Today`s Powerpoint
... C: They have much greater density than adjacent regions D: They have much higher temperature than adjacent regions ...
... C: They have much greater density than adjacent regions D: They have much higher temperature than adjacent regions ...
The Sun
... of protons and electrons ejected at high speed from the corona Travel through solar system and are lost to space Alters appearance of bodies in the solar system Earth’s magnetic field doesn’t allow them to reach our surface --> do affect our atmosphere ...
... of protons and electrons ejected at high speed from the corona Travel through solar system and are lost to space Alters appearance of bodies in the solar system Earth’s magnetic field doesn’t allow them to reach our surface --> do affect our atmosphere ...
Light and dark in this magnetic scan of the Sun indicate
... demonstrated that emission was principally of x ray photons a series of Nike-Asp rockets fired during the 1958 total solar eclipse demonstrated that the x-ray emission extended far beyond the visible disk of the sun and was concentrated in small regions on the surface These series of rocket observat ...
... demonstrated that emission was principally of x ray photons a series of Nike-Asp rockets fired during the 1958 total solar eclipse demonstrated that the x-ray emission extended far beyond the visible disk of the sun and was concentrated in small regions on the surface These series of rocket observat ...
The Sun
... brightening of the region above a sunspot cluster. • During their existence, solar flares release enormous amounts of energy, much of it in the form of ultraviolet, radio, and X-ray radiation. ...
... brightening of the region above a sunspot cluster. • During their existence, solar flares release enormous amounts of energy, much of it in the form of ultraviolet, radio, and X-ray radiation. ...
The Sun, at a mean distance of 92.96 million miles, is the closest
... drops below 3.5 million degrees Fahrenheit in the convective zone, where large bubbles of hot plasma (a soup of ionized atoms) move upwards. The Sun's "surface" - the photosphere - is a 300-mile-thick region, from which most of the Sun's radiation escapes outward and is detected as the sunlight we o ...
... drops below 3.5 million degrees Fahrenheit in the convective zone, where large bubbles of hot plasma (a soup of ionized atoms) move upwards. The Sun's "surface" - the photosphere - is a 300-mile-thick region, from which most of the Sun's radiation escapes outward and is detected as the sunlight we o ...
Solar Flares
... 2. A cool, dense filament forms, suspended by the magnetic field, over the neutral line. 3. The field evolves slowly through equilibrium states, finally reaching a non-equilibrium which causes the closed field to rise and erupts outward. 4. The reconnection of the field below the rising filament pro ...
... 2. A cool, dense filament forms, suspended by the magnetic field, over the neutral line. 3. The field evolves slowly through equilibrium states, finally reaching a non-equilibrium which causes the closed field to rise and erupts outward. 4. The reconnection of the field below the rising filament pro ...
The Sun - Cloudfront.net
... • Are the same number of sunspots always present on the sun? Explain. • No, because the number of sunspots varies in an 11-year cycle. ...
... • Are the same number of sunspots always present on the sun? Explain. • No, because the number of sunspots varies in an 11-year cycle. ...
day 1 hand out - the sun
... • very hot, unstable and changing outer solar “atmosphere” at about 1 000 000°C • extends millions of km above chromosphere • visible during total solar eclipse ...
... • very hot, unstable and changing outer solar “atmosphere” at about 1 000 000°C • extends millions of km above chromosphere • visible during total solar eclipse ...
Probing the Sources of Solar Magnetism with Helioseismology and Simulations PHYSICS COLLOQUIUM
... Abstract: There exist major challenges to understand how the Sun builds the large-scale and intense magnetic fields that we observe at its surface and how these fields evolve in time. The origin of these magnetic fields must rest with dynamo processes occurring deep within the star. Many complex dyn ...
... Abstract: There exist major challenges to understand how the Sun builds the large-scale and intense magnetic fields that we observe at its surface and how these fields evolve in time. The origin of these magnetic fields must rest with dynamo processes occurring deep within the star. Many complex dyn ...
10-Chapter%25206%252..
... generated in the core of the Sun, travel through the main body called it interior. They travel a zigzag path on their way out, as they are scattered back and forth by particles (mostly electrons). ...
... generated in the core of the Sun, travel through the main body called it interior. They travel a zigzag path on their way out, as they are scattered back and forth by particles (mostly electrons). ...
Review2
... c. Telescopes in and above the atmosphere – why we put them there. d. Challenges and solutions with observations at radio wavelengths, infrared, visible and x-rays. 3. The Sun a. Stability of the Sun: balance between gravity and pressure (so-called hydrostatic equilibrium – meaning static water, but ...
... c. Telescopes in and above the atmosphere – why we put them there. d. Challenges and solutions with observations at radio wavelengths, infrared, visible and x-rays. 3. The Sun a. Stability of the Sun: balance between gravity and pressure (so-called hydrostatic equilibrium – meaning static water, but ...
Spectral Classification of Stars
... • Region of sun’s atmosphere just above the photosphere. • Visible, UV, and X-ray lines from highly ionized gases • Temperature increases gradually from ≈ 4500 oK to ≈ 10,000 oK, then jumps to ≈ 1 million oK ...
... • Region of sun’s atmosphere just above the photosphere. • Visible, UV, and X-ray lines from highly ionized gases • Temperature increases gradually from ≈ 4500 oK to ≈ 10,000 oK, then jumps to ≈ 1 million oK ...
The Sun
... gases under low pressure • Few thousand kilometers thick • Found above the photosphere ...
... gases under low pressure • Few thousand kilometers thick • Found above the photosphere ...
$doc.title
... 3. a) Assuming a slap of plasma of cross-‐section A and thickness dx, containing nn neutral particles per unit volume with cross-‐sections σ, show that the flux of an incident beam of electrons varie ...
... 3. a) Assuming a slap of plasma of cross-‐section A and thickness dx, containing nn neutral particles per unit volume with cross-‐sections σ, show that the flux of an incident beam of electrons varie ...
The Sun - TeacherWeb
... • They can cause solar flares – Coronal mass ejections-eruptions from the surface of the sun (corona) – ions and radiation into space - Solar flares create solar winds ...
... • They can cause solar flares – Coronal mass ejections-eruptions from the surface of the sun (corona) – ions and radiation into space - Solar flares create solar winds ...
The Sun
... 7.The Sunspot cycle is ________ years long, but the solar cycle is ________ years long 8.The net result of the proton-proton chain is that ________ protons are fused into a nucleus of ________, two ________ are emitted, and energy is released in the form of ________________. Mass is ________. ...
... 7.The Sunspot cycle is ________ years long, but the solar cycle is ________ years long 8.The net result of the proton-proton chain is that ________ protons are fused into a nucleus of ________, two ________ are emitted, and energy is released in the form of ________________. Mass is ________. ...
F03HW08
... hot enough to sustain nuclear fusion. The temperature of the interior of the sun decreases from the center to the photosphere. At that point the temperature will be lower than is required to cause the nuclei to approach each other with sufficient energy to overcome the coulomb repulsion. Therefore, ...
... hot enough to sustain nuclear fusion. The temperature of the interior of the sun decreases from the center to the photosphere. At that point the temperature will be lower than is required to cause the nuclei to approach each other with sufficient energy to overcome the coulomb repulsion. Therefore, ...
Homework Solutions: Chapter 7, The Sun
... Q: What evidence do we have that corona has a very high temperature? A: The spectral emission lines of the corona are strongly broadened in wavelength, indicating extremely high temperature. Furthermore in the corona’s spectrum we find emission lines of highly ionized gases which also give us more e ...
... Q: What evidence do we have that corona has a very high temperature? A: The spectral emission lines of the corona are strongly broadened in wavelength, indicating extremely high temperature. Furthermore in the corona’s spectrum we find emission lines of highly ionized gases which also give us more e ...
solar-wind-magnetosphere-answers
... 1. the core, within which nuclear fusion takes place 2. the radiative zone, through which energy is transported by photons 3. the convective zone, where energy is transported by convection. 2. Describe the main event that occurs in each of the three parts. As above 3. List the parts of the atmospher ...
... 1. the core, within which nuclear fusion takes place 2. the radiative zone, through which energy is transported by photons 3. the convective zone, where energy is transported by convection. 2. Describe the main event that occurs in each of the three parts. As above 3. List the parts of the atmospher ...
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.