrying works in the field of development of electronic ink. One is E-ink a company at Cambridge, U.S.A. Second is Xerox doing research effort at Xerox's Palo Alto Research Centre? To build e-paper several different technologies exist, some using plastic substrate and electronic so that the display is flexible. E-paper technology is designed to mimic the appearance of ordinary ink on paper. E-paper reflects light like an ordinary paper and holds text and images without drawing electricity, while allowing the image to be change later .An ideal e-paper display can be read directly in sunlight without the image appearing to be fade. II TECHNOLOGY USED Gyricon Gyricon was the first e-paper developed in 1970s at Xerox's Palo Alto Research Centre. It is composed of polyethylene spheres of about 75 to 106 micrometers across. Each sphere (Janus particle) is composed of black plastic on one side and white plastic on the other which is negatively and positively charged respectively. In a -2319-8354(E) 107 | P a g e www.ijarse.com transparent silicone sheet these spheres are embedded, with each sphere dispersed in a bubble of oil so that every sphere can spin freely. The applied voltage polarity to each pair of electrodes determines whether the black or white side is face-up, hence giving the pixel a white or black look. Using this technology, Japanese company Soken has established a wall with electronic wall-paper at the FPD 2008 exhibition. International Journal Of Advance Research In Science And Engineering http://www.ijarse.com IJARSE, Vol. No.2, Issue No.9, September 2013 ISSN Electrophoretic display These displays form visible images, by rearrange charged colored particles using an applied electric field. In this display, titanium dioxide particles are detached in hydrocarbon oil to which a dark colored dye is added with surfactants and charging agents and then this mixture is placed between two parallel conducting plates. When an electric field is applied to it, the particles will move towards the plate bearing opposite charge. If these particles are accumulate at the front side of the display it looks white as light is reflected back by titanium particles and if these are located at the back side then it appears black because incident light is absorbed by colored dye. By applying suitable voltage to each area of the display to generate a pattern of reflecting and absorbing regions, resulting in the configuration of image in these displays. The electrophoretic technology used by E-ink is the most commonly known and used form of E-paper. Electrowetting In this technology, the shape of water/oil interface is controlled by applying appropriate voltage. The interfacial tension between coating and the water, changes when voltage is applied between electrode and the water resulting in a stacked state. This state is no more stable causing the water to move the oil to one side and results in a partially transparent pixel, or in a white pixel, if a reflective white plane is used. The observer only experiences the average reflection due to the small size of pixels and this reflection forms the basis of reflective display. When no voltage is applied, between the water and a hydrophobic insulate covering of an electrode, the oil forms a flat film, resulting in a coloured pixel. Electrowetting displays have several attractive features. These displays consume low voltage and low power and can be made thin and flat. The switching between white and coloured reflection is fast enough to show video content

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO-Virgo Run O3b

We search for gravitational-wave signals associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (2019 November 1 15:00 UTC-2020 March 27 17:00 UTC). We conduct two independent searches: A generic gravitational-wave transients search to analyze 86 GRBs and an analysis to target binary mergers with at least one neutron star as short GRB progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these GRBs. A weighted binomial test of the combined results finds no evidence for subthreshold gravitational-wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each GRB. Finally, we constrain the population of low-luminosity short GRBs using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate. © 2022. The Author(s). Published by the American Astronomical Society

Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo

Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass $M>70$ $M_\odot$) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities $0 < e \leq 0.3$ at $0.33$ Gpc$^{-3}$ yr$^{-1}$ at 90\% confidence level.Comment: 24 pages, 5 figure

Search for gravitational waves associated with gamma-ray bursts detected by Fermi and Swift during the LIGO–Virgo run O3b

We search for gravitational-wave signals associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the second half of the third observing run of Advanced LIGO and Advanced Virgo (2019 November 1 15:00 UTC–2020 March 27 17:00 UTC). We conduct two independent searches: a generic gravitational-wave transients search to analyze 86 GRBs and an analysis to target binary mergers with at least one neutron star as short GRB progenitors for 17 events. We find no significant evidence for gravitational-wave signals associated with any of these GRBs. A weighted binomial test of the combined results finds no evidence for subthreshold gravitational-wave signals associated with this GRB ensemble either. We use several source types and signal morphologies during the searches, resulting in lower bounds on the estimated distance to each GRB. Finally, we constrain the population of low-luminosity short GRBs using results from the first to the third observing runs of Advanced LIGO and Advanced Virgo. The resulting population is in accordance with the local binary neutron star merger rate

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 April of 2019 and lasting six months, O3b starting in November of 2019 and lasting five months, and O3GK starting in April of 2020 and lasting 2 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 dataset, 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.Comment: 27 pages, 3 figure

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 eccentric black hole coalescences during the third observing run of LIGO and Virgo

Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass M&gt;70 M⊙) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities 0&lt;e≤0.3 at 0.33 Gpc−3 yr−1 at 90\% confidence level

Ultralight vector dark matter search using data from the KAGRA O3GK run

Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for U(1)B−L gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the U(1)B−L gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM

Analysis and Improvement of the Checkout Drop-Offs on walmart.com

Walmart eCommerce focuses on the web and mobile applications of the retail giant. I worked as a Product Manager Intern in the Checkout team. For eCommerce platforms, it is said that the checkout flow is where the money is at. But like other platforms, Walmart also observes drop-offs in the Checkout funnel. During my internship, I focused on reducing drop-offs in Checkout to increase conversions and revenue for the company. Through a three-phased approach, I spearheaded the development of new features. These features are currently being developed and are likely to go live on Walmart eCommerce platforms this quarter

Analysis and Improvement of the Checkout Drop-Offs on walmart.com

Walmart eCommerce focuses on the web and mobile applications of the retail giant. I worked as a Product Manager Intern in the Checkout team. For eCommerce platforms, it is said that the checkout flow is where the money is at. But like other platforms, Walmart also observes drop-offs in the Checkout funnel. During my internship, I focused on reducing drop-offs in Checkout to increase conversions and revenue for the company. Through a three-phased approach, I spearheaded the development of new features. These features are currently being developed and are likely to go live on Walmart eCommerce platforms this quarter