Community

In biological terms, a community is a group of interacting species sharing a populated environment. In human communities, intent, belief, resources, preferences, needs, risks, and a number of other conditions may be present and common, affecting the identity of the participants and their degree of cohesiveness.

In sociology, the concept of community has led to significant debate, and sociologists are yet to reach agreement on a definition of the term. There were ninety-four discrete definitions of the term by the mid-1950s.Traditionally a "community" has been defined as a group of interacting people living in a common location. The word is often used to refer to a group that is organized around common values and is attributed with social cohesion within a shared geographical location, generally in social units larger than a household. The word can also refer to the national community or global community.

The word "community" is derived from the Old French communité which is derived from the Latin communitas (cum, "with/together" + munus, "gift"), a broad term for fellowship or organized society.

Since the advent of the Internet, the concept of community no longer has geographical limitations, as people can now virtually gather in an online community and share common interests regardless of physical location.

Web Search Engine

A web search engine is designed to search for information on the World Wide Web and FTP servers. The search results are generally presented in a list of results and are often called hits. The information may consist of web pages, images, information and other types of files. Some search engines also mine data available in databases or open directories. Unlike Web directories, which are maintained by human editors, search engines operate algorithmically or are a mixture of algorithmic and human input.

Cricket

Cricket is a bat-and-ball team sport. Many variations exist, with its most popular form played on an oval-shaped outdoor arena known as a cricket field at the centre of which is a rectangular 22-yard (20.12 m) long pitch that is the focus of the game. A game (or match) is contested between two teams of eleven players each. One team bats, and will try to score as many runs as possible while the other team bowls and fields, trying to dismiss  the batsmen and thus limit the runs scored by the batting team. A run is scored by the striking batsman hitting the ball with his bat, running to the opposite end of the pitch and touching the crease there without being dismissed. The teams switch between batting and fielding at the end of an innings.

There are also variations in the length of a game of cricket. In professional cricket this ranges from a limit of 20 overs per side (Twenty20) to a game played over 5 days (Test cricket, which is the highest level of the game). Depending on the form of the match being played, there are different rules that govern how a game is won, lost, drawn or tied. The rules of two-innings games are known as the Laws of Cricket and maintained by the ICC and the Marylebone Cricket Club (MCC); additional Standard Playing Conditions for Test matches and One Day Internationals augment these laws.In one version of Indoor Cricket, matches include just 6 players per side and include two 12-over innings.

Cricket was first documented as being played in southern England in the 16th century. By the end of the 18th century, it had developed to the point where it had become the national sport of England. The expansion of the British Empire led to cricket being played overseas and by the mid-19th century the first international matches were being held. Today, the game's governing body, the International Cricket Council (ICC), has 104 member countries.With its greatest popularity in the Test playing countries, cricket is the world's second most popular sport after Association football.

Desktop Computer

A desktop computer is a personal computer (PC) in a form intended for regular use at a single location, as opposed to a mobile laptop or portable computer. Prior to the widespread use of microprocessors, a computer that could fit on a desk was considered remarkably small. Desktop computers come in a variety of types ranging from large vertical tower cases to small form factor models that can be tucked behind an LCD monitor. "Desktop" can also indicate a horizontally-oriented computer case  usually intended to have the display screen placed on top to save space on the desktop. Most modern desktop computers have separate screens and keyboards. Tower cases are desktop cases in the earlier sense, though not in the latter. Cases intended for home theater PC systems are usually considered to be desktop cases in both senses, regardless of orientation and placement.

Travel

Travel is the movement of people between relatively distant geographical locations for any purpose and any duration, with or without any means of transport. Travel also includes relatively short stays between successive movements. Movements between locations  requiring only a few minutes are not considered as travel. As an activity, "travel" also covers all the activities performed during a travel (movement).

Travel may be local, regional, national (domestic) or international. In some countries, non-local internal travel may require an internal passport, while international travel typically requires a passport and visa.

Travel can be for recreational purposes, for tourism, to visit people, for business or for commuting, and may occur for numerous other reasons, such as to obtain health care, migration, fleeing war, etc. Travel may occur by human-powered transport such as walking or bicycling, or with vehicles, such as airplanes, private transport, public transport, automobiles and trains.

A round trip is a particular type of travel whereby a person moves from his/her usual residence to one or several locations and returns. A trip can also be part of a round trip.

Mortgage Loan

A mortgage loan is a loan secured by real property through the use of a mortgage note which evidences the existence of the loan and the encumbrance of that realty through the granting of a mortgage which secures the loan. However, the word mortgage alone, in everyday usage, is most often used to mean mortgage loan.

A home buyer or builder can obtain financing (a loan) either to purchase or secure against the property from a financial institution, such as a bank, either directly or indirectly through intermediaries. Features of mortgage loans such as the size of the loan, maturity of the loan, interest rate, method of paying off the loan, and other characteristics can vary considerably.

In many jurisdictions, though not all (Bali, Indonesia being one exception, it is normal for home purchases to be funded by a mortgage loan. Few individuals have enough savings or liquid funds to enable them to purchase property outright. In countries where the demand for home ownership is highest, strong domestic markets have developed.

Loan

A loan is a type of debt. Like all debt instruments, a loan entails the redistribution of financial assets over time, between the lender and the borrower.

In a loan, the borrower initially receives or borrows an amount of money, called the principal, from the lender, and is obligated to pay back or repay an equal amount of money to the lender at a later time. Typically, the money is paid back in regular installments, or partial repayments; in an annuity, each installment is the same amount.

The loan is generally provided at a cost, referred to as interest on the debt, which provides an incentive for the lender to engage in the loan. In a legal loan, each of these obligations and restrictions is enforced by contract, which can also place the borrower under additional restrictions known as loan covenants. Although this article focuses on monetary loans, in practice any material object might be lent.

Acting as a provider of loans is one of the principal tasks for financial institutions. For other institutions, issuing of debt contracts such as bonds is a typical source of funding.

Durga Puja.

Durga Puja ‘Worship of Durga’, also referred to as Durgotsab ‘Festival of Durga’, is an annual Hindu festival in South Asia that celebrates worship of the Hindu goddess Durga. It refers to all the six days observed as Mahalaya, Shashthi , Maha Saptami, Maha Ashtami, Maha Nabami and Bijoya Dashami. The dates of Durga Puja celebrations are set according to the traditional Hindu calendar and the fortnight corresponding to the festival is called Debi Pokkho ‘Fortnight of the Goddess’. Debi Pokkho is preceded by Mahalaya,The last day of the previous fortnight Pitri Pokkho (‘Fortnight of the Forefathers’), and is ended on Kojagori Lokkhi Puja (‘Worship of Goddess Lakshmi on Kojagori Full Moon Night’).

Durga Puja is widely celebrated in the Indian states of West Bengal, Assam, Jharkhand, Orissa and Tripura where it is a five-day annual holiday.In Tripura which has a majority of Bengali Hindus  it is the Biggest festival of the year. Not only it is the biggest Hindu festival celebrated throughout the State, but it is also the most significant socio-cultural event in Bengali society. Apart from eastern India, Durga Puja is also celebrated in Delhi, Uttar Pradesh, Bihar, Maharashtra, Gujarat, Punjab, Kashmir, Karnataka and Kerala. Durga Puja is also celebrated as a major festival in Nepal and in Bangladesh where 10% population are Hindu. Nowadays, many diaspora Bengali cultural organizations arrange for Durgotsab in countries such as the United States, United Kingdom, Australia, Germany, France, and Kuwait, among others. In 2006, a grand Durga Puja ceremony was held in the Great Court of the British Museum.

The prominence of Durga Puja increased gradually during the British Raj in Bengal. After the Hindu reformists resemble Durga with India, she had become an icon for the Indian independence movement. In the first quarter of the 20th century, the tradition of Baroyari  or Community Puja was popularised due to this. After independence, Durga Puja became one of the largest celebrated festivals in the whole world.

Durga Puja includes the worships of Shiva, Lakshmi, Ganesha, Saraswati and Kartikeya. Modern traditions have come to include the display of decorated pandals and artistically depicted idols of Durga, exchange of Bijoya Greetings and publication of Puja Annuals.

Computers

The throat sighs!

E-Book

An electronic book (also e-book, ebook, digital book) is a text- and image-based publication in digital form produced on, published by, and readable on computers or other digital devices."Sometimes the equivalent of a conventional printed book, e-books can also be born digital. The Oxford Dictionary of English defines the e-book as "an electronic version of a printed book,"but e-books can and do exist without any print equivalent. E-books are usually read on dedicated hardware devices known as e-Readers or e-book devices. Personal computers and some cell phones can also be used to read e-books.

AntiVirus

antivirus software is, it can sometimes have drawbacks. Antivirus software can degrade computer performance. Inexperienced users may have trouble understanding the prompts and decisions that antivirus software presents them with. An incorrect decision may lead to a security breach. If the antivirus software employs heuristic detection (of any kind), success depends on achieving the right balance between false positives and false negatives. False positives can be as destructive as false negatives. Finally, antivirus software generally runs at the highly trusted kernel level of the operating system, creating a potential avenue of attack.

In addition to the drawbacks mentioned above, the effectiveness of antivirus software has also been researched and debated. One study found that the detection success of major antivirus software dropped over a one-year period.

The Core

The core of the Sun is considered to extend from the center to about 0.2 to 0.25 solar radii.It has a density of up to 150 g/cm(about 150 times the density of water) and a temperature of close to 13,600,000 K (by contrast, the surface of the Sun is around 5,800 K). Recent analysis of SOHO mission data favors a faster rotation rate in the core than in the rest of the radiative zone.

Through most of the Sun's life, energy is produced by nuclear fusion through a series of steps called the p–p (proton–proton) chain; this process converts hydrogen into helium.[35] Less than 2% of the helium generated in the Sun comes from the CNO cycle.

The core is the only location in the Sun that produces an appreciable amount of heat through fusion; inside 24% of the Sun's radius, 99% of the power has been generated, and by 30% of the radius, fusion has stopped nearly entirely. The rest of the star is heated by energy that is transferred outward from the core and the layers just outside. The energy produced by fusion in the core must then travel through many successive layers to the solar photosphere before it escapes into space as sunlight or kinetic energy of particles.

The proton–proton chain occurs around 9.2 × 1037 times each second in the core of the Sun. Since this reaction uses four free protons (hydrogen nuclei), it converts about 3.7 × 1038 protons to alpha particles (helium nuclei) every second (out of a total of ~8.9 × 1056 free protons in the Sun), or about 6.2 × 1011 kg per second.Since fusing hydrogen into helium releases around 0.7% of the fused mass as energy,the Sun releases energy at the mass-energy conversion rate of 4.26 million metric tons per second, 384.6 yottawatts (3.846×1026 W),or 9.192 × 1010 megatons of TNT per second. This mass is not destroyed to create the energy, rather, the mass is carried away in the radiated energy, as described by the concept of mass-energy equivalence.

The energy production per unit time (power) produced by fusion in the core varies with distance from the solar center. At the center of the Sun, fusion power is estimated by model to be about 276.5 watts/m3,a power production density which more nearly approximates reptile metabolism than a thermonuclear bomb.Peak power production in the Sun has been compared to the volumetric heats generated in an active compost heap. The tremendous power output of the Sun is not due to its high power per volume, but instead due to its large size.

The fusion rate in the core is in a self-correcting equilibrium: a slightly higher rate of fusion would cause the core to heat up more and expand slightly against the weight of the outer layers, reducing the fusion rate and correcting the perturbation; and a slightly lower rate would cause the core to cool and shrink slightly, increasing the fusion rate and again reverting it to its present level.


The gamma rays (high-energy photons) released in fusion reactions are absorbed in only a few millimeters of solar plasma and then re-emitted again in random direction (and at slightly lower energy)—so it takes a long time for radiation to reach the Sun's surface. Estimates of the "photon travel time" range between 10,000 and 170,000 years.

After a final trip through the convective outer layer to the transparent "surface" of the photosphere, the photons escape as visible light. Each gamma ray in the Sun's core is converted into several million visible light photons before escaping into space. Neutrinos are also released by the fusion reactions in the core, but unlike photons they rarely interact with matter, so almost all are able to escape the Sun immediately. For many years measurements of the number of neutrinos produced in the Sun were lower than theories predicted by a factor of 3. This discrepancy was recently resolved through the discovery of the effects of neutrino oscillation: the Sun emits the number of neutrinos predicted by the theory, but neutrino detectors were missing 2⁄3 of them because the neutrinos had changed flavor.

Characteristics Of Sun

The Sun is a G-type main sequence star comprising about 99.8632% of the total mass of the Solar System. It is a near-perfect sphere, with an oblateness estimated at about 9 millionths,which means that its polar diameter differs from its equatorial diameter by only 10 km (6 mi). As the Sun exists in a plasmatic state and is not solid, it rotates faster at its equator than at its poles. This behavior is known as differential rotation, and is caused by convection in the Sun and the movement of mass, due to steep temperature gradients from the core outwards. This mass carries a portion of the Sun’s counter-clockwise angular momentum, as viewed from the ecliptic north pole, thus redistributing the angular velocity. The period of this actual rotation  is approximately 25.6 days at the equator and 33.5 days at the poles. However, due to our constantly changing vantage point from the Earth as it orbits the Sun, the apparent rotation of the star at its equator is about 28 days.

The centrifugal effect of this slow rotation is 18 million times weaker than the surface gravity at the Sun's equator. The tidal effect of the planets is even weaker, and does not significantly affect the shape of the Sun.

The Sun is a Population I, or heavy element-rich,star.The formation of the Sun may have been triggered by shockwaves from one or more nearby supernovae.This is suggested by a high abundance of heavy elements in the Solar System, such as gold and uranium, relative to the abundances of these elements in so-called Population II (heavy element-poor) stars. These elements could most plausibly have been produced by endergonic nuclear reactions during a supernova, or by transmutation through neutron absorption inside a massive second-generation star.

The Sun does not have a definite boundary as rocky planets do, and in its outer parts the density of its gases drops exponentially with increasing distance from its center.Nevertheless, it has a well-defined interior structure, described below. The Sun's radius is measured from its center to the edge of the photosphere. This is simply the layer above which the gases are too cool or too thin to radiate a significant amount of light, and is therefore the surface most readily visible to the naked eye.

The solar interior is not directly observable, and the Sun itself is opaque to electromagnetic radiation. However, just as seismology uses waves generated by earthquakes to reveal the interior structure of the Earth, the discipline of helioseismology makes use of pressure waves (infrasound) traversing the Sun's interior to measure and visualize the star's inner structure.Computer modeling of the Sun is also used as a theoretical tool to investigate its deeper layers.

Sun

The Sun is the star at the center of the Solar System. It has a diameter of about 1,392,000 kilometers (865,000 mi), about 109 times that of Earth, and its mass (about 2 × 1030 kilograms, 330,000 times that of Earth) accounts for about 99.86% of the total mass of the Solar System.About three quarters of the Sun's mass consists of hydrogen, while the rest is mostly helium. Less than 2% consists of heavier elements, including oxygen, carbon, neon, iron, and others.

The Sun's color is white, although from the surface of the Earth it may appear yellow because of atmospheric scattering of blue light.Its stellar classification, based on spectral class, is G2V, and is informally designated a yellow star, because its visible radiation is most intense in the yellow-green portion of the spectrum.In this spectral class label, G2 indicates its surface temperature of approximately 5,778 K (5,505 °C; 9,941 °F), and V (Roman five) indicates that the Sun, like most stars, is a main sequence star, and thus generates its energy by nuclear fusion of hydrogen nuclei into helium. In its core, the Sun fuses 430–600 million tons of hydrogen each second. Once regarded by astronomers as a small and relatively insignificant star, the Sun is now presumed to be brighter than about 85% of the stars in the Milky Way galaxy, most of which are red dwarfs.The absolute magnitude of the Sun is +4.83; however, as the star closest to Earth, the Sun is the brightest object in the sky with an apparent magnitude of −26.74.The Sun's hot corona continuously expands in space creating the solar wind, a stream of charged particles that extends to the heliopause at roughly 100 astronomical units. The bubble in the interstellar medium formed by the solar wind, the heliosphere, is the largest continuous structure in the Solar System.

The Sun is currently traveling through the Local Interstellar Cloud in the Local Bubble zone, within the inner rim of the Orion Arm of the Milky Way galaxy. Of the 50 nearest stellar systems within 17 light-years from Earth (the closest being a red dwarf named Proxima Centauri at approximately 4.2 light years away), the Sun ranks 4th in mass. The Sun orbits the center of the Milky Way at a distance of approximately 24,000–26,000 light years from the galactic center, completing one clockwise orbit, as viewed from the galactic north pole, in about 225–250 million years. Since our galaxy is moving with respect to the cosmic microwave background radiation (CMB) in the direction of constellation Hydra with a speed of 550 km/s, the sun's resultant velocity with respect to the CMB is about 370 km/s in the direction of Crater or Leo.

The mean distance of the Sun from the Earth is approximately 149.6 million kilometers (1 AU), though this varies as the Earth moves from perihelion in January to aphelion in July. At this average distance, light travels from the Sun to Earth in about 8 minutes and 19 seconds. The energy of this sunlight supports almost all life on Earth by photosynthesis,and drives Earth's climate and weather. The enormous effect of the Sun on the Earth has been recognized since prehistoric times, and the Sun has been regarded by some cultures as a deity. An accurate scientific understanding of the Sun developed slowly, and as recently as the 19th century prominent scientists had little knowledge of the Sun's physical composition and source of energy. This understanding is still developing; there are a number of present-day anomalies in the Sun's behavior that remain unexplained.