The Sun: a star in the Solar System (Part 2)
... heating the solar corona almost certainly involve the solar magnetic field ...
... heating the solar corona almost certainly involve the solar magnetic field ...
Understanding the Sun
... Understanding the Sun Our life here on Earth is entirely dependent on the Sun. But although we have been observing the Sun’s passage across the sky for millennia, there are many things about it we still don’t understand. Amongst the hundreds of billions of stars that make up the Milky Way Galaxy, th ...
... Understanding the Sun Our life here on Earth is entirely dependent on the Sun. But although we have been observing the Sun’s passage across the sky for millennia, there are many things about it we still don’t understand. Amongst the hundreds of billions of stars that make up the Milky Way Galaxy, th ...
Document
... Earth. It is made up of very hot gases with the center of the Sun measuring about 15 million °C!!! ...
... Earth. It is made up of very hot gases with the center of the Sun measuring about 15 million °C!!! ...
THE SUN - Van Buren Public Schools
... • Nuclear fusion is the way that the sun produces energy. This reaction converts four hydrogen nuclei into the nucleus of a helium atom, releasing a tremendous amount of energy. • During nuclear fusion, energy is released because some matter is actually converted to energy. • It is thought that a st ...
... • Nuclear fusion is the way that the sun produces energy. This reaction converts four hydrogen nuclei into the nucleus of a helium atom, releasing a tremendous amount of energy. • During nuclear fusion, energy is released because some matter is actually converted to energy. • It is thought that a st ...
ASTRONOMY TEST THE SUN
... 1._____ The chromosphere is faint because of its low density. 2._____ The sun’s mass is over a million times that of our earth 3._____ The sun is a fairly normal star 4._____ The energy of the sun is transported to its surface by convection 5._____ The “solar constant” refers to the observation that ...
... 1._____ The chromosphere is faint because of its low density. 2._____ The sun’s mass is over a million times that of our earth 3._____ The sun is a fairly normal star 4._____ The energy of the sun is transported to its surface by convection 5._____ The “solar constant” refers to the observation that ...
Sunspots - Sage Middle School
... Sunspots •dark cooler (4000K vs. 5800K) regions on the sun •last several days to several weeks •caused by the sun’s magnetic field upwelling to the photosphere •occur in cycles •contribute to solar storms such as flares and coronal mass ejections ...
... Sunspots •dark cooler (4000K vs. 5800K) regions on the sun •last several days to several weeks •caused by the sun’s magnetic field upwelling to the photosphere •occur in cycles •contribute to solar storms such as flares and coronal mass ejections ...
The Sun
... below. So the material sits on the surface and cools off as it radiates to the sky. • Charged particles in a magnetic field feel a force sideways to their motion, binding the gas to the field. • Sunspots are like “magnetic scabs” of gas unable to be recirculated to lower, hotter levels. They are bou ...
... below. So the material sits on the surface and cools off as it radiates to the sky. • Charged particles in a magnetic field feel a force sideways to their motion, binding the gas to the field. • Sunspots are like “magnetic scabs” of gas unable to be recirculated to lower, hotter levels. They are bou ...
a naturally occuring object in space such as a star, planet, moon
... corona - the outermost layer of the Sun. It stretches far into space, appears very thin and faint and can only be seen from Earth during a total solar eclipse. ...
... corona - the outermost layer of the Sun. It stretches far into space, appears very thin and faint and can only be seen from Earth during a total solar eclipse. ...
PHY2083 ASTRONOMY
... wavelengths, causing dark lines. Darkest part of line from regions higher up in the photosphere where the gas is cooler. ...
... wavelengths, causing dark lines. Darkest part of line from regions higher up in the photosphere where the gas is cooler. ...
Like a boiling teakettle atop a COLD stove, the sun`s HOT outer
... themselves to neutralize it. And if a plasma cannot sustain an electric field, it cannot move relative to the magnetic field (or vice versa), because to do so would induce an electric field. This is why astronomers talk about magnetic fields being “frozen” into plasmas. This principle can be quantif ...
... themselves to neutralize it. And if a plasma cannot sustain an electric field, it cannot move relative to the magnetic field (or vice versa), because to do so would induce an electric field. This is why astronomers talk about magnetic fields being “frozen” into plasmas. This principle can be quantif ...
Lecture 12
... B. By observing Doppler shifts of spectral line emitted by solar surface moving up and down C. By seeing how solar prominences wiggle D. By using the Zeeman effect E. By its effect on 1111-year solar activity cycle ...
... B. By observing Doppler shifts of spectral line emitted by solar surface moving up and down C. By seeing how solar prominences wiggle D. By using the Zeeman effect E. By its effect on 1111-year solar activity cycle ...
Structure of the Sun, our nearest star
... o High-speed charged particles (mostly electrons and protons) constantly blowing off the Sun. o May be viewed as an extension of the outer atmosphere of the Sun (the corona) into interplanetary space. ...
... o High-speed charged particles (mostly electrons and protons) constantly blowing off the Sun. o May be viewed as an extension of the outer atmosphere of the Sun (the corona) into interplanetary space. ...
Solar-B - to Nobeyama Radio Observatory
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
Sun note sheet - Lauer Science
... emits only certain wavelengths of light, resulting in a ________________ appearance. We call this the sphere of color, or ___________________. The solar chromosphere is characterized by jets of gas extending upward called ________________. THE SOLAR CORONA – source of the Solar Wind Seen in visibl ...
... emits only certain wavelengths of light, resulting in a ________________ appearance. We call this the sphere of color, or ___________________. The solar chromosphere is characterized by jets of gas extending upward called ________________. THE SOLAR CORONA – source of the Solar Wind Seen in visibl ...
15 September: Basic properties of the Sun
... • Described the Sun’s size (diameter), mass, chemical composition, and temperature • Today, additional features as preparation for solar observing lab ...
... • Described the Sun’s size (diameter), mass, chemical composition, and temperature • Today, additional features as preparation for solar observing lab ...
The Sun – “Our” Star
... The solar luminosity, defined as the amount of energy generated within the Sun every second, is constant. The Sun emits radiation like a blackbody with a surface temperature ~ 5800 K. Astronomers have developed a “standard model” to explain the Sun's interior structure and energy generation processe ...
... The solar luminosity, defined as the amount of energy generated within the Sun every second, is constant. The Sun emits radiation like a blackbody with a surface temperature ~ 5800 K. Astronomers have developed a “standard model” to explain the Sun's interior structure and energy generation processe ...
Midterm 3 Review Sessions Two choices:
... We can write equations expressing the following ideas: • The Sun is a gas. • The Sun is neither contracting nor expanding. • Each point inside the Sun stays at a fixed temperature. • How energy generation rate depends on density, temperature, composition. • How energy is carried outwards. For every ...
... We can write equations expressing the following ideas: • The Sun is a gas. • The Sun is neither contracting nor expanding. • Each point inside the Sun stays at a fixed temperature. • How energy generation rate depends on density, temperature, composition. • How energy is carried outwards. For every ...
Chapter 24 - Cloudfront.net
... Nuclear Fusion – The process by which the sun produces energy; this nuclear reaction converts four hydrogen nuclei into the nucleus of a helium atom and tremendous energy is released It is believed that a star our size can exist in its stable ...
... Nuclear Fusion – The process by which the sun produces energy; this nuclear reaction converts four hydrogen nuclei into the nucleus of a helium atom and tremendous energy is released It is believed that a star our size can exist in its stable ...
Chapter 29.2 notes with lines
... This cycle is characterized by increases and decreases in various types of solar activity, including solar eruptions. ...
... This cycle is characterized by increases and decreases in various types of solar activity, including solar eruptions. ...
Section 24.3 The Sun
... Solar wind is a stream of protons and electrons ejected at high speed from the solar corona. The Active Sun Sunspots A sunspot is a dark spot on the sun that is cool in contrast to the surrounding photosphere. Sunspots appear dark because of their temperature, which is about 1500 K less than t ...
... Solar wind is a stream of protons and electrons ejected at high speed from the solar corona. The Active Sun Sunspots A sunspot is a dark spot on the sun that is cool in contrast to the surrounding photosphere. Sunspots appear dark because of their temperature, which is about 1500 K less than t ...
PPT
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
The Sun Notes File
... to separate to nuclei and electrons Nuclei are positive so push away But high temp and pressure push them ...
... to separate to nuclei and electrons Nuclei are positive so push away But high temp and pressure push them ...
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.