بليز ساعدوني باقرب وقت

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هاااي ..

 

شلونكم ! عساكم بخير

 

ابيكم تساعدوني لموضوع الانج 102 لبروجيكت ويكون طويل

لان بسويه في البوربونت ..

 

بأقرب وووووقت .. لان ماشي وقت عن موعد التسليم

 

ومشكوورين مقدماا << ترى البنت وااثقه

[MOOSAABDULLA]

هاي 2

 

عن شنو بيكون البروكجت ؟؟ (( المواضيع المطلوبة لو ممكن ، وبشوف اذا كانت متوفرة ))

[جرح انسانه]

تفضلي

 

وهاي تقرير اول

 

انج102 :-

 

Venus

I INTRODUCTION

 

interactivity

Orbit

 

Venus (planet), one of the planets in the solar system, the second in distance from the Sun. Except for the Sun and the Moon, Venus is the brightest object in the sky. The planet is called the morning star when it appears in the east at sunrise, and the evening star when it is in the west at sunset. In ancient times the evening star was called Hesperus and the morning star Phosphorus or Lucifer. Because of the distances of the orbits of Venus and Earth from the Sun, Venus is never visible more than three hours before sunrise or three hours after sunset.

 

 

 

Venus Venus is the brightest object in our sky, after the sun and moon. Swirling clouds of sulfur and sulfuric acid obscure Venus’s surface and inhibited study of the planet from Earth until technology permitted space vehicles, outfitted with probes, to visit it. These probes determined that Venus is the hottest of the planets, with a surface temperature of about 460° C (about 860° F). Scientists believe that a greenhouse effect causes the extreme temperature, hypothesizing that the planet’s thick clouds and dense atmosphere trap energy from the sun.Photo Researchers, Inc./NASA/Science Source

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When viewed through a telescope, the planet exhibits phases like the Moon. Maximum brilliance (a stellar magnitude of -4.4, 15 times as bright as the brightest star) is seen in the crescent phase when Venus is closer to Earth. Venus’s full phase appears smaller and dimmer because it occurs when the planet is on the far side of the Sun from Earth. The phases and positions of Venus in the sky repeat every 1.6 years (see Time; Year). Transits of Venus (when the planet moves across the face of the Sun as seen from Earth) are rare, occurring in pairs at intervals of a little more than a century. The next two transits will be in 2004 and 2012.

 

II EXPLORATION

 

Magellan Spacecraft The Magellan probe to Venus mapped almost all of the planet’s surface and provided scientists with a vast amount of data. The probe is shown here in the cargo bay of the space shuttle Atlantis before the shuttle’s 1989 launch. Magellan reached Venus in 1990.NASA

 

Venus's complete cloud cover and deep atmosphere make it difficult to study from Earth. Most knowledge of the planet has been obtained through the use of space vehicles, particularly those carrying probes that descend through the atmosphere. The first flyby was that of Mariner 2, launched by the United States in 1962, followed by Mariner 5 in 1967 and Mariner 10 in 1974. The former Union of Soviet Socialist Republics developed several entry probes, some combined with flybys or orbiters: Venera 4 and 5 (1967), 6 (1969), 7 (1970), 8 (1972), 9 and 10 (1975), 11 and 12 (1978), 13 and 14 (1981), and 15 and 16 (1983); Vega 1 and 2, sent toward Halley's comet in 1984, also flew by Venus and released descent capsules. Several of these probes successfully reached the planet's surface. The United States sent two Pioneer Venus missions in 1978. Pioneer Venus 2 sent four probes to the surface, while the remaining craft explored the upper atmosphere. Pioneer Venus 1, an orbiter, measured the upper atmosphere for 14 years. The Magellan probe, launched toward Venus in 1989, transmitted radar images of the planet from 1990 to 1994.

 

 

III ATMOSPHERE

 

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The atmosphere of the planet consists of 97 percent carbon dioxide (CO2) and is so thick that the surface pressure is 96 bars (compared with 1 bar on Earth). The surface temperature on Venus varies little from place to place and is extremely hot, about 462°C (736 K/864°F). The high surface temperature is explained by an intense greenhouse effect. Even though only a small percentage of the solar energy that falls on Venus reaches the surface, the planet stays hot because the thick atmosphere prevents the energy from escaping.

 

facts and figures

facts and

figures

Venus (planet)

 

That nearly all of Venus's atmosphere is CO2 is not as strange as it might seem; in fact, the crust of Earth contains almost as much CO2 chemically bound in the form of limestone. About 3 percent of the Venusian atmosphere is nitrogen gas (N2). By contrast, 78 percent of Earth's atmosphere is nitrogen. Water and water vapor are extremely rare on Venus. Many scientists argue that Venus, being closer to the Sun, was subjected to a so-called runaway greenhouse effect, which caused any oceans to evaporate into the atmosphere. The hydrogen atoms of the water molecules could have been lost to space and the oxygen atoms to the crust. Another possibility is that Venus had very little water to begin with.

 

Cloud particles on Venus mostly consist of concentrated sulfuric acid. Earth’s atmosphere also contains a very thin haze of sulfuric acid particles in the stratosphere. On Earth, however, sulfuric acid does not build up because rain carries it down to react with surface materials. On Venus the acid evaporates at the cloud base, which lies about 50 km (31 mi) above the surface, and so remains in the atmosphere. The upper parts of the clouds, visible from Earth and from Pioneer Venus 1, extend as haze 70 to 80 km (44 to 50 mi) above the surface. The clouds contain a pale yellow impurity, better detected at near-ultraviolet wavelengths. Variations in the sulfur dioxide content of the atmosphere may indicate active volcanism on the planet.

 

Certain cloud patterns and weather features that can be discerned in the cloud tops give some information about wind motion in the atmosphere. The upper-level winds circle the planet at 360 km/h (225 mph). These winds cover the planet completely, blowing toward the east at virtually every latitude from equator to pole. The motions of descending probes, however, have shown that the bulk of Venus's tremendously dense atmosphere, closer to the planet's surface, is almost stagnant. From the surface up to 10 km (6 mi) altitude, wind speeds are only about 3 to 18 km/h (2 to 11 mph). The high-*****sss winds probably result from the transfer of momentum from Venus's slow-moving, massive lower atmosphere to higher altitudes where the atmosphere is less massive, so that the same momentum results in a much higher velocity.

 

The upper atmosphere and ionosphere were studied in great detail by Pioneer Venus 1, which passed through them once each day. On Earth this region is very hot; on Venus it is not, even though Venus is closer to the Sun. Surprisingly, on the night side of Venus the upper atmosphere is extremely cold. (Day-side temperatures are 40°C/104°F, compared to night-side temperatures of -170°C/-274°F.) Scientists believe that strong winds blow from the day side toward the near vacuum that is caused by the low temperatures on the night side. Such winds would carry along light gases, such as hydrogen and helium, which are concentrated in a night-side “bulge.”

 

In contrast to the very large antenna needed for Earth-based radar mapping of Venus, a modest instrument on Pioneer Venus 1 was able to conduct a nearly global survey. Combined with data from the Soviet probes, the Magellan orbiter, and Earth-based radar, the survey shows that the surface of Venus is primarily a rolling plain interrupted by two continent-sized highland areas, which have been named Ishtar Terra and Aphrodite Terra after two manifestations of the goddess Venus. Aphrodite Terra, although not as high as Ishtar Terra, extends nearly halfway around the equatorial region; it occupies the planet's far side as viewed from Earth at closest approach.

 

The more powerful radar aboard the Magellan spacecraft has revealed huge volcanoes, large solidified lava flows, and a large array of meteorite craters. The largest impact crater is almost 300 km (190 mi) across—the smallest about 5 km (3 mi). Although the probe's radar could resolve even smaller craters, if any were present, Venus's dense atmosphere apparently prevents smaller meteorites from impacting the surface of the planet. It is believed that all craters older than about 500 million years have been obliterated, while the more recent ones show little sign of modification.

 

The global survey and other probes have also revealed evidence that a great deal of tectonic activity has taken place on Venus, at least in the past. Such evidence includes ridges, canyons, a troughlike depression that extends across 1400 km (870 mi) of the surface, and a gigantic volcanic cone whose base is more than 700 km (435 mi) wide. The Soviet probes sent back photographs of the areas in which they set down, and also measured the natural radioactivity of the rocks. The radioactivity resembles that of granite and strongly suggests that the material of Venus is differentiated, or chemically separated, by volcanic activity. Angular rocks that are visible in the Soviet pictures also suggest the existence of geologic activity that would counteract the forces of erosion.

 

وهاي تقرير ثاني

 

Dinosaurs

 

Scientists think the first dinosaurs lived about 230 million years ago in the Triassic Period. Most dinosaurs became extinct at the end of the Cretaceous Period (about 65 million years ago), so that dinosaurs were around for nearly 165 million years!

 

The largest dinosaurs were over 100 feet (30 m) long and up to 50 feet (15 m) tall (like Argentinosaurus, Seismosaurus, Ultrasauros, Brachiosaurus, and Supersaurus). The smallest dinosaurs, like Compsognathus, were about the size of a chicken. Most dinosaurs were in-between. It is very difficult to figure out how the dinosaurs sounded, how they behaved, how they mated, what color they were, or even how to tell whether a fossil was male or female.A dinosaur can be named for the place where it was first found or because it has a unique body part – say a crest on its head or a very long neck. The meat eaters (carnivores) ate other dinosaurs, turtles, lizards, eggs or small mammals. Most dinosaurs, though, were plant-eaters (herbivores) and ate pine needles, ferns, mosses, rushes and other plants. A few may have been omnivorous, that is they ate whatever they could find – meat and plants. Dinosaurs probably didn't talk to each other the way humans do, but there were ways – sounds, movement, skin colors and even the shapes of their heads or crests – that dinosaurs could send messages like modern-day animals. Some adult dinosaurs lived pretty much on their own. Others lived their whole lives in herds. Many of the large plant-eating dinosaurs stayed together for protection or nested in groups to guard the eggs and feed the hatchlings. The dinosaurs went extinct about 65 million years ago, at the end of the Cretaceous period, which was a time of high volcanic and tectonic activity. There are a lot of theories why the extinction occurred. The most widely accepted theory is that an asteroid impact caused major climactic changes to which the dinosaurs couldn't adapt.

 

 

 

We must do something to save the wildlife; because it’s in dander. And we mean that the wildlife is animals and plants that live in natural conditions. People always kill the animals and destroys the area that have plants, and it’s the reason of what is the wildlife in danger.

 

 

 

 

 

*****

 

 

writing ENG 102

 

 

My dream bedroom

 

I like my bedroom because it is the place where I spend most of my time; I think that it is the best place at home. Let me tell you more about it.

 

I have comfortable, small, square, light blue bedroom. There is a table next to my bed, and there is a dressing table in front of floral curtains. There is a small rug above a floral carpet. I have a stereo system beside my chair. However, if I had enough money, I would make some changes in my bedroom. I would put some spotlights, and I would put red curtains. And also I would buy a small TV and some funny pictures.

 

If I wasn’t able to do all that, I think that my room is still the best and the way it doesn’t matter a lot as long as it is comfortable

 

وهاي تقرير بعد

 

 

تقرير انج 102 عن النظام الشمسي (Solar System)

 

 

 

Solar System, the Sun and the celestial bodies orbiting the Sun, including the nine planets and their satellites; the asteroids and comets; and interplanetary dust and gas. The term may also refer to a group of celestial bodies orbiting another star. Solar system refers to the system that includes Earth and the Sun. The dimensions of the solar system are specified in terms of the mean distance from Earth to the Sun, called the astronomical unit (AU). One AU is 150 million km (about 93 million miles). The most distant known planet, Pluto, orbits about 39 AU from the Sun. The boundary between the solar system and interstellar space—called the heliopause—is estimated to occur near 100 AU. Comets, however, achieve the greatest distance from the Sun; they have highly eccentric orbits ranging out to 50,000 AU or more.

 

The solar system was the only planetary system known to exist around a star similar to the Sun until 1995. Since then, astronomers have found planets and disks of dust in the process of forming planets around many other stars. Most astronomers think it likely that solar systems of some sort are numerous throughout the universe.

 

The Sun and the Solar Wind

 

The Sun is a typical star of intermediate size and luminosity. Sunlight and other radiation are produced by the conversion of hydrogen into helium in the Sun’s hot.

 

For all the Sun’s steadiness, it is an extremely active star. On its surface, dark sunspots bounded by intense magnetic fields come and go in 11-year cycles and sudden bursts of charged particles from solar flares can cause auroras and disturb radio signals on Earth. A continuous stream of protons, electrons, and ions also leaves the Sun and moves out through the solar system. This solar wind shapes the ion tails of comets and leaves its traces in the lunar soil.

 

The Major Planets

 

Nine major planets are currently known. They are commonly divided into two groups: the inner planets (Mercury, Venus, Earth, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune). The inner planets are small and are composed primarily of rock and iron. The outer planets are much larger and consist mainly of hydrogen, helium, and ice. Pluto does not belong to either group, and there is an ongoing debate as to whether Pluto should be categorized as a major planet.

 

Mercury is surprisingly dense, apparently because it has an unusually large iron core. With only a transient atmosphere, Mercury has a surface that still bears the record of bombardment by asteroidal bodies early in its history. Venus has a carbon dioxide atmosphere 90 times thicker than that of Earth, causing an efficient greenhouse effect by which the Venusian atmosphere is heated. The resulting surface temperature is the hottest of any planet—about 477°C (about 890°F). Earth is the only planet with abundant liquid water and known life. Strong evidence exists that Mars once had liquid water on its surface, but now its carbon dioxide atmosphere is so thin that the planet is dry and cold, with polar caps of frozen water and solid carbon dioxide, or dry ice.

 

Jupiter is the largest of the planets. Its hydrogen and helium atmosphere contains pastel-colored clouds, and its immense magnetosphere rings, and satellites make it a planetary system unto itself.

 

At least four of Jupiter’s moons have atmospheres, and at least three show evidence that they contain liquid or partially-frozen water. Saturn rivals Jupiter, with a much more intricate ring structure and a similar number of satellites.

 

Uranus and Neptune are deficient in hydrogen compared with Jupiter and Saturn; Uranus, also ringed, has the distinction of rotating at 98° to the plane of its orbit. Pluto seems similar to the larger, icy satellites of Jupiter or Saturn. Pluto is so distant from the Sun and so cold that methane freezes on its surface.

 

Movements of the Planets and Their Satellites

 

If one could look down on the solar system from far above the North Pole of Earth, the planets would appear to move around the Sun in a counterclockwise direction. All of the planets except Venus and Uranus rotate on their axes in this same direction. The entire system is remarkably flat—only Mercury and Pluto have obviously inclined orbits. Pluto’s orbit is so elliptical that it is sometimes closer than Neptune to the Sun.

 

The satellite systems mimic the behavior of their parent planets and move in a counterclockwise direction, but many exceptions are found. Jupiter, Saturn, and Neptune each have at least one satellite that moves around the planet in a retrograde orbit (clockwise instead of counterclockwise), and several satellite orbits are highly elliptical. Jupiter, moreover, has trapped two clusters of asteroids (the so-called Trojan asteroids) leading and following the planet by 60° in its orbit around the Sun. (Some satellites of Saturn have done the same with smaller bodies.) The comets exhibit a roughly spherical distribution of orbits around the Sun.

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السلام عليكم

 

مشوكورين وما تقصرون ان شاء الله اقدار اساعدكم في اي شيء تبونه

 

 

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