Chapter8
... 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! ...
Layers of the Sun (~ 75% Hydrogen ~ 25% Helium)
... Granules: A roughly circular region on the Sun whose bright center indicates hot gases rising to the surface, and whose dark edges indicate cooled gases that are descending towards the interior. Individual granules appear and disappear on time scales of about 5 minutes and are typically about 1000 k ...
... Granules: A roughly circular region on the Sun whose bright center indicates hot gases rising to the surface, and whose dark edges indicate cooled gases that are descending towards the interior. Individual granules appear and disappear on time scales of about 5 minutes and are typically about 1000 k ...
Chapter 2 - The Solar System
... A solar flare is a violent explosion in the Sun's atmosphere with an energy equivalent to tens of millions of hydrogen bombs. The frequency of solar flares varies, from several per day when the Sun is particularly "active" to less than one each week when the Sun is "quiet". Solar flares may take sev ...
... A solar flare is a violent explosion in the Sun's atmosphere with an energy equivalent to tens of millions of hydrogen bombs. The frequency of solar flares varies, from several per day when the Sun is particularly "active" to less than one each week when the Sun is "quiet". Solar flares may take sev ...
sun notes
... Top layer of the Sun’s atmosphere. It extends several million kilometers from the top of the chromosphere. It has a temperature range of 1 million____ to 2 million__ Kelvin. The _density____ of the gas in the corona is so low that it can only be seen during a total solar eclipse. o Gas flows out ...
... Top layer of the Sun’s atmosphere. It extends several million kilometers from the top of the chromosphere. It has a temperature range of 1 million____ to 2 million__ Kelvin. The _density____ of the gas in the corona is so low that it can only be seen during a total solar eclipse. o Gas flows out ...
Questions about the Sun:
... oddly sequenced because they were assigned long ago before we understood their relationship to temperature. O and B stars are rare but very bright; M stars are numerous but dim. The Sun is designated as a ____ star. A). G2 B). K1 C). M1 ...
... oddly sequenced because they were assigned long ago before we understood their relationship to temperature. O and B stars are rare but very bright; M stars are numerous but dim. The Sun is designated as a ____ star. A). G2 B). K1 C). M1 ...
Helioseismology and the Helium Abundance
... It takes only a brief scrutiny of the equations describing the structure and dynamical evolution of the Sun (it is not quite so brief to derive them) and the equations governing the low-amplitude seismic modes of oscillation to appreciate what broadly can, at least in principle, be reliably inferred ...
... It takes only a brief scrutiny of the equations describing the structure and dynamical evolution of the Sun (it is not quite so brief to derive them) and the equations governing the low-amplitude seismic modes of oscillation to appreciate what broadly can, at least in principle, be reliably inferred ...
Astronomy 10B Study Guide – by Chapter
... Flares – X-ray explosions more powerful than 1,000,000 H-bombs Can injure astronauts in space Can damage spacecraft Also release bursts of high speed electrons and protons Coronal Mass Ejection’s (CME’s) – ejections of hot plasma Sometimes they have magnetic fields These mag fields can tangle with E ...
... Flares – X-ray explosions more powerful than 1,000,000 H-bombs Can injure astronauts in space Can damage spacecraft Also release bursts of high speed electrons and protons Coronal Mass Ejection’s (CME’s) – ejections of hot plasma Sometimes they have magnetic fields These mag fields can tangle with E ...
Solar Nebula Theory
... Radiation Zone (350,000 km region that surrounds core) Energy is transported by absorption/emission of photons by atoms: ...
... Radiation Zone (350,000 km region that surrounds core) Energy is transported by absorption/emission of photons by atoms: ...
What is the Sun? - River Dell Regional School District
... of hot ionized gas (plasma) above the locations of Sunspots. Notice that the shapes of these loops are just like the loops of force between two opposite poles of a magnetic field. The plasma acts just like iron filings and traces out the magnetic field on the Sun. ...
... of hot ionized gas (plasma) above the locations of Sunspots. Notice that the shapes of these loops are just like the loops of force between two opposite poles of a magnetic field. The plasma acts just like iron filings and traces out the magnetic field on the Sun. ...
The Sun - bronzan.net
... will rise before you. To see such a sight, however, you will need to look in the direction of the ecliptic. All of the planets and their moons orbit the Sun in nearly the same plane, the ecliptic plane. From the Earth, this means that each day they will all rise in nearly the same direction - and la ...
... will rise before you. To see such a sight, however, you will need to look in the direction of the ecliptic. All of the planets and their moons orbit the Sun in nearly the same plane, the ecliptic plane. From the Earth, this means that each day they will all rise in nearly the same direction - and la ...
Astronomy – Name: ______KEY___________________ Date
... 21. About how many miles is the earth from the sun? 93 M miles 22. What is meant by “space weather” in this context? The activity of the sun, and how it impacts the earth 23. How many years does a solar cycle last? 11 years 24. The peak of these cycles is called a solar maximum. 25. The surface of t ...
... 21. About how many miles is the earth from the sun? 93 M miles 22. What is meant by “space weather” in this context? The activity of the sun, and how it impacts the earth 23. How many years does a solar cycle last? 11 years 24. The peak of these cycles is called a solar maximum. 25. The surface of t ...
The Sun - Judson ISD
... high-density gas from the solar chromosphere into the corona where it can be seen during a solar eclipse or by observing strong spectral lines in its emission spectrum. ...
... high-density gas from the solar chromosphere into the corona where it can be seen during a solar eclipse or by observing strong spectral lines in its emission spectrum. ...
Document
... microwave emission can be used for coronal magnetic loops and loops current diagnostics. ...
... microwave emission can be used for coronal magnetic loops and loops current diagnostics. ...
slide-show source file - Bartol Research Institute
... For cool Red Giant stars, P-Cygni profiles suggest relatively slow speeds, 10-50 km/s, but with mass loss rates up to million times that of the solar wind, i.e., ~ 10-8 MO/yr. For these cool-star winds, the driving mechanism is not well understood, but may involve a combination of stellar pulsatio ...
... For cool Red Giant stars, P-Cygni profiles suggest relatively slow speeds, 10-50 km/s, but with mass loss rates up to million times that of the solar wind, i.e., ~ 10-8 MO/yr. For these cool-star winds, the driving mechanism is not well understood, but may involve a combination of stellar pulsatio ...
Chapter 08
... Energy generated in the sun’s center must be transported outward. In the photosphere, this happens through ...
... Energy generated in the sun’s center must be transported outward. In the photosphere, this happens through ...
21.1 wksht
... Section: Formation of the Solar System 1. Describe how current models of the solar system differ from either Aristotle’s or Copernicus’s model. _________________________________________________________________ _________________________________________________________________ ________________________ ...
... Section: Formation of the Solar System 1. Describe how current models of the solar system differ from either Aristotle’s or Copernicus’s model. _________________________________________________________________ _________________________________________________________________ ________________________ ...
19.3 Key Terms
... Section: Formation of the Solar System 1. Describe how current models of the solar system differ from either Aristotle’s or Copernicus’s model. _________________________________________________________________ _________________________________________________________________ ________________________ ...
... Section: Formation of the Solar System 1. Describe how current models of the solar system differ from either Aristotle’s or Copernicus’s model. _________________________________________________________________ _________________________________________________________________ ________________________ ...
What Are Sunspots?
... called plasma. (On Earth, most matter exists in one of three states: solid, liquid, or gas. On the sun, a fourth state of matter is found -- plasma.) On Earth, burning fossil fuels like gasoline or coal gives us energy for our cars and heating our homes. But the sun's energy doesn't come from burnin ...
... called plasma. (On Earth, most matter exists in one of three states: solid, liquid, or gas. On the sun, a fourth state of matter is found -- plasma.) On Earth, burning fossil fuels like gasoline or coal gives us energy for our cars and heating our homes. But the sun's energy doesn't come from burnin ...
Chapter 9 The Sun - Otto
... chromosphere • Temperature climbs through transition zone • Reaches several million K in corona ...
... chromosphere • Temperature climbs through transition zone • Reaches several million K in corona ...
The Sun Sun
... boundaries exist between its various layers layers. Keeping this in mind, we can divide the sun into four parts: the solar interior; the visible surface, or photosphere; and two atmospheric layers, the chromosphere and corona. ...
... boundaries exist between its various layers layers. Keeping this in mind, we can divide the sun into four parts: the solar interior; the visible surface, or photosphere; and two atmospheric layers, the chromosphere and corona. ...
Chapter 9: Our Star, the Sun
... Some solar flares and some prominences are powerful enough that they can cause a CME. ...
... Some solar flares and some prominences are powerful enough that they can cause a CME. ...
electromagnetic spectrum
... Keeping this in mind, we can divide the sun into four parts: the solar interior; the visible surface, or photosphere; and two atmospheric layers, the chromosphere and corona. ...
... Keeping this in mind, we can divide the sun into four parts: the solar interior; the visible surface, or photosphere; and two atmospheric layers, the chromosphere and corona. ...
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.