Presentation on theme: "Our solar system's star, the Sun, has inspired mythological stories in cultures around the world, including those of the ancient Egyptians, the Aztecs."— Presentation transcript:
1Our solar system's star, the Sun, has inspired mythological stories in cultures around the world, including those of the ancient Egyptians, the Aztecs of Mexico, Native American tribes of North America and Canada, the Chinese, and many others. A number of ancient cultures built stone structures or modified natural rock formations to observe the Sun and Moon, they charted the seasons, created calendars, and monitored solar and lunar eclipses. These architectural sites show evidence of deliberate alignments to astronomical phenomena: sunrises, moonrises, moonsets, even stars or planets.THE SUN
2The Sun is the closest star to Earth, at a mean distance from our planet of million kilometers (92.96 million miles).This distance is known as an astronomical unit (abbreviated AU), and sets the scale for measuring distances all across the solar system.The Sun, a huge sphere of mostly ionized gas, supports life on Earth.It powers photosynthesis in green plants, and is ultimately the source of all food and fossil fuel.The connection and interactions between the Sun and Earth drive the seasons, ocean currents, weather, and climate
3Photosynthesis is the way a plant makes food for itself Photosynthesis is the way a plant makes food for itself. Chlorophyll in the "green" part of the leaves captures energy from the sun and this powers the building of food from very simple ingredients - carbon dioxide and water. Oxygen is released as a by-product of photosynthesis.Plants "breathe in" carbon dioxide and "breathe out" oxygen. They breathe through tiny holes in their leaves called stomata; they also lose water through the stomata.The tree draws up water through its roots and the water is then drawn up through the tree and comes out through the stomata in its leaves. The whole process of sucking up water and losing it again is called transpiration.
4PARTICLES MOVE THE MOST PLASMA = IONIZED GASPARTICLES MOVE THE MOST
5The rotation of the Earth, the revolution of the Earth around the Sun and the Moon around the Earth are the basis of terrestrial timekeeping.The solar day is measured using the passage of the mean Sun across the sky. It lasts 24 hours - the average interval between two successive midnights.Looking down to the north pole, the Earth rotates in an anticlockwise direction.
6The sidereal day is measured with respect to the stars The sidereal day is measured with respect to the stars. It lasts 23 hours 56 minutes and 4 seconds. This is the time between two successive passages of a star across the meridian - the line connecting the due north and south points on the horizon with the overhead point (the zenith).Each solar day the Earth rotates 360º with respect to the Sun. Similarly the Earth rotates 360º with respect to the background stars in a sidereal day. During each solar day, the motion of the Earth around the Sun means the Earth rotates 361º with respect to the background stars.
7The difference between the solar and sidereal days means that a given star will rise four minutes earlier each day. The diagrams illustrates how the constellation of Orion reaches the same position four minutes earlier on each successive day
8The year and the calendar The sidereal year is the time taken for the Earth to travel once around the Sun and return to the same place with respect to the background stars. It lasts days.Our calendar is based on the cycle of the seasons and the so-called 'tropical' year, which measures the time take for the Earth to travel from equinox to equinox. It lasts days, around 20 minutes less than the sidereal year.Almost the whole world now uses the Gregorian calendar. Most calendar years are rounded down to a length of 365 days, leaving an error of about ¼ day per year. After 4 years an extra correction day is added to make a leap year. This ensures that the calendar stays in step with the seasons.Even this correction produces a small error of days, which is corrected by a special rule for century years (1900, 2000 etc). These years are only leap years if they are exactly divisible by 400 with no remainder.
9THE SUN AND THE SEASONSEarth's equator is tilted at 23.5º to the plane of its orbit around the Sun, the ecliptic. The axis of rotation of the Earth always points to the same direction, towards the north celestial pole.Starting in December, the northern hemisphere of the Earth is tilted away from the Sun.North of the tropics, the Sun will appear to be lower in the sky and the days will be shorter, reaching a minimum length on December 21, the winter solstice.
10Sunlight hits the ground at a shallow angle, so the heat is spread out over a large area, making the weather colder. In the southern hemisphere, the Sun is high in the sky and it is summer.By March, both hemispheres of the Earth have days and nights of similar length. In the north, the Sun will now be higher in the sky. At the vernal equinox on about 22 March, the Sun is above the horizon for around 12 hours over most of the Earth's surface. The northern spring and southern autumn begin this month.Other side of globe is illuminated
11North of the tropics, the northern hemisphere has the longest days during June, when it is tilted towards the Sun.The Sun is high in the sky, so its heat strikes the ground at a steep angle leading to warmer weather.The Sun reaches its highest point on 21 June, the summer solstice. At this time of year, the part of the Earth to the south of the tropics is entering winter.
12In September, both hemispheres again have days and nights of similar length. At the autumnal equinox on 23 September, the Sun is again above the horizon for 12 hours across the globe. This month sees the onset of autumn in the northern hemisphere and spring south of the equator.
14In June Tromso never rotates into the Earth's shadow, experiencing 24 hours of daylight In Greenwich we experience long summer days and short nights At the equator days and nights are of equal length Sydney has short hours of daylight and long nights Equinoxes All points on the Earth experience days and nights of roughly 12 hours in length In December Tromso never rotates into daylight, experiencing continuous night Greenwich has short winter days and long nights At the equator days and nights are of equal length Sydney has long hours of daylight and short nights
15During the winter the Sun's radiation strikes the ground at a shallow angle and days are short. This results in cooler weather. However, during the summer the reverse is true; the Sun's radiation strikes the ground at a steeper angle, and the days are longer, resulting in warmer weather.In winter the Sun rises in the south-east and sets in the south-west. At the equinoxes the Sun rises in the east and sets in the west. In summer the Sun rises in the north-east and sets in the north-west.
16Questions to think about 1. Explain with a diagram why some places of the Earth have 24 hours of daylight and 24 hours of darkness for part of the year.2. Rewrite and correct the following statement:During the summer, the northern hemisphere of the Earth is tilted towards the Sun. This means that the UK is closer to the Sun and so the weather is warmer. In winter, it is tilted away from the Sun so the UK is further away and the weather is colder.3. Mars has an orbit where its distance from the Sun ranges from 210 to 250 million km. The southern winter takes place when it is furthest from the Sun and southern summer occurs when it is nearest. What effect will this have on the seasons in each hemisphere?4. Why do you think the view of the stars from Earth changes with the seasons?
17Data for the Sun dated on September 14, 2006. Sun Earth SunEarthRatio (Sun/Earth)Mass (1024 kg)1,989,1005.9736333,000Volume (1012 km3)1,412,0001.0831,304,000Average Radius (km)696,0006371109.2Average Density (kg/m3)140855150.255Surface Gravity at Equator (m/s2)274.09.7828.0Escape Velocity (km/s)617.711.255.2Rotation Rate at Equator (hours)609.1225.449Rotation Rate at Poles (hours)~ 936~ 39Axial Tilt7.25°23.45°0.309Ellipticity0.00340.015Polar Magnetic Field (gauss)1 to 20.30713.3 to 6.5Visual Magnitude-26.73-3.86N/AAbsolute Magnitude+4.83Luminosity (1024 J/s)384.6Mass Conversion Rate (106 kg/s)4300Average Energy Production (10-3 J/kg)0.1937Surface Emission (106 J/(m2 s))63.29Speed Relative to Nearby Stars (km/s)19.4Spectral TypeG2 Vdated on September 14, 2006.