Counter Strike 1.6 – SK Gaming
Counter Strike 1.6 – SK Gaming
Download this Counter Strike 1.6 – Click Here
It’s modified version of Counter Strike 1.6 (CS 1.6) game, it’s version 48 of CS 1.6 game released few year’s ago and counted a huge amount of this game version fan’s. This game version have a lot of fan’s (players who play CS 1.6 with version 48 build of CS game), because in this version of the game you will find fixed a lot of game bug’s, updated graphics (player’s and gun’s model’s), updated sound’s, details of the map’s and much more. With CS 1.6 V48 you can join any CS 1.6 game server (Protocol 47, protocol 48 and double protocol – 47+48), this version of the game have only one bad thing – With this version of the game you will not be able to join STEAMED CS 1.6 game server if you will use NON-STEAM game version, but this thing you will find not only in version 48 of CS 1.6 game, all non steam game version’s have that problem.
The first video and computer games, such as NIMROD (1951), OXO (1952), and Spacewar! (1962), were for one or two players sitting at a single computer which was being used only to play the game. Later in the 1960s, computers began to support time-sharing, which allowed multiple users to share use of a computer simultaneously. Systems of computer terminals were created allowing users to operate the computer from a different room than where the computer was housed. Soon after, Modem links further expanded this range so that users did not have to be in the same building as the computer; terminals could connect to their host computers via dial-up or leased telephone lines. With the increased remote access, “host based” games were created, in which users on remote systems connected to a central computer to play single-player, and soon after, multiplayer games.
Later, in the 1970s, packet-based computer networking technology began to mature. Between 1973 and 1975, Xerox PARC developed Local Area Networks based on Ethernet. Additionally, the Wide Area Network ARPANET further developed from its 1969 roots, lead to the creation of the Internet on January 1, 1983. These LANs and WANS allowed for network games, where the game created and received network packets; Systems located across LANs or the Internet could run games with each other in peer-to-peer or client–server models
In the early 1970s, the PLATO time-sharing system, created by the University of Illinois and Control Data Corporation allowed students at several locations to use online lessons in one of the earliest systems for computer aided instruction. In 1972, PLATO IV terminals with new graphics capabilities were introduced, and students started using this system to create multiplayer games. By 1978, PLATO had multiplayer interactive graphical dungeon crawls, air combat (Airfight), tank combat, space battles (Empire and Spasim), with features such as inter-player messaging, persistent game characters, and team play for at least 32 simultaneous players.
A key goal of early network systems such as ARPANET and JANET was to allow users of “dumb” text-based terminals attached to one host computer (or, later, to terminal servers) to interactively use programs on other host computers. This meant that games on those systems were accessible to users in many different locations by use of programs such as telnet.
Most of the early host-based games were single-player, and frequently originated and were primarily played at universities. A sizable proportion were written on DEC-20 mainframes, as those had a strong presence in the university market. Games such as The Oregon Trail (1971), Colossal Cave Adventure (1976), and Star Trek (1972) were very popular, with several or many students each playing their own copy of the game at once, time-sharing the system with each other and users running other programs.
Eventually, though, multiplayer host-based games on networked computers began to be developed. One of the most important of these was MUD (1978), a program which spawned a genre and had significant input into the development of concepts of shared world design, having formative impact on the evolution of MMORPG’s. In 1984, MAD debuted on BITNET; this was the first MUD fully accessible from a worldwide computer network. During its two-year existence, 10% of the sites on BITNET connected to it. In 1988, another BITNET MUD named MUDA appeared. It lasted for five years, before going off line due to the retirement of the computers it ran on.
In the summer of 1973, Maze War was first written at NASA’s Ames Research Center in California by high school summer interns using Imlac PDS-1 computers. The authors added two-player capability by connecting two IMLAC computers with serial cables. Since two computers were involved, as opposed to “dumb terminals”, they could use formatted protocol packets to send information to each other, so this could be considered the first peer-to-peer computer video game. It could also be called the first First person shooter.
In 1983, Gary Tarolli wrote a flight simulator demonstration program for Silicon Graphics workstation computers. In 1984, networking capabilities were added by connecting two machines using serial cables just as had been done with the IMLACs for Mazewar at NASA eleven years earlier. Next, XNS support was added, allowing multiple stations to play over an Ethernet, just as with the Xerox version of Mazewar. In 1986, UDP support was added (port 5130), making SGI Dogfight the first game to ever use the Internet protocol suite. The packets used, though, were broadcast packets, which meant that the game was limited to a single network segment; it could not cross a router, and thus could not be played across the Internet. Around 1989, IP Multicast capability was added, and the game became playable between any compatible hosts on the Internet, assuming that they had multicast access (which was quite uncommon). The multicast address is 220.127.116.11, making this only the third multicast application (and the first game) to receive an address assignment, with only the VMTP protocol (18.104.22.168) and the Network Time Protocol (22.214.171.124) having arrived earlier.
Eclipses can only occur when the Sun, Earth, and Moon are all in a straight line (termed “syzygy”). Solar eclipses occur at new moon, when the Moon is between the Sun and Earth. In contrast, lunar eclipses occur at full moon, when Earth is between the Sun and Moon. The apparent size of the Moon is roughly the same as that of the Sun, with both being viewed at close to one-half a degree wide. The Sun is much larger than the Moon but it is the precise vastly greater distance that gives it the same apparent size as the much closer and much smaller Moon from the perspective of Earth. The variations in apparent size, due to the non-circular orbits, are nearly the same as well, though occurring in different cycles. This makes possible both total (with the Moon appearing larger than the Sun) and annular (with the Moon appearing smaller than the Sun) solar eclipses. In a total eclipse, the Moon completely covers the disc of the Sun and the solar corona becomes visible to the naked eye. Because the distance between the Moon and Earth is very slowly increasing over time, the angular diameter of the Moon is decreasing. Also, as it evolves toward becoming a red giant, the size of the Sun, and its apparent diameter in the sky, are slowly increasing.[l] The combination of these two changes means that hundreds of millions of years ago, the Moon would always completely cover the Sun on solar eclipses, and no annular eclipses were possible. Likewise, hundreds of millions of years in the future, the Moon will no longer cover the Sun completely, and total solar eclipses will not occur.
Because the Moon’s orbit around Earth is inclined by about 5° to the orbit of Earth around the Sun, eclipses do not occur at every full and new moon. For an eclipse to occur, the Moon must be near the intersection of the two orbital planes. The periodicity and recurrence of eclipses of the Sun by the Moon, and of the Moon by Earth, is described by the saros, which has a period of approximately 18 years.
Because the Moon is continuously blocking our view of a half-degree-wide circular area of the sky,[m] the related phenomenon of occultation occurs when a bright star or planet passes behind the Moon and is occulted: hidden from view. In this way, a solar eclipse is an occultation of the Sun. Because the Moon is comparatively close to Earth, occultations of individual stars are not visible everywhere on the planet, nor at the same time. Because of the precession of the lunar orbit, each year different stars are occulted.
Understanding of the Moon’s cycles was an early development of astronomy: by the 5th century BC, Babylonian astronomers had recorded the 18-year Saros cycle of lunar eclipses, and Indian astronomers had described the Moon’s monthly elongation. The Chinese astronomer Shi Shen (fl. 4th century BC) gave instructions for predicting solar and lunar eclipses. Later, the physical form of the Moon and the cause of moonlight became understood. The ancient Greek philosopher Anaxagoras (d. 428 BC) reasoned that the Sun and Moon were both giant spherical rocks, and that the latter reflected the light of the former. Although the Chinese of the Han Dynasty believed the Moon to be energy equated to qi, their ‘radiating influence’ theory also recognized that the light of the Moon was merely a reflection of the Sun, and Jing Fang (78–37 BC) noted the sphericity of the Moon. In the 2nd century AD Lucian wrote a novel where the heroes travel to the Moon, which is inhabited. In 499 AD, the Indian astronomer Aryabhata mentioned in his Aryabhatiya that reflected sunlight is the cause of the shining of the Moon. The astronomer and physicist Alhazen (965–1039) found that sunlight was not reflected from the Moon like a mirror, but that light was emitted from every part of the Moon’s sunlit surface in all directions. Shen Kuo (1031–1095) of the Song dynasty created an allegory equating the waxing and waning of the Moon to a round ball of reflective silver that, when doused with white powder and viewed from the side, would appear to be a crescent.
the Moon marked the boundary between the spheres of the mutable elements (earth, water, air and fire), and the imperishable stars of aether, an influential philosophy that would dominate for centuries. However, in the 2nd century BC, Seleucus of Seleucia correctly theorized that tides were due to the attraction of the Moon, and that their height depends on the Moon’s position relative to the Sun. In the same century, Aristarchus computed the size and distance of the Moon from Earth, obtaining a value of about twenty times the radius of Earth for the distance. These figures were greatly improved by Ptolemy (90–168 AD): his values of a mean distance of 59 times Earth’s radius and a diameter of 0.292 Earth diameters were close to the correct values of about 60 and 0.273 respectively. Archimedes (287–212 BC) designed a planetarium that could calculate the motions of the Moon and other objects in the Solar System.
During the Middle Ages, before the invention of the telescope, the Moon was increasingly recognised as a sphere, though many believed that it was “perfectly smooth”.
In 1609, Galileo Galilei drew one of the first telescopic drawings of the Moon in his book Sidereus Nuncius and noted that it was not smooth but had mountains and craters. Telescopic mapping of the Moon followed: later in the 17th century, the efforts of Giovanni Battista Riccioli and Francesco Maria Grimaldi led to the system of naming of lunar features in use today. The more exact 1834–36 Mappa Selenographica of Wilhelm Beer and Johann Heinrich Mädler, and their associated 1837 book Der Mond, the first trigonometrically accurate study of lunar features, included the heights of more than a thousand mountains, and introduced the study of the Moon at accuracies possible in earthly geography. Lunar craters, first noted by Galileo, were thought to be volcanic until the 1870s proposal of Richard Proctor that they were formed by collisions. This view gained support in 1892 from the experimentation of geologist Grove Karl Gilbert, and from comparative studies from 1920 to the 1940s, leading to the development of lunar stratigraphy, which by the 1950s was becoming a new and growing branch of astrogeology.
The Cold War-inspired Space Race between the Soviet Union and the U.S. led to an acceleration of interest in exploration of the Moon. Once launchers had the necessary capabilities, these nations sent unmanned probes on both flyby and impact/lander missions. Spacecraft from the Soviet Union’s Luna program were the first to accomplish a number of goals: following three unnamed, failed missions in 1958, the first human-made object to escape Earth’s gravity and pass near the Moon was Luna 1; the first human-made object to impact the lunar surface was Luna 2, and the first photographs of the normally occluded far side of the Moon were made by Luna 3, all in 1959.
The first spacecraft to perform a successful lunar soft landing was Luna 9 and the first unmanned vehicle to orbit the Moon was Luna 10, both in 1966. Rock and soil samples were brought back to Earth by three Luna sample return missions (Luna 16 in 1970, Luna 20 in 1972, and Luna 24 in 1976), which returned 0.3 kg total. Two pioneering robotic rovers landed on the Moon in 1970 and 1973 as a part of Soviet Lunokhod programme.
The United States launched unmanned probes to develop an understanding of the lunar surface for an eventual manned landing: the Jet Propulsion Laboratory’s Ranger program produced the first close-up pictures; the Lunar Orbiter program produced maps of the entire Moon; the Surveyor program landed its first spacecraft four months after Luna 9. NASA’s manned Apollo program was developed in parallel; after a series of unmanned and manned tests of the Apollo spacecraft in Earth orbit, and spurred on by a potential Soviet lunar flight, in 1968 Apollo 8 made the first crewed mission to lunar orbit. The subsequent landing of the first humans on the Moon in 1969 is seen by many as the culmination of the Space Race.
Neil Armstrong became the first person to walk on the Moon as the commander of the American mission Apollo 11 by first setting foot on the Moon at 02:56 UTC on 21 July 1969. An estimated 500 million people worldwide watched the transmission by the Apollo TV camera, the largest television audience for a live broadcast at that time. The Apollo missions 11 to 17 (except Apollo 13, which aborted its planned lunar landing) returned 380.05 kilograms (837.87 lb) of lunar rock and soil in 2,196 separate samples. The American Moon landing and return was enabled by considerable technological advances in the early 1960s, in domains such as ablation chemistry, software engineering and atmospheric re-entry technology, and by highly competent management of the enormous technical undertaking.
Scientific instrument packages were installed on the lunar surface during all the Apollo landings. Long-lived instrument stations, including heat flow probes, seismometers, and magnetometers, were installed at the Apollo 12, 14, 15, 16, and 17 landing sites. Direct transmission of data to Earth concluded in late 1977 due to budgetary considerations, but as the stations’ lunar laser ranging corner-cube retroreflector arrays are passive instruments, they are still being used. Ranging to the stations is routinely performed from Earth-based stations with an accuracy of a few centimetres, and data from this experiment are being used to place constraints on the size of the lunar core