Magnetic Reconnection Project - University of California
... density cavities that map the magnetic separatrix ...
... density cavities that map the magnetic separatrix ...
Chapter 13 section 2
... Sunspots look this way because they are cooler than the area around them. Scientists have been studying sunspots for hundreds of years. They have observed the way that sunspots move. The fact that sunspots move has led scientists to determine that the Sun rotates. However, the Sun does not rotate li ...
... Sunspots look this way because they are cooler than the area around them. Scientists have been studying sunspots for hundreds of years. They have observed the way that sunspots move. The fact that sunspots move has led scientists to determine that the Sun rotates. However, the Sun does not rotate li ...
Yeatman-Liddell College Preparatory Middle School Winter
... become a red giant. The core will continue to burn helium, the other main fuel in a star. A red giant can swell to a thousand times its previous size, although its core is still dense and no larger than Earth. Our own Sun is expected to swell to only 30 times its present diameter. It will look very ...
... become a red giant. The core will continue to burn helium, the other main fuel in a star. A red giant can swell to a thousand times its previous size, although its core is still dense and no larger than Earth. Our own Sun is expected to swell to only 30 times its present diameter. It will look very ...
Video: The `shape` of an electric field
... equations that now go by the name “Maxwell’s Equations” was to realize that changing electric fields also give rise to magnetic fields. Three sources of magnetic fields: ...
... equations that now go by the name “Maxwell’s Equations” was to realize that changing electric fields also give rise to magnetic fields. Three sources of magnetic fields: ...
Astronomy - Dallas ISD
... If a coronal mass ejection from the Sun reaches the Earth’s magnetosphere, it can disrupt communication and power generation on Earth. At what point in the solar cycle are these coronal mass ejections most frequent and why? A ...
... If a coronal mass ejection from the Sun reaches the Earth’s magnetosphere, it can disrupt communication and power generation on Earth. At what point in the solar cycle are these coronal mass ejections most frequent and why? A ...
E/DE
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=c/ov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=c/ov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
SolarGrandMinimaThreat Analysis
... The oceans are the key to unlocking the mysteries of climate change. About 70 percent of the Earth’s surface is covered in water, which absorbs sunlight and warms. The oceans act as a large planetary heat sink because they retain heat better than land masses. Considering the available data, it is cl ...
... The oceans are the key to unlocking the mysteries of climate change. About 70 percent of the Earth’s surface is covered in water, which absorbs sunlight and warms. The oceans act as a large planetary heat sink because they retain heat better than land masses. Considering the available data, it is cl ...
Presentation - Los Angeles City College
... Benefits: The CDM is smaller and lighter than current Doppler and Magnetoraph instruments that are used in space. The transverse field MOF should provide an improvement in the sensitivity of the CDM. ...
... Benefits: The CDM is smaller and lighter than current Doppler and Magnetoraph instruments that are used in space. The transverse field MOF should provide an improvement in the sensitivity of the CDM. ...
Spheromaks, solar prominences, and Alfvén instability of current
... hence the λ profile. However, most plasmas of interest (solar, magnetospheric, and laboratory) have insufficient resistivity for resistive tearing modes to be relevant because their growth rate is much too slow (hence the oft-used invocation of ‘anomalous’ resistivity). Observational evidence points ...
... hence the λ profile. However, most plasmas of interest (solar, magnetospheric, and laboratory) have insufficient resistivity for resistive tearing modes to be relevant because their growth rate is much too slow (hence the oft-used invocation of ‘anomalous’ resistivity). Observational evidence points ...
ppt - Astronomy at Swarthmore College
... The geometry and viewing angle are relatively well established for this star. There is a 45 tilt between the rotation axis and both the magnetic axis and the direction of the Earth: we see a full range of viewing angles of the magnetosphere, and have Chandra observations for four of ...
... The geometry and viewing angle are relatively well established for this star. There is a 45 tilt between the rotation axis and both the magnetic axis and the direction of the Earth: we see a full range of viewing angles of the magnetosphere, and have Chandra observations for four of ...
2. Stellar Physics
... Problem of stellar structure is simplified by making several reasonable assumptions, which hold in most (not all) cases. 1) Spherical symmetry An isolated, non-rotating star which does not contain strong magnetic fields will be spherically symmetric, i.e.: All quantities (e.g. density, temperature, ...
... Problem of stellar structure is simplified by making several reasonable assumptions, which hold in most (not all) cases. 1) Spherical symmetry An isolated, non-rotating star which does not contain strong magnetic fields will be spherically symmetric, i.e.: All quantities (e.g. density, temperature, ...
A coupled PIC-Poisson-solver code for the extraction of charged
... Neutral beams from negative ion sources are expected to be one of the heating techniques chosen for ITER. The numerical simulation of the production and extraction mechanisms of negative hydrogen ions is necessary for the optimization of the source efficiency and as basis for the ion optics. Numeric ...
... Neutral beams from negative ion sources are expected to be one of the heating techniques chosen for ITER. The numerical simulation of the production and extraction mechanisms of negative hydrogen ions is necessary for the optimization of the source efficiency and as basis for the ion optics. Numeric ...
The Nature of Light II
... q The brightness of a star is measured in terms of the radiant flux received from the star by observers. q The radiant flux is the total amount of light energy of all wavelength that crosses a unit area oriented perpendicular to the direction of the light’s travel per unit time. q It is the nu ...
... q The brightness of a star is measured in terms of the radiant flux received from the star by observers. q The radiant flux is the total amount of light energy of all wavelength that crosses a unit area oriented perpendicular to the direction of the light’s travel per unit time. q It is the nu ...
PYTS/ASTR 206 – The Sun
... Magnetic field lines inhibit convection where they intersect the surface Surface cools off – sunspot forms Sunspots are ~4500K ...
... Magnetic field lines inhibit convection where they intersect the surface Surface cools off – sunspot forms Sunspots are ~4500K ...
1st EXAM VERSION C - Department of Physics and Astronomy
... C. *two stars whose combined light output when measured from Earth appears to vary periodically as the two stars move in front of one another. D. two stars that are clearly seen as separate but associated in the sky. 25. Absorption lines in the spectra of some binary stars are seen to change periodi ...
... C. *two stars whose combined light output when measured from Earth appears to vary periodically as the two stars move in front of one another. D. two stars that are clearly seen as separate but associated in the sky. 25. Absorption lines in the spectra of some binary stars are seen to change periodi ...
Presentation 1: Spectroscopy
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=c/ov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=c/ov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
Review Sheet // Study Guide: ESS Semester II 2002
... 3. What is the difference between actual motion and apparent motion of stars? Give examples of each. 4. What is the difference between absolute and apparent magnitude? 5. Which star is the brighter one with an apparent magnitude of 4 or –1? 6. What happens during the various stages of stellar evolut ...
... 3. What is the difference between actual motion and apparent motion of stars? Give examples of each. 4. What is the difference between absolute and apparent magnitude? 5. Which star is the brighter one with an apparent magnitude of 4 or –1? 6. What happens during the various stages of stellar evolut ...
Fingerprints in Sunlight Notes
... The Sun emits a continuous spectrum All light from the Sun comes from the surface, or photosphere, 5800 degrees K As the atoms bounce around the photosphere, photons are constantly being absorbed and re-emitted Although the original light was traveling our way, re-emitted photons are sent off in all ...
... The Sun emits a continuous spectrum All light from the Sun comes from the surface, or photosphere, 5800 degrees K As the atoms bounce around the photosphere, photons are constantly being absorbed and re-emitted Although the original light was traveling our way, re-emitted photons are sent off in all ...
Return-current formation in the electron beam – plasma system
... of the electron beam and (b) electromagnetic effects of the beam electric current (van den Oord, 1990). Return-current effects on the dynamics of nonthermal electron beams and the heating of the flare atmosphere have been described and studied by Emslie (1980), Karlický et al. (1990), Karlický and ...
... of the electron beam and (b) electromagnetic effects of the beam electric current (van den Oord, 1990). Return-current effects on the dynamics of nonthermal electron beams and the heating of the flare atmosphere have been described and studied by Emslie (1980), Karlický et al. (1990), Karlický and ...
Friday, April 11
... – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. First letter is the spectral type: K (one of OBAFGKM), the arab number (5) is like a second digit to the spectral type, so K0 is very close to G, K9 is very close to M. ...
... – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. First letter is the spectral type: K (one of OBAFGKM), the arab number (5) is like a second digit to the spectral type, so K0 is very close to G, K9 is very close to M. ...
ppt document - FacStaff Home Page for CBU
... Solar Flair Marshal Space Flight Center relatively cool, the areas around sunspots are very active with the result that when there are more sunspots there is generally a little more power being put out by the sun. Solar flares often are seen in these areas around sunspots. Solar flares last about 20 ...
... Solar Flair Marshal Space Flight Center relatively cool, the areas around sunspots are very active with the result that when there are more sunspots there is generally a little more power being put out by the sun. Solar flares often are seen in these areas around sunspots. Solar flares last about 20 ...
Section_32_Magnetic_..
... Magnetic reconnection can occur as a steady state process in which two oppositely directed magnetic fields are pushed together by external means. The reconnection then occurs at a constant rate . Magnetic reconnection can also occur spontaneously as a resistive instability. The magnetic island the ...
... Magnetic reconnection can occur as a steady state process in which two oppositely directed magnetic fields are pushed together by external means. The reconnection then occurs at a constant rate . Magnetic reconnection can also occur spontaneously as a resistive instability. The magnetic island the ...
Driven reconnection and bursty bulk flows
... where 81,2 is given by Eqs. (9) and (10). For γ < 0, the driven reconnection lasts for a very brief period and hence it is termed as a bursty type of reconnection. For the parameters of the near-Earth plasma, |γ | is typically of the order of one minute or so. The numerical simulation of driven reco ...
... where 81,2 is given by Eqs. (9) and (10). For γ < 0, the driven reconnection lasts for a very brief period and hence it is termed as a bursty type of reconnection. For the parameters of the near-Earth plasma, |γ | is typically of the order of one minute or so. The numerical simulation of driven reco ...
b - GPSM
... Focus on potential arc generator region, by using conjugated FAST and CLUSTER data (at 4000km and 100000km altitude, respectively). CLUSTER ESA mission consisting of 4 identical s/c, each of them equipped with 11 identical instruments. Launched in July – August 2000, after a failed start in ...
... Focus on potential arc generator region, by using conjugated FAST and CLUSTER data (at 4000km and 100000km altitude, respectively). CLUSTER ESA mission consisting of 4 identical s/c, each of them equipped with 11 identical instruments. Launched in July – August 2000, after a failed start in ...
Dynamical theory of the solar wind
... extended temperatures lead to equilibria which are subsonic or static. The hypothetical case of a corona with no energy supply other than thermal conduction from its base is considered at some length because the equations may be solved by analytical methods and illustrate the transition from subsoni ...
... extended temperatures lead to equilibria which are subsonic or static. The hypothetical case of a corona with no energy supply other than thermal conduction from its base is considered at some length because the equations may be solved by analytical methods and illustrate the transition from subsoni ...
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.