bluuebunny/crossref_metadata_2025_split huggingface dataset:
An Analysis Study of Paddy Cultivation in Sivagangai District – A Case Study
Authors: Nageswari R , Maya Murugan R 
Published: April 2019

Agricultural development is a precondition for the overall economic development of a country. India occupies sixth rank in the world in terms of agricultural development. India stands in the second rank in the production of rice next to china. The share of Indian agriculture is 2.4 percent in the world. Rapid growth in agriculture is essential not only to achieve self-reliance but also for the food security of the household. The agricultural sector through its product contribution, factor contribution, and market contribution might act as the leading sector for economic development. Economist Arthur Lewis thinks that agricultural surplus is used by the secondary and tertiary sectors for their expansion for maintaining food security and at the same time mobilizing a large agricultural surplus for the urban areas is much needed for agricultural development.
This paper is mostly focussed on the Log- Linear Regression model of Cob Douglas type and it is adopted to estimate the vital factor which determines the yield. A Yield is for two farm size that is small and large farmers in the regression model, yield is considered as a dependent variable and input factor of the following analyses.
Enrolment of Health Insurance by Cardiovascular Disease Affected Informal Industrial Workers in Coimbatore
Authors: Naagarajan R , Jayavasuki K 
Published: April 2019

Health care costs have risen drastically over few years, and any medical treatment can make a dent on individual’s savings but with the help of these special health insurance plans, an individual can give extra cushion to them and can come out good from these problems. Insurance may be described as a social device to reduce or eliminate the risk of life and property. Under the plan of insurance, a large number of people associate themselves by sharing risk, attached to an individual insurance plan that exclusively covers healthcare costs and is called Health Insurance. One possible solution to the above said problem was to reduce the financial barrier through health insurance. Unfortunately, currently only about 10 percent of the population protected under any health insurance coverage. The most are for employees in the formal (Ellis et al. 2000). The informal workers were unprotected and had to depend on those above poorly financed public sector or the expensive private sector to take care of its needs. The government is keen to increase the insurance coverage and has even introduced special health insurance packages for the poor (Times of India, 2003). Health insurance schemes are one way of guaranteeing access to health care services. Under such schemes ideally, people should apply for membership and be making monthly contributions so that in the event of any sickness; the health insurer will be able to meet the cost of medical care. Health insurance plays important role in healthcare service provision. It should again be noted that the health insurance market depends on policy interventions to balance supply side and demand side forces. Demand-side forces would naturally involve health insurance participation, and for credible policy interventions it may be important that those factors affecting participation be established (Mhere, 2013). Health insurance is the fast emerging as an important mechanism to finance the health care needs of the people. The need for an insurance system that works on the basic principle of pooling risks of unexpected costs of persons falling ill and needing hospitalization by charging a premium from a wider population base of the community (Bhatia and John, 2000). Work-related health problems result in an economic loss of four to six percent of gross domestic product for most countries. About 70 percent of workers does not have any insurance to compensate them in case of occupational disease and injuries.
Regional Rural Banks and Rural Development: A Case of Pragathi Krishna Gramin Bank
Authors: Tigari Harish , Gaganadeepa M G 
Published: April 2019

The rural banking is one of the important roles in rural development of our country, and the village economy is the backbone of the Indian economy. Without the development of the rural economy, the objective of economic planning cannot be achieved. Hence the Regional rural banks (RRBs) are plays a vital role in the rural development for the economy in India. The RRBs were established on October 2, 1975, with the main objective of a provisional credit to rural people who are not economically strong enough, especially the small farmers, artisans, agricultural laborers, and even small entrepreneurs. The present study is a modest attempt to rural credit structure and the role played by RRBs in the development of rural economy. The present research paper is designed in nature and makes use of secondary data. The relevant secondary data have been collected mainly through the articles, journals, books, and websites have been referred. This paper is to examine the rural credit structure in RRBs of Pragathi Krishna Gramin Bank. And this study is focused only on the specific area like loans and advances made by the RRBs for three years period of 2015-16 to the year 2017-18.
Need of Virtual Reality to Enrich Teacher Education
Authors: Nachimuthu K , Revathi A 
Published: April 2019

Virtual reality (VR) is a technology which allows a user to interact with a computer-simulated imaginary environment. Users can interact with a virtual environment through the keyboard and mouse or special devices. Virtual reality can be defined as an upcoming technology that makes users feel in a Virtual Environment (VE) by using computer hardware and software. VR provides a different way to see and experience information, one that is dynamic and immediate. This paper explains the different models of VR devices in the world.
The aim of the research is to identify the level of awareness of virtual technology in the B.Ed college student-teachers in the Tamil Nadu State of India. A descriptive survey method to adopt and a total of 350 first year student-teachers from Seven B.Ed Colleges in and around Salem district of Tamil Nadu were selected by using simple random sampling technique. An awareness of virtual technology (AVT) tool with 0.89 reliability and known content validity was used.
The calculated ‘t' value among student-teachers with respect to gender; mobile in the home; to having PC in the home; and net course already passed significantly differ at 0.05 level could be noticed as rejected these hypotheses. Whereas locality and type of college of education are accepted the hypothesis. Postgraduate qualified student teachers had better awareness than undergraduate qualified student-teachers. The author recommends the students may be encouraged to use the network in their home.
Credibility of Teachers - The Decisive Aspect in Building the Credibility of the Institution
Authors: Padmini P 
Published: April 2019

The constructed credibility of an institution is primarily dependent upon how the institution is perceived by others. Knowledge and expertise of subject matter, honesty of intent, and concern for others all play into the credibility of an educational institution. There are different criteria generally used by the community to consider an institution a credible one. Credibility in education includes a wide range of issues like the credibility of the teacher, credibility of instructional resources, the credibility of information, and the credibility of research material.
Of all these, the most crucial one is the credibility of the teacher. It is important for a credible institution to have dedicated and qualified teachers. Of course in all the institutions they follow certain prescribed norms for appointing teachers and naturally only qualified teachers are employed. However it is important to probe a little deeper and ask ourselves whether we need qualified teachers or credible teachers. a teacher is always considered the best source of knowledge. In such a situation the credibility of the teacher becomes more important.
A credible teacher is expert and trustworthy person who shapes his pupils. This paper aims to identify and analyse the different factors that would enable the credibility of a teacher and how this credibility of the teacher becomes the decesive aspect in building the credibility of the institution.
Fate of the Runner in Hit-and-run Collisions
Authors: Emsenhuber Alexandre , Asphaug Erik 
Published: April 2019

Abstract
In similar-sized planetary collisions, a significant part of the impactor often misses the target and continues downrange. We follow the dynamical evolution of “runners” from giant impacts to determine their ultimate fate. Surprisingly, runners reimpact their target planets only about half of the time for realistic collisional and dynamical scenarios. Otherwise, they remain in orbit for tens of millions of years (the limit of our N-body calculations) and longer, or they sometimes collide with a different planet than the first one. When the runner does return to collide again with the same target planet, its impact velocity is mainly constrained by the outcome of the prior collision. Impact angle and orientation, however, are unconstrained by the prior collision.
On the Nature of the Compact Sources in IRAS 16293–2422 Seen at Centimeter to Submillimeter Wavelengths
Authors: Hernández-Gómez Antonio , Loinard Laurent , Chandler Claire J. , Rodríguez Luis F. , Zapata Luis A. , Wilner David J. , Ho Paul T. P. , Caux Emmanuel , Quénard David , Bottinelli Sandrine , Brogan Crystal L. , Hartmann Lee , Menten Karl M. 
Published: April 2019

Abstract
We present multi-epoch continuum observations of the Class 0 protostellar system IRAS 16293–2422 taken with the Very Large Array (VLA) at multiple wavelengths between 7 mm and 15 cm (41 GHz down to 2 GHz), as well as single-epoch Atacama Large Millimeter/submillimeter Array continuum observations covering the range from 0.4 to 1.3 mm (700 GHz down to 230 GHz). The new VLA observations confirm that source A2 is a protostar driving episodic mass ejections, and reveal the complex relative motion between A2 and A1. The spectrum of component B can be described by a single power law (S

ν
∝ ν
2.28) over the entire range from 3 to 700 GHz (10 cm down to 0.4 mm), suggesting that the emission is entirely dominated by dust even at λ = 10 cm. Finally, the size of source B appears to increase with frequency up to 41 GHz, remaining roughly constant (at 0.″39 ≡ 55 au) at higher frequencies. We interpret this as evidence that source B is a dusty structure of finite size that becomes increasingly optically thick at higher frequencies until, in the millimeter regime, the source becomes entirely optically thick. The lack of excess free–free emission at long wavelengths, combined with the absence of high-velocity molecular emission, indicates that source B does not drive a powerful outflow, and might indicate that source B is at a particularly early stage of its evolution.
Temporal Evolution of the Latitude and Energy Dependence of the Energetic Neutral Atom Spectral Indices Measured by the Interstellar Boundary Explorer (IBEX) Over the First Nine Years
Authors: Desai M. I. , Dayeh M. A. , Allegrini F. , McComas D. J. , Funsten H. , Heerikhuisen J. , Fuselier S. A. , Pogorelov N. , Schwadron N. A. , Zank G. P. , Zirnstein E. J. , Sokół J. M. , Tokumaru M. , Bzowski M. , Kubiak M A. , Reisenfeld D. B. 
Published: April 2019

Abstract
We surveyed the temporal evolution of the latitude and energy dependence of the ∼0.5–6 keV energetic neutral atom (ENA) spectral indices in the globally distributed flux (GDF) observed by the Interstellar Boundary Explorer from 2009 to 2017. We show that (1) the ENA fluxes in the GDF diminish substantially at all latitudes from 2009 to 2016, with the largest decreases occurring above ∼2.73 keV in the northern hemisphere; and (2) the latitudinal ordering of the >1.36 keV ENA spectral indices during 2009–2013 is disrupted during 2014–2017, with the indices exhibiting a north–south asymmetry. This north–south asymmetry is due to the asymmetric decrease in the GDF and the resulting occurrence of significantly steeper spectra in the northern hemisphere. The latitudinal organization of the ENA spectral indices during 2009–2013 and its disruption during 2013–2017 are remarkably similar to that of the solar wind (SW) speed profile observed in the inner heliosphere, thus confirming that the latitudinal profile of the ENA spectral indices in the GDF is a direct manifestation of the SW latitudinal speed profile following a ∼2–3 yr delay due to the SW-ENA recycling time. Based on these results and the SW speed profiles during 2014–2017, we speculate that the ENA spectral indices during 2018–2020 will not exhibit the systematic latitudinal ordering observed during 2009–2014, but instead will show relatively constant and similar values at all energies and all latitudes. There may also be a small north–south asymmetry wherein the northern hemisphere ENA spectra will be slightly flatter compared to those in the southern hemisphere.
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Authors: Li K. J. , Xu J. C. , Yin Z. Q. , Feng W. 
Published: April 2019

Abstract
Coronal heating is a big question for modern astronomy. Daily measurement of 985 solar spectral irradiances (SSIs) at the spectral intervals 1–39 and 116–2416 nm during 2003 March 1 to 2017 October 28 is utilized to investigate characteristics of solar rotation in the solar atmosphere by means of the Lomb–Scargle periodogram method to calculate their power spectra. The rotation period of coronal plasma is determined to be 26.3 days, and that of the solar atmosphere at the bottom of the photosphere modulated by magnetic structures is 27.5 days. Here we report for the first time that, unexpectedly, the coronal atmosphere is found to rotate faster than the underlying photosphere. When time series of SSIs are divided into different cycles as well as the ascending and descending periods of a solar cycle, the rotation rate in the corona is also found to be larger than that in the photosphere, and this actually uncovers hidden evidence: it is small-scale magnetic activity that heats the corona.
Transits of Inclined Exomoons—Hide and Seek and an Application to Kepler-1625
Authors: Martin David V. , Fabrycky Daniel C. , Montet Benjamin T. 
Published: April 2019

Abstract
A Neptune-sized exomoon candidate was recently announced by Teachey & Kipping, orbiting a 287 day gas giant in the Kepler-1625 system. However, the system is poorly characterized and needs more observations to be confirmed, with the next potential transit in 2019 May. In this Letter, we aid observational follow up by analyzing the transit signature of exomoons. We derive a simple analytic equation for the transit probability and use it to demonstrate how exomoons may frequently avoid transit if their orbit is larger than the stellar radius and sufficiently misaligned. The nominal orbit for the moon in Kepler-1625 has both of these characteristics, and we calculate that it may only transit ≈40% of the time. This means that ≈six non-transits would be required to rule out the moon’s existence at 95% confidence. When an exomoon’s impact parameter is displaced off the star, the planet’s impact parameter is displaced the other way, so larger planet transit durations are typically positively correlated with missed exomoon transits. On the other hand, strong correlations do not exist between missed exomoon transits and transit timing variations of the planet. We also show that nodal precession does not change an exomoon’s transit probability and that it can break a prograde-retrograde degeneracy.
Supermassive Binaries in Quasars and BL Lac Objects: Electromagnetic and Gravitational Wave Emissions
Authors: Cavaliere A. , Tavani M. , Munar-Adrover P. , Argan A. 
Published: April 2019

Abstract
The search in active galactic nuclei (AGNs) for supermassive binary systems with total mass M ∼ 108–109
M
⊙ is intertwined with the observational efforts aimed at their contributions to the stochastic background of gravitational waves (GWs). Here we discuss and compare two classes of AGNs that are outstanding in electromagnetic bands: bright, relatively distant and massive quasars, and closer jetted and less massive BL Lac objects (BL Lacs). Among the latter, we focus on the source PG 1553+113 at redshift z ≃ 0.5, one of the best periodic candidates so far, that features a five-fold repetitive pattern of period P = 2.2 yr recurring in its gamma-ray light curve, as continuously monitored by Fermi-LAT for over 9 yr and updated here to 2018 March 15. We discuss this object as an interesting candidate for hosting a supermassive binary source of GWs, and explore the possible contributions to the GW stochastic background from it and similar sources in the BL Lac class. We find the possible contributions of such sources to lie below the limits set by the current Pulsar Timing Arrays, but well within the reach of the upcoming Square Kilometer Array.
Simulating the Dark Matter Decay Signal from the Perseus Galaxy Cluster
Authors: Lovell Mark R. , Iakubovskyi Dmytro , Barnes David , Bose Sownak , Frenk Carlos S. , Theuns Tom , Hellwing Wojciech A. 
Published: April 2019

Abstract
The nearby Perseus galaxy cluster is a key target for indirect detection searches for decaying dark matter. We use the C-EAGLE simulations of galaxy clusters to predict the flux, width, and shape of a dark matter decay line, paying particular attention to the unexplained 3.55 keV line detected in the spectra of some galaxies and clusters, and the upcoming XRISM X-ray observatory mission. We show that the line width in C-EAGLE clusters similar to Perseus is typically [600–800]

, and therefore narrower than the amplitude of the velocity dispersion of galaxies in the cluster. Halos that are significantly disturbed can, however, exhibit galaxy velocity dispersions higher than 1000

, and in this case will show a large difference between the line profiles of on- and off-center observations. We show that the line profile is likely to be slightly asymmetric, but still well approximated by a Gaussian at the 10% level, and that the halo asymmetry can lead to fluxes that vary by a factor of two. In summary, we predict that, if the previously reported 3.55 keV line detections do originate from dark matter decay, the XRISM mission will detect a line with a roughly Gaussian profile at a rest-frame energy of 3.55 keV, with a width >600

and flux approximately in the range

.
Turning up the Heat on ‘Oumuamua
Authors: Forbes John C. , Loeb Abraham 
Published: April 2019

Abstract
We explore what may be learned by close encounters between extrasolar minor bodies like ‘Oumuamua and the Sun. These encounters may yield strong constraints on the bulk composition and possible origin of ‘Oumuamua-like objects. We find that such objects collide with the Sun once every 30 yr, while about two pass within the orbit of Mercury each year. We identify preferred orientations for the orbits of extrasolar objects and point out known solar system bodies with these orientations. We conclude using a simple Bayesian analysis that one of these objects is extrasolar in origin, even if we cannot tell which.
Gas Flows Within Cavities of Circumbinary Disks in Eccentric Binary Protostellar Systems
Authors: Mösta Philipp , Taam Ronald E. , Duffell Paul C. 
Published: April 2019

Abstract
The structure and evolution of gas flows within the cavity of a circumbinary disk (CBD) surrounding the stellar components in eccentric binaries are examined via two-dimensional hydrodynamical simulations. The degree to which gas fills the cavity between the circumstellar disks (CSDs) and the CBD is found to be greater for highly eccentric systems, in comparison to low-eccentricity systems, reflecting the spatial extent over which mass enters into the cavity throughout the orbit. The pattern of the gas flow in the cavity differs for eccentric binaries from that of binaries in a circular orbit. In particular, the former reveals tightly wound gas streams and figure-eight-like structures for systems characterized by eccentricies e ≥ 0.4, whereas the latter only reveal relatively loosely bent streams from the CBD to the CSDs. Hence, the description of the stream structures can be a probe of sufficient non-circularity of the binary orbital motion. Given that the inner edge of the CBD is not very well defined for highly eccentric systems due to the complex gas structures, it is suggested that the area of the cavity for high-sensitivity imaging observations may prove to be a more useful diagnostic for probing the effectiveness of CBD clearing in the future.
NuSTAR Measurement of Coronal Temperature in Two Luminous, High-redshift Quasars
Authors: Lanzuisi G. , Gilli R. , Cappi M. , Dadina M. , Bianchi S. , Brusa M. , Chartas G. , Civano F. , Comastri A. , Marinucci A. , Middei R. , Piconcelli E. , Vignali C. , Brandt W. N. , Tombesi F. , Gaspari M. 
Published: April 2019

Abstract
X-ray emission from the active galactic nucleus (AGN) is believed to be produced via Comptonization of optical/ultraviolet seed photons emitted by the accretion disk, upscattered by hot electrons in a corona surrounding the black hole. A critical compactness versus temperature threshold is predicted above which any increase in the source luminosity, for a fixed size, would then generate positron–electron pairs rather than continue heating the coronal plasma. Current observations seem to confirm that all AGNs populate the region below this critical line. These models, however, have never been probed by observations in the high-luminosity regime, where the critical line is expected to reach low temperatures. To fill this observational gap, we selected two luminous (log(L
Bol) > 47.5 erg s−1) quasars, 2MASSJ1614346+470420 (z = 1.86) and B1422+231 (z = 3.62), and obtained XMM–Newton and NuSTAR deep observations for them. We performed detailed spectral analysis of their quasisimultaneous soft and hard X-ray data, in order to constrain the parameters of their coronae. Using a phenomenological cutoff power-law model, with the inclusion of a reflection component, we derived rest-frame values of the high-energy cutoff of E
cut =

keV and E
cut =

keV, respectively. Comptonization models consistently give as best-fit parameters electron temperatures of ∼45 keV and ∼28 keV, respectively, and optically thick coronae (τ > 1). These low coronal temperatures fall in the limited region allowed at these luminosities to avoid runaway pair production.