PG_Lecture_Dec18_2008
... Atmospheres of “active” stars and the Sun Flare stars and the Sun have hot atmospheres, usually a corona (temperature ~ 106 K) plus a chromosphere (~10,000 K) and “transition region” (~105 K). These temperatures are generally much hotter than their surface temperatures. E.g. The Sun has surface (ph ...
... Atmospheres of “active” stars and the Sun Flare stars and the Sun have hot atmospheres, usually a corona (temperature ~ 106 K) plus a chromosphere (~10,000 K) and “transition region” (~105 K). These temperatures are generally much hotter than their surface temperatures. E.g. The Sun has surface (ph ...
Solar System Power Point
... • How energy is produced in the center of stars • Takes millions of years for energy to reach the sun’s surface. • It takes 8.3 minutes for sunlight to reach the Earth ...
... • How energy is produced in the center of stars • Takes millions of years for energy to reach the sun’s surface. • It takes 8.3 minutes for sunlight to reach the Earth ...
powerpoint version
... The Solar Atmosphere Photosphere: visible “surface” of the Sun, about 500 km thick. Moving outwards temperature falls from 8000 K to 4500 K and density of gas rapidly decreases. Granulation of surface indicates large scale movement of gas - convection currents transfer heat. Chromosphere: outside ph ...
... The Solar Atmosphere Photosphere: visible “surface” of the Sun, about 500 km thick. Moving outwards temperature falls from 8000 K to 4500 K and density of gas rapidly decreases. Granulation of surface indicates large scale movement of gas - convection currents transfer heat. Chromosphere: outside ph ...
The Sun and the Origin of the Solar System
... • surface areas that are darker than surroundings (lower temperatures) • regions of intense magnetic activity ...
... • surface areas that are darker than surroundings (lower temperatures) • regions of intense magnetic activity ...
$doc.title
... We can probe the solar interior using the Sun’s own vibrations • Helioseismology is the study of how the Sun ...
... We can probe the solar interior using the Sun’s own vibrations • Helioseismology is the study of how the Sun ...
Stars, Galaxies, and the Universe
... Corona: Outer layer, extends several million kilometers (p. 757) ...
... Corona: Outer layer, extends several million kilometers (p. 757) ...
Part 1
... Quic kTime™ and a TIFF (Uncompress ed) dec ompres sor are needed to s ee this pic ture. ...
... Quic kTime™ and a TIFF (Uncompress ed) dec ompres sor are needed to s ee this pic ture. ...
The Sun: A Medium-sized Star
... The energy moves outward into the convective zone, where cool matter sinks and hot matter rises. Photosphere: Suns surface where energy escapes as light. Atmosphere: is divided into the chromosphere and the corona. Chromosphere: inner atmosphere, very hot—about 60 000 ºC hotter than the phot ...
... The energy moves outward into the convective zone, where cool matter sinks and hot matter rises. Photosphere: Suns surface where energy escapes as light. Atmosphere: is divided into the chromosphere and the corona. Chromosphere: inner atmosphere, very hot—about 60 000 ºC hotter than the phot ...
Intro to Space
... • You will be divided into a group of 4 or 5 • You will need to take your information from the website and design our solar system on paper • Be creative! Make sure you use the facts in some way from the website and incorporate it into your design • INCLUDE all the parts of the solar system • You wi ...
... • You will be divided into a group of 4 or 5 • You will need to take your information from the website and design our solar system on paper • Be creative! Make sure you use the facts in some way from the website and incorporate it into your design • INCLUDE all the parts of the solar system • You wi ...
Student notes for first part of topic
... The universe began about 14 billion years ago At the beginning there was nothing more than a singularity -The singularity had no space but contained all the energy the universe would ever contain - The energy was in the form of gamma rays -The singularity expanded and continued to expand -The fi ...
... The universe began about 14 billion years ago At the beginning there was nothing more than a singularity -The singularity had no space but contained all the energy the universe would ever contain - The energy was in the form of gamma rays -The singularity expanded and continued to expand -The fi ...
VII. Uranus - Napa Valley College
... 15 minutes to a half an hour. — Size: a few hundred km across. — We see them because the hot interior is brighter than the cool borders. — Convection cells in the photosphere (Aside — Modes of heat transport 1. Conduction: heat transport through solids. (Not important in stars) 2. Convection — hot m ...
... 15 minutes to a half an hour. — Size: a few hundred km across. — We see them because the hot interior is brighter than the cool borders. — Convection cells in the photosphere (Aside — Modes of heat transport 1. Conduction: heat transport through solids. (Not important in stars) 2. Convection — hot m ...
VOC 3J-2
... 15. Energy is produced in the center, or ______________________, of the sun. 16. Energy passes from the sun’s core through a dense region called the______________________. 17. Hot gases are carried to the sun’s visible surface from a region called the______________________. 18. Energy leaves the sun ...
... 15. Energy is produced in the center, or ______________________, of the sun. 16. Energy passes from the sun’s core through a dense region called the______________________. 17. Hot gases are carried to the sun’s visible surface from a region called the______________________. 18. Energy leaves the sun ...
Document
... 11. One AU is 149,500,000 kM. It is the distance between the Earth and the Sun. How many AUs is Mars, if it is 207,000,000 kM from the Sun? If ...
... 11. One AU is 149,500,000 kM. It is the distance between the Earth and the Sun. How many AUs is Mars, if it is 207,000,000 kM from the Sun? If ...
Video Universe Secrets of the Sun
... If the Sun were made of wood and burned, how long would it take to burn out? What is the process by which the Sun produces energy (heat/light)? What are the particles called that bring heat and light from the center of the Sun to Earth? How long does it take light that leaves the Sun to reach Earth? ...
... If the Sun were made of wood and burned, how long would it take to burn out? What is the process by which the Sun produces energy (heat/light)? What are the particles called that bring heat and light from the center of the Sun to Earth? How long does it take light that leaves the Sun to reach Earth? ...
Preface
... of the physical interactions that govern the interaction of an incoming plasma (mainly the solar wind, but in some cases a magnetospheric plasma) with solar system objects. The Alfvén conference emphasized comparisons of phenomena from different, but similar, planets and moons, in order to increase ...
... of the physical interactions that govern the interaction of an incoming plasma (mainly the solar wind, but in some cases a magnetospheric plasma) with solar system objects. The Alfvén conference emphasized comparisons of phenomena from different, but similar, planets and moons, in order to increase ...
Astro-Spectroscpy
... Though the surface temperature of the Sun is 5,770 degrees Kelvin, the Sun is surrounded by very hot gas in the solar corona at more than a million degrees. Solar flares and coronal mass ejections (CMEs) frequently erupt from the Sun emitting intense radiation and charged particles. ...
... Though the surface temperature of the Sun is 5,770 degrees Kelvin, the Sun is surrounded by very hot gas in the solar corona at more than a million degrees. Solar flares and coronal mass ejections (CMEs) frequently erupt from the Sun emitting intense radiation and charged particles. ...
superflares on Sun-like stars
... Many stars show flares similar to solar flares, and often such stellar flares are much more energetic than solar flares. The total energy of a solar flare is typically 1029 –1032 erg. There are much more energetic flares (1033 –1038 erg) in stars, especially in young stars with rapid rotation. These ...
... Many stars show flares similar to solar flares, and often such stellar flares are much more energetic than solar flares. The total energy of a solar flare is typically 1029 –1032 erg. There are much more energetic flares (1033 –1038 erg) in stars, especially in young stars with rapid rotation. These ...
Ch. 26 The Sun and the Solar System
... areas than the surrounding photosphere. Very strong magnetic fields (1000 times stronger than that of the surrounding photosphere) Move from left to right across the Sun’s surface (first indication that the Sun rotates on an axis much like Earth) Sunspot activity cycles on an average of 11 yrs betwe ...
... areas than the surrounding photosphere. Very strong magnetic fields (1000 times stronger than that of the surrounding photosphere) Move from left to right across the Sun’s surface (first indication that the Sun rotates on an axis much like Earth) Sunspot activity cycles on an average of 11 yrs betwe ...
Coronal Mass Ejections, Flares, and the Solar Wind
... Coronal Mass Ejections, Flares, and the Solar Wind Some of the most dramatic space weather effects occur in association with eruptions of material from the solar atmosphere into interplanetary space. These eruptions are known as coronal mass ejections, or CMEs. A large CME can contain 10.0E16 grams ...
... Coronal Mass Ejections, Flares, and the Solar Wind Some of the most dramatic space weather effects occur in association with eruptions of material from the solar atmosphere into interplanetary space. These eruptions are known as coronal mass ejections, or CMEs. A large CME can contain 10.0E16 grams ...
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.