On the origin of the fast solar wind in polar coronal funnels
... find a diverging magnetic field, which tends (coming from its compressed state in the convection zone) to expand initially and to become finally homogeneous in the corona. The solar wind flows through this funnel structure, which is described by the magnetic field, and exactly follows the magnetic f ...
... find a diverging magnetic field, which tends (coming from its compressed state in the convection zone) to expand initially and to become finally homogeneous in the corona. The solar wind flows through this funnel structure, which is described by the magnetic field, and exactly follows the magnetic f ...
Our Sun - Stephen W. Ramsden
... Stellar fusion reactions gradually convert hydrogen into helium through the p-p chain. When a star runs out of hydrogen fuel, it either stops burning (becoming a dwarf star) or, if it is large enough (so that gravity compresses the helium strongly) it begins burning the helium into heavier elements. ...
... Stellar fusion reactions gradually convert hydrogen into helium through the p-p chain. When a star runs out of hydrogen fuel, it either stops burning (becoming a dwarf star) or, if it is large enough (so that gravity compresses the helium strongly) it begins burning the helium into heavier elements. ...
Chapter 5 Summary
... Electrons in an atom may occupy various permitted orbits around the nucleus but not orbits in between. The size of an electron's orbit depends on the energy stored in the electron's motion. An electron may be excited to a higher orbit during a collision between atoms, or it may move from one orbit t ...
... Electrons in an atom may occupy various permitted orbits around the nucleus but not orbits in between. The size of an electron's orbit depends on the energy stored in the electron's motion. An electron may be excited to a higher orbit during a collision between atoms, or it may move from one orbit t ...
Brown Dwarfs and M Dwarfs
... • Low mass “objects” do not have stable thermonuclear reactions to heat their cores and halt the gravitational contraction → rapid rotation and degenerate convective cores → secular cooling of the atmosphere. • Cool atmospheres have very low ionization → decoupling of turbulent flows and magnetic fi ...
... • Low mass “objects” do not have stable thermonuclear reactions to heat their cores and halt the gravitational contraction → rapid rotation and degenerate convective cores → secular cooling of the atmosphere. • Cool atmospheres have very low ionization → decoupling of turbulent flows and magnetic fi ...
The Universe: Secrets of the Sun (History Channel production)
... 4. The material in the Sun is not considered a gas; it is called a ________________________. 5. The fusion of two hydrogen atoms produces helium particles with extra mass; this mass is given off as __________________________. 6. Particles of light and heat are called _________________________; once ...
... 4. The material in the Sun is not considered a gas; it is called a ________________________. 5. The fusion of two hydrogen atoms produces helium particles with extra mass; this mass is given off as __________________________. 6. Particles of light and heat are called _________________________; once ...
SNC 1D - othsmath
... at a temperature of about 10,000,000C in the area surrounding the Sun’s core.) The surface layer of the Sun. The temperature here is usually around 6 000oC. An area of strong magnetic fields on the photosphere of the Sun. These areas are cooler than the rest of the photosphere at about 4 500oC so t ...
... at a temperature of about 10,000,000C in the area surrounding the Sun’s core.) The surface layer of the Sun. The temperature here is usually around 6 000oC. An area of strong magnetic fields on the photosphere of the Sun. These areas are cooler than the rest of the photosphere at about 4 500oC so t ...
Slide 1
... loop. The electrically charged plasma in the prominence allows the prominence to be shaped by the magnetic field. ...
... loop. The electrically charged plasma in the prominence allows the prominence to be shaped by the magnetic field. ...
Chapter 12 (Sun)
... 2. The solar corona is much hotter than the photosphere. yet it is the latter that dominates our daytime sky. When can we see the corona, and why is it so faint? 3. Explain why the photosphere gives off a continuous spectrum with some absorption lines, yet the spectrum of the corona is bright emissi ...
... 2. The solar corona is much hotter than the photosphere. yet it is the latter that dominates our daytime sky. When can we see the corona, and why is it so faint? 3. Explain why the photosphere gives off a continuous spectrum with some absorption lines, yet the spectrum of the corona is bright emissi ...
SL2 IIIC Carter 280911 - Particle Solids Interactions group
... Debate has been going on for centuries! • The intense localised magnetic field in the umbra reduces the flow of hot material to that region of the Photosphere. • Alternatively, strong magnetic fields enhance flow of heat but converts about 80% into “hydromagnetic waves” which propagate through the P ...
... Debate has been going on for centuries! • The intense localised magnetic field in the umbra reduces the flow of hot material to that region of the Photosphere. • Alternatively, strong magnetic fields enhance flow of heat but converts about 80% into “hydromagnetic waves” which propagate through the P ...
Fact Sheet - Solar Probe Plus - The Johns Hopkins University
... our knowledge of the origin and evolution of the solar wind. It will also make critical contributions to our ability to forecast changes in Earth’s space environment that impact life and technology on Earth. ...
... our knowledge of the origin and evolution of the solar wind. It will also make critical contributions to our ability to forecast changes in Earth’s space environment that impact life and technology on Earth. ...
The Turbulent Sun - Beck-Shop
... A word of warning here: Solar observing can be dangerous, and to look straight at the Sun through any telescope or binoculars will result in eye damage – perhaps blindness – unless careful precautions are taken. Fitting a dark filter over the telescope eyepiece is not recommended for the newcomer; f ...
... A word of warning here: Solar observing can be dangerous, and to look straight at the Sun through any telescope or binoculars will result in eye damage – perhaps blindness – unless careful precautions are taken. Fitting a dark filter over the telescope eyepiece is not recommended for the newcomer; f ...
lec1_2008 - Stanford Solar Physics
... Feb. 14, Thursday. Solar atmosphere. The structure of the solar atmosphere, photosphere, chromosphere, corona. Transition region. Chromospheric network, filaments, prominences, spicules. Feb. 19, Tuesday. Sunspots. Active regions. Flux tubes. Observations. Static models. Flows, Evershed effect. Form ...
... Feb. 14, Thursday. Solar atmosphere. The structure of the solar atmosphere, photosphere, chromosphere, corona. Transition region. Chromospheric network, filaments, prominences, spicules. Feb. 19, Tuesday. Sunspots. Active regions. Flux tubes. Observations. Static models. Flows, Evershed effect. Form ...
Year of the Sun
... distorted and energy starts to build up. Under the right conditions this energy is released, producing a huge explosion that is called a solar flare. Solar flares manifest themselves in many ways and their symptoms last from minutes to hours. They heat up gases in the solar atmosphere to 100 million ...
... distorted and energy starts to build up. Under the right conditions this energy is released, producing a huge explosion that is called a solar flare. Solar flares manifest themselves in many ways and their symptoms last from minutes to hours. They heat up gases in the solar atmosphere to 100 million ...
PPT - DOE Plasma Science Center
... facilitates crystal growth while neutral gas heating inhibits growth. ...
... facilitates crystal growth while neutral gas heating inhibits growth. ...
Magnetic reconnection
... Original idea is converting magnetic field energy to plasma kinetic energy. Recently plasma heating, particle acceleration and wave excitation are also well discussed in the category of magnetic reconnection. These energy conversion rates are heavily depending on the plasma conditions. In that sense ...
... Original idea is converting magnetic field energy to plasma kinetic energy. Recently plasma heating, particle acceleration and wave excitation are also well discussed in the category of magnetic reconnection. These energy conversion rates are heavily depending on the plasma conditions. In that sense ...
Atmosphere
... sunspots may be visible After, they decrease Cycle begins when more sunspots begin to appear ...
... sunspots may be visible After, they decrease Cycle begins when more sunspots begin to appear ...
The Sun Worksheet
... 12. In which layer of the Sun do temperatures reach about 15 million degrees Celsius? ...
... 12. In which layer of the Sun do temperatures reach about 15 million degrees Celsius? ...
The Electromagnetic Spectrum
... Hydrogen fusion to Helium • The sun’s core is 10 million °K. • At this temperature, hydrogen nuclei fuse into helium • Huge amounts of energy are released. ...
... Hydrogen fusion to Helium • The sun’s core is 10 million °K. • At this temperature, hydrogen nuclei fuse into helium • Huge amounts of energy are released. ...
Inospheric Physics refresher
... 8. The part of the atmosphere where also ionosphere is located is called _____________________________. Below it, ________________________ is located and the coldest place in the atmosphere is at __________________ 9. The ionospheric regions from down to up are: _________________________. During nig ...
... 8. The part of the atmosphere where also ionosphere is located is called _____________________________. Below it, ________________________ is located and the coldest place in the atmosphere is at __________________ 9. The ionospheric regions from down to up are: _________________________. During nig ...
Stars
... Movie starting with photosphere, then chromosphere, then x-ray view of corona. Note the connections between locations of sunpots in photosphere, and activity further out. ...
... Movie starting with photosphere, then chromosphere, then x-ray view of corona. Note the connections between locations of sunpots in photosphere, and activity further out. ...
The ADAHELI (ADvanced Astronomy for HELIophysics) solar mission
... Italian project for the investigation of solar activity and dynamics proposed in the framework of ASI Italian Space Agency Small Missions Program call. It is devoted to the study of photospheric and chromospheric structure and dynamics. The scientific payload consists of ISODY, a telescope with a fo ...
... Italian project for the investigation of solar activity and dynamics proposed in the framework of ASI Italian Space Agency Small Missions Program call. It is devoted to the study of photospheric and chromospheric structure and dynamics. The scientific payload consists of ISODY, a telescope with a fo ...
introduction to heliophysics
... temporal data. It has gradually become clear to solar scientists that much of the observed structure owes its existence to the Sun’s magnetic field. This major discovery brought new insights into the detailed structure of the solar interior, solar atmosphere, solar wind and their coupling. These phy ...
... temporal data. It has gradually become clear to solar scientists that much of the observed structure owes its existence to the Sun’s magnetic field. This major discovery brought new insights into the detailed structure of the solar interior, solar atmosphere, solar wind and their coupling. These phy ...
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.