Section 14.7: The Sun
... • Scientists estimate the sun will continue to produce energy for another 5 billion years before it runs out of fuel. ...
... • Scientists estimate the sun will continue to produce energy for another 5 billion years before it runs out of fuel. ...
The Sun
... • The Active Sun: The Sun’s surface features vary in an 11year cycle. This is related to a 22-year cycle in which the surface magnetic field increases, decreases, and then increases again with the opposite polarity. • Sunspots are relatively cool regions produced by local concentrations of the Sun’s ...
... • The Active Sun: The Sun’s surface features vary in an 11year cycle. This is related to a 22-year cycle in which the surface magnetic field increases, decreases, and then increases again with the opposite polarity. • Sunspots are relatively cool regions produced by local concentrations of the Sun’s ...
The sun
... Most of the material in the nebula was pulled into the center and formed the sun. According to the theory the pressure in the center became great enough to make the nuclear reactions that powered the sun. Eventually the solar eruptions occurred casing a solar wind. In the center of the solar system ...
... Most of the material in the nebula was pulled into the center and formed the sun. According to the theory the pressure in the center became great enough to make the nuclear reactions that powered the sun. Eventually the solar eruptions occurred casing a solar wind. In the center of the solar system ...
Unit A, “Processes of Living Things”
... The sun is a huge ball of gases, mostly _______hydrogen________ and ________helium_______. The sun releases energy as … Light and heat What is fusion? When hydrogen particle fuse, or join together, to produce helium Give three examples of waves (the energy from the sun): 1. Infrared waves (heat) ...
... The sun is a huge ball of gases, mostly _______hydrogen________ and ________helium_______. The sun releases energy as … Light and heat What is fusion? When hydrogen particle fuse, or join together, to produce helium Give three examples of waves (the energy from the sun): 1. Infrared waves (heat) ...
The Planets and the Sun
... • The sun is a burning sphere made up of several layers of gases. The layer we see is the photoshere ______. This layer is blanketed by the sun’s corona atmosphere, or _____. It is the only part we can see during a solar eclipse. Dark areas on the sunspots These dark surface of the sun are ______. S ...
... • The sun is a burning sphere made up of several layers of gases. The layer we see is the photoshere ______. This layer is blanketed by the sun’s corona atmosphere, or _____. It is the only part we can see during a solar eclipse. Dark areas on the sunspots These dark surface of the sun are ______. S ...
The sun - Salwan Education Trust
... million! That is a huge number as you can see, and the lines of force (magnetic energy) which emanate from these poles intersect and loop each other continuously. These conflicting lines of force can cause some very interesting phenomena. For example, this may lead to a change in the shape of the pl ...
... million! That is a huge number as you can see, and the lines of force (magnetic energy) which emanate from these poles intersect and loop each other continuously. These conflicting lines of force can cause some very interesting phenomena. For example, this may lead to a change in the shape of the pl ...
Science 3 - Segment 1 Review
... 10. Name and describe the three types of galaxies. Which one do we fit into? (2.02) ...
... 10. Name and describe the three types of galaxies. Which one do we fit into? (2.02) ...
Chapter 26 – The Sun and the Solar System
... a. Some are barely visible while others are 4 times larger than Earth b. Small one may last a few hour – large ones months c. Are very hot and bright – look dark because the photosphere is so much hotter and brighter than the sunspots d. Move from left to right across surface i This gave evidence th ...
... a. Some are barely visible while others are 4 times larger than Earth b. Small one may last a few hour – large ones months c. Are very hot and bright – look dark because the photosphere is so much hotter and brighter than the sunspots d. Move from left to right across surface i This gave evidence th ...
hotstar_xrays
... models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing downward. Note that as the wind attenuation increases less and less of the ...
... models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing downward. Note that as the wind attenuation increases less and less of the ...
Powerpoint
... ✴sun’s magnetic field gets tangled up and flips every 11 or so years ✴magnetic field sticks out of surface (in prominences) and causes prominences and cooler places called sunspots ...
... ✴sun’s magnetic field gets tangled up and flips every 11 or so years ✴magnetic field sticks out of surface (in prominences) and causes prominences and cooler places called sunspots ...
The Sun
... 4 1H → 4He + energy 4 protons have 0.048*10-27 kg (= 0.7 %) more mass than 4He. Energy gain = Dm*c2 = 0.43*10-11 J per reaction. Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity. ...
... 4 1H → 4He + energy 4 protons have 0.048*10-27 kg (= 0.7 %) more mass than 4He. Energy gain = Dm*c2 = 0.43*10-11 J per reaction. Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity. ...
Invisible sunspots uncovered
... Sunspots appear as dark patches on the Sun's photosphere. They were first observed by Chinese astronomers and later extensively studied by Galileo with the aid of a telescope. Their temperature is of approximately 4,000 degrees, lower than that of the surrounding photosphere (6,000 degrees). The bir ...
... Sunspots appear as dark patches on the Sun's photosphere. They were first observed by Chinese astronomers and later extensively studied by Galileo with the aid of a telescope. Their temperature is of approximately 4,000 degrees, lower than that of the surrounding photosphere (6,000 degrees). The bir ...
The Sun and the Stars
... • What is the single most distinguishing feature of a star? • Luminosity is a term that astronomers use when describing the total amount of energy it radiated by the star ( the twinkle) • It can be measured more precisely as a star’s total energy output per second, measured in Joules per second (J/s ...
... • What is the single most distinguishing feature of a star? • Luminosity is a term that astronomers use when describing the total amount of energy it radiated by the star ( the twinkle) • It can be measured more precisely as a star’s total energy output per second, measured in Joules per second (J/s ...
Space Physics Handout 2 : The Earth`s magnetosphere and
... atmosphere. At altitudes above 80km collisions in the atmosphere are too infrequent to result in rapid recombination and a permanent ionised population results, known as the ionosphere. Typical values of electron density in the mid-latitude ionosphere are ~ 105 cm-3 and typical temperatures ~ 103 K, ...
... atmosphere. At altitudes above 80km collisions in the atmosphere are too infrequent to result in rapid recombination and a permanent ionised population results, known as the ionosphere. Typical values of electron density in the mid-latitude ionosphere are ~ 105 cm-3 and typical temperatures ~ 103 K, ...
Unit 1
... Solar activity reflected by the number of sunspots is believed to influence the climate on Earth as ...
... Solar activity reflected by the number of sunspots is believed to influence the climate on Earth as ...
APS Centenary Poster - Bartol Research Institute
... Images made by orbiting X-ray telescopes show the solar corona has a high degree of spatial structure, organized by magnetic fields. Within closed field coronal loops, these effectively hold back the coronal expansion. But along radially oriented, open-field regions the wind flows rapidly outward, ...
... Images made by orbiting X-ray telescopes show the solar corona has a high degree of spatial structure, organized by magnetic fields. Within closed field coronal loops, these effectively hold back the coronal expansion. But along radially oriented, open-field regions the wind flows rapidly outward, ...
how the Sun impacts the Earth
... How do we account for one of the most basic properties of the solar system; the difference between the Terrestrial and Jovian planets? We think this is a consequence of different temperatures in different parts of the solar nebula “the solar nebula was heated by release of gravitational energy…it w ...
... How do we account for one of the most basic properties of the solar system; the difference between the Terrestrial and Jovian planets? We think this is a consequence of different temperatures in different parts of the solar nebula “the solar nebula was heated by release of gravitational energy…it w ...
Grade 9 Science – Unit 4
... RADIATIVE ZONE – Area of moving gases where temperature and pressure increases CHROMOSPHERE – The inner atmosphere of the Sun PHOTOSPHERE – The “surface’ of the Sun. It is NOT solid; rather, it is an area of churning gases. Average temperature is 5 500OC CORONA – The hot outer part of the Su ...
... RADIATIVE ZONE – Area of moving gases where temperature and pressure increases CHROMOSPHERE – The inner atmosphere of the Sun PHOTOSPHERE – The “surface’ of the Sun. It is NOT solid; rather, it is an area of churning gases. Average temperature is 5 500OC CORONA – The hot outer part of the Su ...
Astronomy
... 23. What process creates the light emitted by stars? 24. Stars spend most of their lives in this stage: 25. A visual representation of the temperature and luminosity of stars is called: 26. Relatively dark spots on the sun that contains intense magnetic fields are known as: 27. These reactions join ...
... 23. What process creates the light emitted by stars? 24. Stars spend most of their lives in this stage: 25. A visual representation of the temperature and luminosity of stars is called: 26. Relatively dark spots on the sun that contains intense magnetic fields are known as: 27. These reactions join ...
Scientific Method
... from which most of the visible light escapes into space (5800 K) • Sunspots: A region of the solar photosphere that is cooler than its surroundings & therefore appears dark (~4800 K) • Sunspots can be used to determine the sun’s rotation period ~ 24-27 days • Sunspots were discovered by Galileo ...
... from which most of the visible light escapes into space (5800 K) • Sunspots: A region of the solar photosphere that is cooler than its surroundings & therefore appears dark (~4800 K) • Sunspots can be used to determine the sun’s rotation period ~ 24-27 days • Sunspots were discovered by Galileo ...
Corona
A corona (Latin, 'crown') is an aura of plasma that surrounds the sun and other celestial bodies. The Sun's corona extends millions of kilometres into space and is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The word ""corona"" is a Latin word meaning ""crown"", from the Ancient Greek κορώνη (korōnē, “garland, wreath”).The high temperature of the Sun's corona gives it unusual spectral features, which led some in the 19th century to suggest that it contained a previously unknown element, ""coronium"". Instead, these spectral features have since been explained by highly ionized iron (Fe-XIV). Bengt Edlén, following the work of Grotrian (1939), first identified the coronal lines in 1940 (observed since 1869) as transitions from low-lying metastable levels of the ground configuration of highly ionised metals (the green Fe-XIV line at 5303 Å, but also the red line Fe-X at 6374 Å). These high stages of ionisation indicate a plasma temperature in excess of 1,000,000 kelvin, much hotter than the surface of the sun.Light from the corona comes from three primary sources, which are called by different names although all of them share the same volume of space. The K-corona (K for kontinuierlich, ""continuous"" in German) is created by sunlight scattering off free electrons; Doppler broadening of the reflected photospheric absorption lines completely obscures them, giving the spectral appearance of a continuum with no absorption lines. The F-corona (F for Fraunhofer) is created by sunlight bouncing off dust particles, and is observable because its light contains the Fraunhofer absorption lines that are seen in raw sunlight; the F-corona extends to very high elongation angles from the Sun, where it is called the zodiacal light. The E-corona (E for emission) is due to spectral emission lines produced by ions that are present in the coronal plasma; it may be observed in broad or forbidden or hot spectral emission lines and is the main source of information about the corona's composition.