October 15 - Astronomy
... about the same number and size distribution of impacts. All the other geologic processes (volcanism, tectonics, and erosion) tend to erase impact craters on the surface. ...
... about the same number and size distribution of impacts. All the other geologic processes (volcanism, tectonics, and erosion) tend to erase impact craters on the surface. ...
Review 1
... 1. Photosphere produces the continuum spectrum peaking in yellow. This tells us that its temperature is 5800 K 2. Upper levels of Photosphere are cooler, making an absorption line spectrum. 3. Dark edges in Solar granules imply lower temperature. 4. The Chromosphere has an emission line spectrum. It ...
... 1. Photosphere produces the continuum spectrum peaking in yellow. This tells us that its temperature is 5800 K 2. Upper levels of Photosphere are cooler, making an absorption line spectrum. 3. Dark edges in Solar granules imply lower temperature. 4. The Chromosphere has an emission line spectrum. It ...
Comparison Between Sawteeth Oscillations in Bean and Oval
... Magnetic reconnection (the tearing and healing of magnetic field lines) is thought to be responsible for many disruptive events observed in plasmas. In particular, it is believed to play a role in the magnetic storms that periodically beset communication satellites, as well as in the sawtooth oscill ...
... Magnetic reconnection (the tearing and healing of magnetic field lines) is thought to be responsible for many disruptive events observed in plasmas. In particular, it is believed to play a role in the magnetic storms that periodically beset communication satellites, as well as in the sawtooth oscill ...
The solar energetic balance and the dynamics of the radiative zone
... • Introduction of all the dynamical phenomena in the 1D solar models, also 2-3D simulations • Very small effect on the solar structure except near the surface • Then we will examine the interplay between phenomena and estimate the potential for other cycles or variabilities than the 11 year in order ...
... • Introduction of all the dynamical phenomena in the 1D solar models, also 2-3D simulations • Very small effect on the solar structure except near the surface • Then we will examine the interplay between phenomena and estimate the potential for other cycles or variabilities than the 11 year in order ...
Picture - The Russell Elementary Science Experience
... Review over Sun Features I. Vocabulary 1. The surface of the sun is known as the photosphere, or sphere of light. This is the surface of the sun we see. 2. Above the photosphere is the sun’s atmosphere, the corona. 3. Sunspots are dark because they are cooler than the rest of the photosphere. 4. Sol ...
... Review over Sun Features I. Vocabulary 1. The surface of the sun is known as the photosphere, or sphere of light. This is the surface of the sun we see. 2. Above the photosphere is the sun’s atmosphere, the corona. 3. Sunspots are dark because they are cooler than the rest of the photosphere. 4. Sol ...
File
... Spectrograph –device used to break up the sun’s light into a spectrum. Scientist can determine the amount of elements that are present in a star’s atmosphere ...
... Spectrograph –device used to break up the sun’s light into a spectrum. Scientist can determine the amount of elements that are present in a star’s atmosphere ...
SOLAR ORBITER All the space you need
... and its energy directly or indirectly fuels almost every living thing on our planet. Furthermore, virtually all the energy we use to sustain our complex society has its origins in the sun’s rays hitting the Earth’s surface. Because of its fundamental importance to our existence, the Sun is a critica ...
... and its energy directly or indirectly fuels almost every living thing on our planet. Furthermore, virtually all the energy we use to sustain our complex society has its origins in the sun’s rays hitting the Earth’s surface. Because of its fundamental importance to our existence, the Sun is a critica ...
Astronomy
... 15. In the HR diagram, stable stars with the smallest mass and lowest temperature are found in the ______ of the diagram. a. center (main sequence) b. upper left corner c. upper right corner d. lower right corner ...
... 15. In the HR diagram, stable stars with the smallest mass and lowest temperature are found in the ______ of the diagram. a. center (main sequence) b. upper left corner c. upper right corner d. lower right corner ...
D.S.Q.:
... Bell Work: turn in Friday’s homework to the in box. 1. The sun is actually a ____ not a planet. ...
... Bell Work: turn in Friday’s homework to the in box. 1. The sun is actually a ____ not a planet. ...
CH 26 PPT
... times of peak solar activity, more than 100 sunspots can be seen. During periods of low solar activity, several days may pass where no sunspots are visible. The sunspot cycle averages about 11 years from one period of peak activity to the next. ...
... times of peak solar activity, more than 100 sunspots can be seen. During periods of low solar activity, several days may pass where no sunspots are visible. The sunspot cycle averages about 11 years from one period of peak activity to the next. ...
Unit 3 - Lesson 8.2 2011 Sun
... The sun rotates on its axis one time every 25 days. currents are caused as a heated material is forced away from the core while cooled materials fall back down. are darker, cooler areas visible on the sun’s photosphere are found in active regions and release large quantities of gas (big bulge) _____ ...
... The sun rotates on its axis one time every 25 days. currents are caused as a heated material is forced away from the core while cooled materials fall back down. are darker, cooler areas visible on the sun’s photosphere are found in active regions and release large quantities of gas (big bulge) _____ ...
space research in slovakia - Astronomical Institute WWW Homepage
... revealed a number of regularities over more than five solar cycles. A pronounced north/south asymmetry of the solar corona was identified and discussed including the quasi-biennial oscillations [1,2,5,22]. Observations of ten total solar eclipses (1973-1999) (Fig.3) enable to describe mutual relatio ...
... revealed a number of regularities over more than five solar cycles. A pronounced north/south asymmetry of the solar corona was identified and discussed including the quasi-biennial oscillations [1,2,5,22]. Observations of ten total solar eclipses (1973-1999) (Fig.3) enable to describe mutual relatio ...
Astronomy II (ASTR1020) — Exam 1 Test No. 1D
... 4. Which of the following best describes a photon’s journey inside the Sun? a) Travels in a straight line at the speed of 2.997925 × 105 km/s. b) Travels in a curved path following the Sun’s magnetic field. c) Travels in a zig-zag (random walk) type of path. d) Photons do not exist inside the Sun. e ...
... 4. Which of the following best describes a photon’s journey inside the Sun? a) Travels in a straight line at the speed of 2.997925 × 105 km/s. b) Travels in a curved path following the Sun’s magnetic field. c) Travels in a zig-zag (random walk) type of path. d) Photons do not exist inside the Sun. e ...
LETG Spring, 2015
... 2000 years ago by those precocious Chinese observers—it took until the early 1900’s and Hale’s spectrohelioscope to realize they were regions of strong magnetic field. A century later, we still do not really have a fully successful start-to-finish model for the dynamo that generates the solar magnet ...
... 2000 years ago by those precocious Chinese observers—it took until the early 1900’s and Hale’s spectrohelioscope to realize they were regions of strong magnetic field. A century later, we still do not really have a fully successful start-to-finish model for the dynamo that generates the solar magnet ...
Unit 49-59 Review
... b. As a solid body c. Due to its magnetic field 12. Magnetic field lines play a role in a. Sun spots b. Prominences c. Solar flares d. Coronal mass ejections e. All of the above 13. About how many years elapse between times of maximum solar activity? a. 3 b. 5 c. 11 d. 33 e. 105 14. Parallax is a. P ...
... b. As a solid body c. Due to its magnetic field 12. Magnetic field lines play a role in a. Sun spots b. Prominences c. Solar flares d. Coronal mass ejections e. All of the above 13. About how many years elapse between times of maximum solar activity? a. 3 b. 5 c. 11 d. 33 e. 105 14. Parallax is a. P ...
Life Cycle of Our Sun
... caused by the earth’s rotation. The moving molten metal in our core (mostly iron and nickel) is similar to common types of metals on Earth that have the capability of being magnetic. ...
... caused by the earth’s rotation. The moving molten metal in our core (mostly iron and nickel) is similar to common types of metals on Earth that have the capability of being magnetic. ...
The Sun (continued). - Department of Physics and Astronomy
... The X-ray Chandra Observatory 1999 The Spitzer Space (IR) Observatory 2003 ...
... The X-ray Chandra Observatory 1999 The Spitzer Space (IR) Observatory 2003 ...
EARTH SCIENCE HOMEWORK 11-7 Sun`s surface
... 1. Areas on the Sun’s surface that appear dark because they are cooler than surrounding areas are called __________. (730, P2) 2. Sunspots aren’t ___________ features of the Sun. The number of sunspots increases and decreases in a fairly regular pattern called a _________, or solar ___________, cycl ...
... 1. Areas on the Sun’s surface that appear dark because they are cooler than surrounding areas are called __________. (730, P2) 2. Sunspots aren’t ___________ features of the Sun. The number of sunspots increases and decreases in a fairly regular pattern called a _________, or solar ___________, cycl ...
welsch_harvey_20100526
... and can extend through the photosphere into the corona, coupling the Sun's interior with its outer atmosphere. Hence, measurements of magnetic fields at the photosphere can provide insights into magnetic evolution both in the interior and the outer atmosphere. While maps of the photospheric magnetic ...
... and can extend through the photosphere into the corona, coupling the Sun's interior with its outer atmosphere. Hence, measurements of magnetic fields at the photosphere can provide insights into magnetic evolution both in the interior and the outer atmosphere. While maps of the photospheric magnetic ...
Different wavelengths…
... What causes the sun’s magnetic field? The hydrogen atoms in the sun are actually ions (charged nuclei), in which the electrons are removed from the atoms because of the high temperature of the sun. As these ions move, they generate electric and magnetic fields – these moving fields are the lig ...
... What causes the sun’s magnetic field? The hydrogen atoms in the sun are actually ions (charged nuclei), in which the electrons are removed from the atoms because of the high temperature of the sun. As these ions move, they generate electric and magnetic fields – these moving fields are the lig ...
New Theory of Nuclear Fusion Processes in Sun and other
... This new hypothesis of nuclear fusion on the surface of the sun resolves the problem of coronal heating which cannot be explained using conventional model of fusion (with fusion inside the core of sun). With this new model of fusion all the heat is generated on the surface and this heat is dispersed ...
... This new hypothesis of nuclear fusion on the surface of the sun resolves the problem of coronal heating which cannot be explained using conventional model of fusion (with fusion inside the core of sun). With this new model of fusion all the heat is generated on the surface and this heat is dispersed ...
section 16 powerpoint
... Photosphere = light sphere. The region (disk) of the Sun from which light appears to originate. It also constitutes the solar atmosphere. Chromosphere = coloured sphere. The region lying above the solar photosphere containing spicules where the temperature increases with height. Corona = crown. The ...
... Photosphere = light sphere. The region (disk) of the Sun from which light appears to originate. It also constitutes the solar atmosphere. Chromosphere = coloured sphere. The region lying above the solar photosphere containing spicules where the temperature increases with height. Corona = crown. The ...
Extract, Datei
... (e.g. Schrijver & Zwaan 2000; Berdyugina et al. 2005; Fluri & Berdyugina 2005). The large sample of cool, active stars gives us therefore an ideal testing ground for improving our understanding of magnetic activity, by considering also a wider range of parameters (rotation rate, stellar structure, c ...
... (e.g. Schrijver & Zwaan 2000; Berdyugina et al. 2005; Fluri & Berdyugina 2005). The large sample of cool, active stars gives us therefore an ideal testing ground for improving our understanding of magnetic activity, by considering also a wider range of parameters (rotation rate, stellar structure, c ...
Magnetic field generation by sound waves in the solar atmosphere
... absorption of the waves is caused by "collisionless" resonance effects (such as Landau damping). On the other hand, in the case of the solar atmosphere, in which we are interested, the collision frequency is many orders higher than the frequency of the oscillations generated in the convective zone, ...
... absorption of the waves is caused by "collisionless" resonance effects (such as Landau damping). On the other hand, in the case of the solar atmosphere, in which we are interested, the collision frequency is many orders higher than the frequency of the oscillations generated in the convective zone, ...
Normal Stars - Chandra X
... The release of magnetic energy can occur steadily and provide for the heating of the tubes of hot gas which make up the stellar corona. Or it can occur violently and produce flares. Flares can occur on the Sun at any time, but their frequency tends to rise from a peak of five to ten a day and fall ...
... The release of magnetic energy can occur steadily and provide for the heating of the tubes of hot gas which make up the stellar corona. Or it can occur violently and produce flares. Flares can occur on the Sun at any time, but their frequency tends to rise from a peak of five to ten a day and fall ...
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.