Lecture102102 - FSU High Energy Physics
... travel outward from the Sun responsible for comet’s tail and for blowing away primary atmospheres of inner planets pushes interstellar dust out of the Solar System ...
... travel outward from the Sun responsible for comet’s tail and for blowing away primary atmospheres of inner planets pushes interstellar dust out of the Solar System ...
Physics of the Weird Solar Minimum: New observations of the Sun
... New observations of the Sun Dr. E.J. Zita The Evergreen St. College Olympia WA 98505 zita@evergreen.edu ...
... New observations of the Sun Dr. E.J. Zita The Evergreen St. College Olympia WA 98505 zita@evergreen.edu ...
powerpoint - High Energy Physics at Wayne State
... At very high temperatures, atoms like iron can have 9 to 13 electrons ejected - ionized. 9-times ionized iron is only produced at temperatures of 1.3 million K 13-times ionized iron means the temperature gets up to 2.3 million K! ...
... At very high temperatures, atoms like iron can have 9 to 13 electrons ejected - ionized. 9-times ionized iron is only produced at temperatures of 1.3 million K 13-times ionized iron means the temperature gets up to 2.3 million K! ...
Lecture notes 4: The Sun as a Star i
... limb. If the temperature gradient dt/dr falls with height in the photosphere we therefore expect the observed effect of limb darkening since high temperature gas emits more vigorously than low temperature gas. Should we expect that the color of the light is different at the limb and at sun center? Th ...
... limb. If the temperature gradient dt/dr falls with height in the photosphere we therefore expect the observed effect of limb darkening since high temperature gas emits more vigorously than low temperature gas. Should we expect that the color of the light is different at the limb and at sun center? Th ...
Formation of the solar system
... The result would be a protosun with a disk outside it - several possible mechanisms. This creates a tendency for particles to be drawn by gravity to the midplane. The disk is a turbulent region so that angular momentum can be easily transferred away from the protosun. In the disk, material starts to ...
... The result would be a protosun with a disk outside it - several possible mechanisms. This creates a tendency for particles to be drawn by gravity to the midplane. The disk is a turbulent region so that angular momentum can be easily transferred away from the protosun. In the disk, material starts to ...
hw4
... helium nucleus. Much more energy is released in fusion since some of the mass is converted directly into energy (E=mc2). A burning log relies on breaking chemical bonds for releasing energy. Describe how an aurora is produced and why we are more likely to see one from College Park during times of so ...
... helium nucleus. Much more energy is released in fusion since some of the mass is converted directly into energy (E=mc2). A burning log relies on breaking chemical bonds for releasing energy. Describe how an aurora is produced and why we are more likely to see one from College Park during times of so ...
A startling new Sun
... photosphere, at a temperature of about 6000 K; the warmer and rarer chromosphere at about 104 K; and the very much hotter corona at 2–5 MK that stretches to the Earth and beyond. In the photosphere you see sunspots, dark regions where strong magnetic flux tubes poke through the solar surface. The ph ...
... photosphere, at a temperature of about 6000 K; the warmer and rarer chromosphere at about 104 K; and the very much hotter corona at 2–5 MK that stretches to the Earth and beyond. In the photosphere you see sunspots, dark regions where strong magnetic flux tubes poke through the solar surface. The ph ...
*Students will be required to draw and label the solar system.
... explain how our solar system works? system showing the order of the planets.* We can make a model of the solar system using different balls of different sizes. Vocabulary: Word: solar system ...
... explain how our solar system works? system showing the order of the planets.* We can make a model of the solar system using different balls of different sizes. Vocabulary: Word: solar system ...
The Photosphere
... • Assuming a value of T0 , the temperature at the center of the disk (not at the center of the Sun!), one can then determine a series of values of T vs. τ and thus provide informaCon ab ...
... • Assuming a value of T0 , the temperature at the center of the disk (not at the center of the Sun!), one can then determine a series of values of T vs. τ and thus provide informaCon ab ...
Stars Take Center Stage in
... Toomre has been studying solar dynamism for more than a decade. A self-proclaimed “deep miner” of the sun, his focus has been the sun's internal, unseen structures rather than its outer regions. “It's not enough to know what comes out of the surface,” Toomre says. “We would like to understand how th ...
... Toomre has been studying solar dynamism for more than a decade. A self-proclaimed “deep miner” of the sun, his focus has been the sun's internal, unseen structures rather than its outer regions. “It's not enough to know what comes out of the surface,” Toomre says. “We would like to understand how th ...
ΗΛΙΟΣ: Το κοντινότερο αστέρι
... Photos from Skylab/SMM/Yohkoh seem to agree so well with this cartoon? Pictures some times may lead you to the wrong conclusions so be careful how far you push the connection of the visual impression with the energy release when you form cartoons ...
... Photos from Skylab/SMM/Yohkoh seem to agree so well with this cartoon? Pictures some times may lead you to the wrong conclusions so be careful how far you push the connection of the visual impression with the energy release when you form cartoons ...
june 2011 - Holt Planetarium
... high overall density implies that it's hiding a very large metallic core, an iron-rich cannonball that takes up three-fourths of its diameter and half its volume. So how did it get that way? The most likely among the major formation theories is the "big splat" scenario. That is, Mercury was initiall ...
... high overall density implies that it's hiding a very large metallic core, an iron-rich cannonball that takes up three-fourths of its diameter and half its volume. So how did it get that way? The most likely among the major formation theories is the "big splat" scenario. That is, Mercury was initiall ...
june 2011 - Holt Planetarium
... high overall density implies that it's hiding a very large metallic core, an iron-rich cannonball that takes up three-fourths of its diameter and half its volume. So how did it get that way? The most likely among the major formation theories is the "big splat" scenario. That is, Mercury was initiall ...
... high overall density implies that it's hiding a very large metallic core, an iron-rich cannonball that takes up three-fourths of its diameter and half its volume. So how did it get that way? The most likely among the major formation theories is the "big splat" scenario. That is, Mercury was initiall ...
Photosphere - Solar Physics and Space Weather
... • Corona is made of very high-temperature gases at extremely low density • It extends to several million Km • Because of hot temperature, it expands into the outer space forming solar wind ...
... • Corona is made of very high-temperature gases at extremely low density • It extends to several million Km • Because of hot temperature, it expands into the outer space forming solar wind ...
aas_gdemessieres - Astronomy at Swarthmore College
... Our results: Lines in t Sco are not as narrow as those in coronal sources, but they are only slightly broadened. Typical velocities are 200 km s-1, while the observed wind terminal velocity for t Sco is at least 1500 km s-1. Furthermore, the lines are slightly redshifted (mean value ~50 km s-1 for ~ ...
... Our results: Lines in t Sco are not as narrow as those in coronal sources, but they are only slightly broadened. Typical velocities are 200 km s-1, while the observed wind terminal velocity for t Sco is at least 1500 km s-1. Furthermore, the lines are slightly redshifted (mean value ~50 km s-1 for ~ ...
Measuring the Magnetic Free Energy Available for Solar Activity
... each observation was averaged. The dotted line shows the energy of the equivalent potential field and the dashed line shows the equivalent open field energy. ...
... each observation was averaged. The dotted line shows the energy of the equivalent potential field and the dashed line shows the equivalent open field energy. ...
The Sun, Stars, and Beyond
... for “normal” convective fluid flow, which brings the heat to the surface, or photosphere. ...
... for “normal” convective fluid flow, which brings the heat to the surface, or photosphere. ...
Does the Sun rotate?
... Sunspots – temporary features / areas of concentrated intense magnetic fields. Prominences – magnetic loops above sunspots, can carry plasma (hot ionized ...
... Sunspots – temporary features / areas of concentrated intense magnetic fields. Prominences – magnetic loops above sunspots, can carry plasma (hot ionized ...
photosphere
... line emission of ionized Calcium indicate magnetic activity also on other stars. ...
... line emission of ionized Calcium indicate magnetic activity also on other stars. ...
Stellar Activity
... evidence for spot modulation or spot cycles • Sometimes spots are present, sometimes not • Variable light levels – long period, low amplitude modulation? (mostly in dM’s with M>0.5MSun) • Spots may come and go on short time scales or be distributed evenly around the star • Large isolated spots are N ...
... evidence for spot modulation or spot cycles • Sometimes spots are present, sometimes not • Variable light levels – long period, low amplitude modulation? (mostly in dM’s with M>0.5MSun) • Spots may come and go on short time scales or be distributed evenly around the star • Large isolated spots are N ...
File - Earth Science with Mr. Lanik
... surface is a region of hot plasma called the corona. The corona is about 2 million K (3.6 million degrees F), much hotter than the visible surface, and it is even hotter in a flare. Why the atmosphere gets so hot has been a mystery for decades; SOHO's observations are helping to solve this mystery. ...
... surface is a region of hot plasma called the corona. The corona is about 2 million K (3.6 million degrees F), much hotter than the visible surface, and it is even hotter in a flare. Why the atmosphere gets so hot has been a mystery for decades; SOHO's observations are helping to solve this mystery. ...
The Inner Solar System
... • The gases are thin at this layer • The chromosphere and corona can only be seen during solar eclipses. ...
... • The gases are thin at this layer • The chromosphere and corona can only be seen during solar eclipses. ...
Section 27.1
... called the photosphere, which means “sphere of light.” Just above it is the chromosphere. This is a very hot layer of plasma, a highenergy state of matter. ...
... called the photosphere, which means “sphere of light.” Just above it is the chromosphere. This is a very hot layer of plasma, a highenergy state of matter. ...
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.