Understanding the Structure and Energy Production of the Sun
Explore the composition and nuclear fusion processes of the Sun through spectroscopy and the generation of energy via nuclear fusion using hydrogen nuclei. Discover how hydrogen and helium make up the majority of the Sun's mass, with multiple elements present in trace amounts. Learn about the steps of nuclear fusion in the Sun, culminating in the creation of helium nuclei and the release of energy.
Download Presentation
Please find below an Image/Link to download the presentation.
The content on the website is provided AS IS for your information and personal use only. It may not be sold, licensed, or shared on other websites without obtaining consent from the author. Download presentation by click this link. If you encounter any issues during the download, it is possible that the publisher has removed the file from their server.
E N D
Presentation Transcript
Structure of the Sun Mr. Villegas Astronomy Haltom HS
The Suns Energy Section 1
Composition of the Sun Using a device called a spectrograph, scientists break up the sun s light into a spectrum. Dark lines form in the spectra of stars when gases in the stars outer layers absorb specific wavelengths of the light that passes through the layers. By studying the spectrum of a star, scientists can determine the amounts of elements that are present in a star s atmosphere.
Composition of the Sun Because each element produces a unique pattern of spectral lines, astronomers can match the spectral lines of starlight to those of Earth s elements, and identify the elements in the star s atmosphere. Both hydrogen and helium occur in the sun. About 75% of the sun s mass is hydrogen, and hydrogen and helium together make up about 99% of the sun s mass. The sun s spectrum reveals that the sun contains traces of almost all other chemical elements.
Nuclear Fusion Nuclear fusion occurs inside the sun. Nuclei of hydrogen atoms are the primary fuel for the sun s fusion. Nuclear fusion produces most of the suns energy and consists of three steps.
Nuclear Fusion In the first step, two hydrogen nuclei, or protons, collide and fuse. In this step, the positive charge of one of the protons is neutralized as that proton emits a particle called a positron. As a result, the proton becomes a neutron and changes the original two protons into a proton- neutron pair.
Nuclear Fusion In the second step, another proton combines with this proton-neutron pair to produce a nucleus made up of two protons and one neutron. In the third step, two nuclei made up of two protons and one neutron collide and fuse. As this fusion happens, two protons are released. The remaining two protons and two neutrons are fused together and form a helium nucleus. At each step, energy is released
The Final Product One of the final products of the fusion of hydrogen in the sun is always a helium nucleus. The helium nucleus has about 0.7% less mass than the hydrogen nuclei that combined to form it do. The lost mass is converted into energy during the series of fusion reactions that forms helium. The energy released during the three steps of nuclear fusion causes the sun to shine and gives
Mass Changing into Energy The sun s energy comes from fusion, and the mass that is lost during fusion becomes energy. In 1905, Albert Einstein proposed that a small amount of matter yields a large amount of energy. This proposal was part of Einstein s special theory of relativity. This theory included the equation: E = mc2
Mass Changing into Energy In Einstein s equation E = mc2, E represents energy produced; m represents the mass; c represents the speed of light, which is about 300,000 km/s. Einstein s equation can be used to calculate the amount of energy produced from a given amount of matter.
Spot Question How did the equation E = mc2help scientists understand the energy of the sun? Einstein s equation helped scientists understand the source of the sun s energy. The equation explained how the sun could produce huge amounts of energy without burning up.
The Core The parts of the sun include the core, the radiative zone, and the convective zone. At the center of the sun is the core. The core makes up 25% of the sun s total diameter of 1,390,000 km. The temperature of the core is about 15,000,000 km C. The core is made up entirely of ionized gas, and is 10 times as dense as iron.
The Radiative Zone The radiative zone of the sun surrounds the core. The temperature of the radiative zone ranges from about 2,000,000 C to 7,000,000 C . In the radiative zone, energy moves outward in the form of electromagnetic waves
The Convective Zone The convective zone surrounds the radiative zone. The temperature of the convective zone is about 2,000,000 C. Energy produced in the core moves through this zone by convection. Convection is the transfer of energy
The Suns Atmosphere The sun s atmosphere surrounds the convective zone of the sun s core. Because the sun is made of gases, the term atmosphere refers to the uppermost region of solar gases. The sun s atmosphere has three layers: the photosphere, the chromosphere, and the corona.
The Photosphere Photosphere means sphere of light. The photosphere of the sun is the innermost layer of the sun s atmosphere. It is the visible surface of the sun The photosphere is made of gases that have risen from the convective zone. The temperature in the photosphere is about 6,000 C. Much of the energy given off from the photosphere is in the form of visible light.
Spot Question What layers make up the sun s atmosphere? The sun s atmosphere consists of the photosphere, the chromosphere, and the corona.
The Chromosphere The chromosphere lies just above the photosphere. The chromosphere s temperature ranges from 4,000 C to 50,000 C. Also known as the Color Sphere .
The Suns Outer Parts The corona is a huge region of gas that has a temperature above 1,000,000 C. As the corona expands, electrons and electrically charged particles called ions stream out into space. These particles make up solar wind, which flows outward from the sun to the rest of the solar system
Sunspots Sunspot are dark area cooler areas of the photosphere Magnetic fields cause convection to slow in parts of the convective zone. This causes a less energy to go from the core to the photosphere. Less energy makes these regions of the photosphere are considerably cooler. Cooler areas appear darker than their surrounding regions.
The Sunspot Cycle Observations of sunspots have shown that the sun rotates. The numbers and positions of sunspots vary in a cycle that lasts about 11 years. Sunspots initially appear in groups about midway between the sun s equator and poles. The # will peak at about 100 of more sunspots. After the peak, the number of sunspots begins to decrease until it reaches a minimum
Solar Ejections The solar-activity cycle is caused by the changing solar magnetic field. This cycle is characterized by increases and decreases in various types of solar activity, including solar ejections. Solar ejections are events in which the sun emits atomic particles.
` Solar ejections include prominences, solar flares, and coronal mass ejections. Prominences are huge arches of glowing gases that follow the curved lines of the magnetic force from a region of one magnetic force to a region of the opposite magnetic.
Solar Ejections: Solar Flares Solar flares are the most violent of all solar disturbances. Solar flares release the energy stored in the strong magnetic fields of sunspots
Solar Ejections: Coronal Mass Ejections Some of the particles from a solar flare escape into space, increasing the strength of the solar wind. Particles also escape as coronal mass ejections. The particles in the ejection can cause disturbances to Earth s magnetic field. These disturbances have been known to interfere with radio communications, satellites, and even cause blackouts
Auroras Auroras are the result of the interaction between the solar wind and Earth s magnetosphere. Auroras are usually seen close to Earth s magnetic poles because electrically charged particles are guided toward earth s magnetic poles by Earth s magnetosphere.
Auroras Depending on the pole there are near they are called different things. North Pole= aurora borealis or northern light. South Pole= aurora australis or southern lights. Auroras are most frequent just after peak sunspot cycles In the United States auroras are visible about 5 times per year, however in Alaska auroras can be seen almost every clear night. Astronauts can even see auroras in orbit.
Go to full-size image Go to full-size image Go to full-size image Go to full-size image
