Chapter 10The Sun, Our Star.ppt
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1、Chapter 10 The Sun, Our Star,The Sun support life on Earth The Sun provides energy for photosynthesis, which releases oxygen into the atmosphere. The greenhouse effect trap some of the solar energy on Earth, keeping it warm (at the right temperature for us). The Sun ultimately determines the fate of
2、 the life on Earth. The Sun is the only star that we can study in details. The Sun is the test bed for our theory of the stars.,General Properties Luninosity Solar Energy Internal Structure Solar Atmosphere Surface Features Magnetic Fields Solar Activities Solar Cycle,General Properties,Luminosity,
3、Watts, Joules, and Calories,LuminosityThe energy an object radiates per unit time. So, it is a measure of power. WattUnit of power. One watt is one Joule per second. JouleUnit of energy. Lifting a 1 kg (2.2 lb) mass up by 10 cm (4 inches) on the surface of Earth would requires 1 joule of energy. Acc
4、elerating a 2 kilograms (4.4 Pounds) mass from rest to a speed of 1 m/sec (2.25 miles/hour) requires 1 joule of energy. 1 Calories = 4.2 Joules. The Sun generates 9 1025 calories of energy every second, or 90,000,000,000,000,000,000,000,000 calories per second.,Solar Luminosity and Solar Constant,So
5、, how do we measure solar luminosity? The total energy output of the Sun can be derived from Stefan-Boltzmann Law If we know the size of the Sun is 700,000 km, that its surface temperature is 5,800 K, and assume it is radiating like a blackbody, then we can calculate the total energy the Sun is irra
6、diating per second (the luminosity) according to Stefan-Blotzmann Law. If we know the luminosity of the Sun is 3.81026 watts, and know that the distance between the Sun and the Earth is 1AU, then we can predict how much energy we should be receiving from the Sun just outside the Earths atmosphere So
7、lar Constant1366 w/m2, or 1.36 kW/m2The magnitude of energy flow from the Sun measured in a 1 m2 (or 10 ft 10 ft) area outside of the Earths atmosphere is measured to be 1366 joules every second. This is precisely what we predicted from Stefan-Boltzmann Law. The energy output of the Sun was thought
8、to be constant in time (but this is not strictly correct), therefore, it is referred to as the solar constant. 1300 watts of electric power is enough to Light thirteen 100 watts light bulbs Run 20 laptop PCs,Blackbody,A blackbody is an object that absorbs all electromagnetic radiation on it. It also
9、 irradiate a thermal radiation according to its temperature.,Solar Energy and Your Electricity Bill,In 2001, 107 million US households consumed 1,140 billion kWh of electricityhttp:/www.eia.doe.gov/emeu/reps/enduse/er01_us.html hWh: kilo-Watt hour 1 kW = 1000 Watt = 1000 juoles/sec 1 kWh = 1000 joul
10、es/sec 1 hour = 1000 joules/sec 3600 sec = 3.6 million joules Each US household needs 1.2 kW of electric power constantly 1,140 109 kWh 107 106 households 365 days 24 hour/day = 1.2 kWh per hour per household= 1.2 kW per household So, ideally, if you can build a solar energy collector with 100% effi
11、ciency, and that the Sun shines 24 hours a day, and the Earths atmosphere is completely transparent, and it is never cloudy, then you only need a solar energy collector with a size of 1 m2 to supply all your electricity need!,Of Course, in Reality,On the surface of the Earth, solar irradiance is red
12、uced due to the reflection and absorption by the atmosphere, and only about 1 kW is available near the equator It is always cloudy The Sun doesnt shine 24 hours a day Solar cell efficiency is about only 10% to 30% (very expansive material) Solar cells utilize an effect called photoelectric effect: w
13、hen photons with sufficient energy is illuminated on certain type of materials, the electrons in the materials can escape the bound of the atoms and become free electrons (in the material) to generate electric currentAlbert Einsteins theoretical work on photoelectric effect earned him the 1921 Nobel
14、 Prize in Physics.,Coming Homework Problem,According to the Hawaii Electric Company (HECO), its power generating capacity is approximately 1,700 MW (Mega Watts), or 1.7 109 Watts (1 Watt is 1 Joule per second), or 1.7 109 Joule per second (1 Joule is about 4.2 Calories). The amount of solar energy o
15、utside the Earths atmosphere is 1,300 Watt/m2, meaning if we can collect all the solar energy falling on a 1 m2 size solar energy collector; we can extract 1,300 Joule of energy per second. Assuming that after the absorption of the solar energy by the atmosphere, and the inefficiency of the solar en
16、ergy collector, we can get about 500 Watt/m2 on the ground. How big a solar energy collector (in unit of m2 or km2) do we need to completely replace the power generating capacity of HECO?,So, how does the Sun generate so much energy?,General Properties Internal Structure Source of Solar Energy How d
17、o we study the interior of the Sun Solar Atmosphere Surface Features Magnetic Fields Solar Activities Solar Cycle,The Energy Source of the Sun,This is a simplified picture thats not exactly correct. Electric charge is not conserved!,Before Einsteins special theory of relativity, the most plausible t
18、heory for the generation of the energy in the Sun was gravitational contraction: as the solar nebula collapses due to the gravitational pull of the denser core region, gravitational potential energy is converted into thermal energy. However, according to calculation, the Sun can sustain its energy o
19、utput for only about 25 million years if gravitational potential energy is the source of the solar energy. Today, we understand that the energy source of the Sun is the nuclear fusion process which combines hydrogen nuclei to form helium, and at the same time releasing a very large amount of energy
20、per reaction. The increase of temperature at the center of the Sun due to gravitational contraction eventually trigger nuclear fusion, which converts some of the mass into energy, according to Einsteins mass-energy equation, E = mc2.,The Internal Structure of the Sun,Core The region where nuclear fu
21、sion takes place to generate the solar energy. T 15 million degrees K. Radiation Zone Energy is transported outward primarily by photons traveling through this region. T 10 million degrees K and decreases outward. No nuclear fusion. Convection Zone Energy is transported through convection: hot gas r
22、ises, irradiates their energy, and becomes cold. Cold gas sink to the bottom. Example at home: boiling water. Example at play: glider and hang-glider.,The Equilibrium Between Gravity and Pressure,The temperature and density inside the Sun increase due to gravitational contraction. Without a force to
23、 counter gravitation force, the Sun will continue to contract. However, as the Sun contracts, the density and temperature of the interior also increase. This increases the thermal pressure of the interior, pushing outward against the gravitational force.,Gravitational force pulls the gas inward Ther
24、mal pressure push the gas outward When inward gravitational force is equal to the outward push of thermal pressure, the size of the Sun remains constantIf the mass of the Sun is high enough, the internal pressure and temperature can be high enough for nuclear fusion to begin,Why Does Nuclear Fusion
25、Occurs Only at the Center of the Sun?,Temperature & Density Temperature is a measurement of the average kinetic energy of the particles. A volume of gas at very high temperature means that the particles of the gas move at very high speed. The very high speed is needed to overcome the repulsive elect
26、romagnetic force between the protons to get them very close to each other. High density is necessary so that the probability of fusion is high. Once the protons are close to each other, the strong nuclear force can bind them together to make a new and heavier element.,Click on image to start animati
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