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This article uncovers the congruity of Neo-Platonism in Autobiography of a Yogi by Yogananda. The philosophy of Neo- Platonism postulates that the phenomenal creation is the emanation of the Cosmic One which radiates pervasive wisdom, the world soul and the living being. Thus, the spark of divinity dwells in every living being. Likewise, Yogananda's Autobiography of a Yogi expounds that the entirety of creation is the qualitative growth of the unitary cosmic consciousness that is known as God. With the experience of Kriya Yoga, one can transform this mundane identity into a cosmic self by establishing communion with cosmic consciousness or God. This is the ultimate way to realize God Consciousness, liberating oneself from the bondage of the phenomenal world. Besides, this work also enthralls the dichotomy of soul and body by substantiating the concept that creation is the idea of a divine unitary mind. The body is the source of frozen energy. The moment it embraces yogic vibes, it suffuses to realize its original source. In this way, both Neo- Platonism and Yogananda unite to open the gateway to realize the effulgence of the One, the highest Good, cosmic consciousness, or God. To explore these concepts, this article implements the paradigm of qualitative approach, interpreting Autobiography of Yogi from the philosophical lens of Neo-Platonism propounded both in the East and the West.

This is the author accepted manuscript. The final version is available from Elsevier via the DOI in this record ; The harvesting of electrical energy from sunrays with low cost, clean form and prosperity is an excellent progression. In this context, significant advancement has been made in the solar energy area in terms of cell's design to enhance efficiency. Light scattering may benefit solar cells in this aspect by extending the travelling distance of light within the photoelectrode film. In this work, dextran templating high-surface-area contained CeO2 nanoparticles (~22 nm) were employed to improve the power conversion efficiency (PCE) of a TiO2-based dye-sensitized solar cell (DSSCs). Various physicochemical techniques were investigated to characterize the synthesized CeO2 nanoparticles. Synthesized cubic CeO2 nanoparticles were further explored as an additional layer on the top of the synthesized anatase TiO2 nanocube based film to fabricate CeO2-TiO2 hybrid photoanode, encouraging light scattering in DSSCs. A comparative study was undertaken to understand the effect of the CeO2 layer on the synthesized and standard anatase TiO2. The overall power conversion efficiency obtained for hybrid photoanode-based DSSC is 8.92%, ~46% higher than that of TiO2 nanocubes-based photoanode, a considerably improved open-circuit voltage of 0.83V under 1 SUN 1.5 AM. In addition, the PCE enhancement is observed only ~8% using standard TiO2 based photoanode under the same condition. The photovoltaic performance highlights that dextran templating CeO2 nanoparticle exhibits a significant impact as the light scattering layer and heterojunction formation when incorporating on top of the anatase TiO2 nanocube resulting in a hybrid photoanode enhancing the PCE of DSSCs. This alternative approach could facilitate the performance of TiO2 based DSSCs towards improving efficiency ; Department of Science and Technology (DST), Government of India ; British Council

This is the final version. Available on open access from MDPI via the DOI in this record ; The rapid efficiency enhancement of perovskite solar cells (PSCs) make it a promising photovoltaic (PV) research, which has now drawn attention from industries and government organizations to invest for further development of PSC technology. PSC technology continuously develops into new and improved results. However, stability, toxicity, cost, material production and fabrication become the significant factors, which limits the expansion of PSCs. PSCs integration into a building in the form of building-integrated photovoltaic (BIPV) is one of the most holistic approaches to exploit it as a next-generation PV technology. Integration of high efficiency and semi-transparent PSC in BIPV is still not a well-established area. The purpose of this review is to get an overview of the relative scope of PSCs integration in the BIPV sector. This review demonstrates the benevolence of PSCs by stimulating energy conversion and its perspective and gradual evolution in terms of photovoltaic applications to address the challenge of increasing energy demand and their environmental impacts for BIPV adaptation. Understanding the critical impact regarding the materials and devices established portfolio for PSC integration BIPV are also discussed. In addition to highlighting the apparent advantages of using PSCs in terms of their demand, perspective and the limitations, challenges, new strategies of modification and relative scopes are also addressed in this review. ; University of Exeter

SB would like to thank Tara Murphy, Martin Bell, Paul Hancock, Keith Bannister, Chris Blake and Bing Zhang for useful discussions. ; We report the discovery of four Fast Radio Bursts (FRBs) in the ongoing SUrvey for Pulsars and Extragalactic Radio Bursts at the Parkes Radio Telescope: FRBs 150610, 151206, 151230 and 160102. Our real-time discoveries have enabled us to conduct extensive, rapid multimessenger follow-up at 12 major facilities sensitive to radio, optical, X-ray, gamma-ray photons and neutrinos on time-scales ranging from an hour to a few months post-burst. No counterparts to the FRBs were found and we provide upper limits on afterglow luminosities. None of the FRBs were seen to repeat. Formal fits to all FRBs show hints of scattering while their intrinsic widths are unresolved in time. FRB 151206 is at low Galactic latitude, FRB 151230 shows a sharp spectral cut-off, and FRB 160102 has the highest dispersion measure (DM = 2596.1 ± 0.3 pc cm−3) detected to date. Three of the FRBs have high dispersion measures (DM > 1500 pc cm−3), favouring a scenario where the DM is dominated by contributions from the intergalactic medium. The slope of the Parkes FRB source counts distribution with fluences >2 Jy ms is α=−2.2+0.6−1.2 and still consistent with a Euclidean distribution (α = −3/2). We also find that the all-sky rate is 1.7+1.5−0.9×103 FRBs/(4π sr)/day above ∼2Jyms and there is currently no strong evidence for a latitude-dependent FRB sky rate. ; The Parkes radio telescope and the Australia Telescope Compact Array are part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. VLAis run by theNational Radio Astronomy Observatory (NRAO). NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was performed on the gSTAR national facility at Swinburne University of Technology. gSTAR is funded by Swinburne and the Australian Government's Education Investment Fund. This work is also based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We thank the LSST Project for making their code available as free software at http://dm.lsstcorp.org. Funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 617199 (EP). Access to the Lovell Telescope is supported through an STFC consolidated grant. The 100-m telescope in Effelsberg is operation by the Max- Planck-Institut für Radioastronomie with funds of the Max-Planck Society. The Sardinia Radio Telescope (SRT) is funded by the Department of University and Research (MIUR), the Italian Space Agency (ASI), and the Autonomous Region of Sardinia (RAS) and is operated as National Facility by the National Institute for Astrophysics (INAF). TB and RWW are grateful to the STFC for financial support (grant reference ST/P000541/1). Research support to IA is provided by the Australian Astronomical Observatory. The ANTARES authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commission Européenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cité (ANR-10- LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR- 11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001- 02), Région Île-de-France (DIM-ACAV), Région Alsace (contrat CPER), Région Provence-Alpes-Côte d'Azur, Département du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium für Bildung und Forschung (BMBF), Germany; IstitutoNazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Economía y Competitividad (MINECO): Plan Estatal de Investigación (refs. FPA2015- 65150-C3-1-P, -2-P and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisolía programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of data, software and/or web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsstcorp.org. RPE/MK gratefully acknowledges support from ERC Synergy Grant "BlackHoleCam" Grant Agreement Number 610058

A trade mark is a visual symbol that distinguishes the goods or services of one enterprise from those of the competitors. A reference to goods will imply services also, unless the context prohibits it. Trade Marks are at the centre of global business today. They are the major source of product differentiation and non-price competition in a modern, market driven economy. Consumers come to associate certain value in terms of performance, durability, price, after-sales service etc in the goods sold under specific brands, which may be among the greatest assets of the enterprise. In the language of the law, brand names are known as trademarks. Several products, of the same category or of different categories, can be marketed under one brand name. Recently, non-visual signs have made a strong claim for recognition as trademarks. Smell and sound signs fall under such category though they are not yet recognised in India. Several broadcasting organisations and film producers have specific signature tunes to identify their programmes. This article review about the features of legislation, function and selection of trademark, types of trademark that can be registered, duration and benefits of trademark, who can apply and use the trademark, how to apply for and formalities of major trademark transaction.