Sun - International Year of Astronomy 2009
... During this time we see the Sun going from a calm star, to a very turbulent active star, and switching the polarity of the ...
... During this time we see the Sun going from a calm star, to a very turbulent active star, and switching the polarity of the ...
Presentation for perspective graduate students 2006
... •Hydrogen burning occurs only deep in the interior of the Sun (and other stars) because this is the only place where •A) There is sufficient hydrogen •B) The density is sufficiently low for the high temperature atoms to build up enough energy to collide and undergo fusion •C) The temperature is low ...
... •Hydrogen burning occurs only deep in the interior of the Sun (and other stars) because this is the only place where •A) There is sufficient hydrogen •B) The density is sufficiently low for the high temperature atoms to build up enough energy to collide and undergo fusion •C) The temperature is low ...
PHYS 2410 General Astronomy Homework 5
... collisional broadening is observed in spectral lines. ...
... collisional broadening is observed in spectral lines. ...
Solar flare
... names. Sometimes these phenomena are observed in isolation, but more often, in particular for the largest events, all or many of them are associated with each other. Flares occur near ...
... names. Sometimes these phenomena are observed in isolation, but more often, in particular for the largest events, all or many of them are associated with each other. Flares occur near ...
ph507lecnote06
... sunspot cycle. At these times, the corona is much less regular and much more extended than at sunspot minimum. Astronomers believe that coronal heating is caused by surface activity on the Sun. The changing shape and size of the corona are the direct result of variations in prominence and flare acti ...
... sunspot cycle. At these times, the corona is much less regular and much more extended than at sunspot minimum. Astronomers believe that coronal heating is caused by surface activity on the Sun. The changing shape and size of the corona are the direct result of variations in prominence and flare acti ...
The Sun: the Solar Atmosphere, Nuclear Fusion
... • The Sun is a star, a fairly common and typical star • Its spectral type is G2, which means Teff~5800 K • A star is a ball of gas held in equilibrium against its own self-gravity by the thermal pressure and outflow of energy from center to the surface • The Sun radiates away a lot of energy. Every ...
... • The Sun is a star, a fairly common and typical star • Its spectral type is G2, which means Teff~5800 K • A star is a ball of gas held in equilibrium against its own self-gravity by the thermal pressure and outflow of energy from center to the surface • The Sun radiates away a lot of energy. Every ...
The Small Objects. The Sun.
... They collide with other charged particles and change their direction (random walk). They also decrease their energy while walking. It takes ~10 million year to get outside. The random bouncing occurs in the radiation zone (from the core to ~70% of the Sun’s radius). At T<2 million K, the convection ...
... They collide with other charged particles and change their direction (random walk). They also decrease their energy while walking. It takes ~10 million year to get outside. The random bouncing occurs in the radiation zone (from the core to ~70% of the Sun’s radius). At T<2 million K, the convection ...
Understanding Our Home Star FDP: Full Disk Patrol Telescope ISS
... Full-disk digital images of the Sun in select wavelengths as rapidly as every 10 seconds. Earlier NSO instruments typically delivered one image per day on film in a limited number of wavelengths. Significance: Much of the solar activity that affects us is visible in two lower layers of the solar atm ...
... Full-disk digital images of the Sun in select wavelengths as rapidly as every 10 seconds. Earlier NSO instruments typically delivered one image per day on film in a limited number of wavelengths. Significance: Much of the solar activity that affects us is visible in two lower layers of the solar atm ...
Document
... Areas around sunspots are active; large eruptions may occur in photosphere Solar prominence is large sheet of ejected gas: ...
... Areas around sunspots are active; large eruptions may occur in photosphere Solar prominence is large sheet of ejected gas: ...
The sun - E
... heat. By passing the white light through a prism, we see a rainbow. We call this rainbow a ‘spectrum’ and the colours in a spectrum always follow the same order of red, orange, yellow, green, blue, indigo and violet. The sun has an interior and an atmosphere. It does not have a solid surface. The su ...
... heat. By passing the white light through a prism, we see a rainbow. We call this rainbow a ‘spectrum’ and the colours in a spectrum always follow the same order of red, orange, yellow, green, blue, indigo and violet. The sun has an interior and an atmosphere. It does not have a solid surface. The su ...
How stars form slide show File
... drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotter as it becomes smaller. •Eventually the protostar becomes hot enough for nuclear fu ...
... drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotter as it becomes smaller. •Eventually the protostar becomes hot enough for nuclear fu ...
File - YEAR 11 EBSS PHYSICS DETAILED STUDIES
... Astrophysicists use computers to model the conditions within the sun. In doing so, they have been able come up with ‘facts’ about our sun. (These facts are all theoretical as it is impossible to test them) These facts include: Fusion occurs within 0.25R where temperatures reach above 10 million d ...
... Astrophysicists use computers to model the conditions within the sun. In doing so, they have been able come up with ‘facts’ about our sun. (These facts are all theoretical as it is impossible to test them) These facts include: Fusion occurs within 0.25R where temperatures reach above 10 million d ...
The Sun : Our Closest Star
... C. Surface Features of the Sun 1. Solar Flares = violent gas eruptions a. They cause damage to satellites, b. interfere with radio & T.V., c. and cause Aurora Borealis ( the Northern Lights). The Norse myth of the Valkaries Is connected to this. a. Gov. Web ...
... C. Surface Features of the Sun 1. Solar Flares = violent gas eruptions a. They cause damage to satellites, b. interfere with radio & T.V., c. and cause Aurora Borealis ( the Northern Lights). The Norse myth of the Valkaries Is connected to this. a. Gov. Web ...
The Sun: Our nearest star
... • Although biological organisms are pretty well protected from the solar wind, solar storms can have serious consequences. (1) The Earth’s atmosphere expands -Certain types of communications are disrupted -Satellites can be dragged out of orbit (2) Large currents can get induced in power grids (3) T ...
... • Although biological organisms are pretty well protected from the solar wind, solar storms can have serious consequences. (1) The Earth’s atmosphere expands -Certain types of communications are disrupted -Satellites can be dragged out of orbit (2) Large currents can get induced in power grids (3) T ...
Chapter 29 Notes-
... • Explain how sunspots are related to powerful magnetic fields on the sun. • Compare prominences, solar flares, and coronal mass ejections. • Describe how the solar wind can cause auroras on Earth. Sunspots-a dark area of the photosphere of the sun that is cooler than the surrounding areas and that ...
... • Explain how sunspots are related to powerful magnetic fields on the sun. • Compare prominences, solar flares, and coronal mass ejections. • Describe how the solar wind can cause auroras on Earth. Sunspots-a dark area of the photosphere of the sun that is cooler than the surrounding areas and that ...
Chapter 08
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
The Milky Way
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
The Sun
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
... photosphere (T ≈ 4240 K). Only appear dark against the bright sun. Would still be brighter than the full moon when placed on the night sky! ...
SOLAR PHYSICS
... Since hydrogen atoms have been ionized only the heavier trace elements like iron and calcium are able to retain a few of their electrons in this intense heat It is emission from these elements that produce the color associated with the emission line corona http://science.msfc.nasa.gov/ssl/pad/so ...
... Since hydrogen atoms have been ionized only the heavier trace elements like iron and calcium are able to retain a few of their electrons in this intense heat It is emission from these elements that produce the color associated with the emission line corona http://science.msfc.nasa.gov/ssl/pad/so ...
intro - Big Bear Solar Observatory
... Analysis of the non-thermal broadening of soft X-ray spectral lines in solar flares observed with Yohkoh (Alexander et al. 1998, Harra et al. 2001) showed that the non-thermal velocity begins to rise before the flare onset and peaks often before the Hard X-ray emission. COES X-ray flux ...
... Analysis of the non-thermal broadening of soft X-ray spectral lines in solar flares observed with Yohkoh (Alexander et al. 1998, Harra et al. 2001) showed that the non-thermal velocity begins to rise before the flare onset and peaks often before the Hard X-ray emission. COES X-ray flux ...
The Sun - Lauer Science
... ● Explain that the sun (like all stars) has a lifespan based on initial mass and that our sun’s life span is about 10 billion years. ● Using a model, predict how the relative proportions of hydrogen to helium change as the sun ages. Vocabulary: ● Radiation: heat transfer by electromagnetic waves ● S ...
... ● Explain that the sun (like all stars) has a lifespan based on initial mass and that our sun’s life span is about 10 billion years. ● Using a model, predict how the relative proportions of hydrogen to helium change as the sun ages. Vocabulary: ● Radiation: heat transfer by electromagnetic waves ● S ...
The Evolution of Coronal X
... An interesting question is to ask what did the Sun look like in the past? What was the overall level of its high energy irradiance? By how much did it vary? How frequently did it flare? Etc. Why is this important? Aside from the intrinsic interest of understanding how the mechanisms of generating an ...
... An interesting question is to ask what did the Sun look like in the past? What was the overall level of its high energy irradiance? By how much did it vary? How frequently did it flare? Etc. Why is this important? Aside from the intrinsic interest of understanding how the mechanisms of generating an ...
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.