The Sun`s Exterior
... is the layer that contains the bright red storms visible during a solar eclipse. The temperature in the chromosphere ...
... is the layer that contains the bright red storms visible during a solar eclipse. The temperature in the chromosphere ...
(Sol) Basic information Sun “Sol” Size
... • energy is transported outward from core • conduction: energy transfer via atomic collisions (eg) iron frying pan on the stove • convection: energy carried by fluid motion (eg) water on the stove; thunderheads • radiation: energy radiated via EM waves (eg) a nice fire; you! CLICKER: Sunshine warms ...
... • energy is transported outward from core • conduction: energy transfer via atomic collisions (eg) iron frying pan on the stove • convection: energy carried by fluid motion (eg) water on the stove; thunderheads • radiation: energy radiated via EM waves (eg) a nice fire; you! CLICKER: Sunshine warms ...
approximate temperature of the corona
... The magnetic field of the Sun can be clearly seen affecting the shape of the corona, which spreads out an enormous distance from the Sun. The poles show the orientation of the Sun. A false eclipse or coronagraph view of the corona can be produced when a total eclipse is not occurring. An opaque, cir ...
... The magnetic field of the Sun can be clearly seen affecting the shape of the corona, which spreads out an enormous distance from the Sun. The poles show the orientation of the Sun. A false eclipse or coronagraph view of the corona can be produced when a total eclipse is not occurring. An opaque, cir ...
The Sun
... • Class G • Color Yellow • Surface Temperature 5,000 – 6,000 ºC • Elements hydrogen and helium • Greek word for Sun is Helios ...
... • Class G • Color Yellow • Surface Temperature 5,000 – 6,000 ºC • Elements hydrogen and helium • Greek word for Sun is Helios ...
Comparing Earth, Sun and Jupiter
... Energy is transported to the surface via either radiation or convection. The Sun has a convective envelope and radiative interior. Low mass main-sequence stars are entirely convective. More massive stars are much more luminous (the fusion reactions release much more energy) Therefore they bu ...
... Energy is transported to the surface via either radiation or convection. The Sun has a convective envelope and radiative interior. Low mass main-sequence stars are entirely convective. More massive stars are much more luminous (the fusion reactions release much more energy) Therefore they bu ...
Fundamental properties of the Sun - University of Iowa Astronomy
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
... The Sun has a “heartbeat”; its properties change on a period of 11 years ...
Sun: The Nearest Star
... giant. After a billion years as a red giant, it will suddenly collapse into a white dwarf. It may take a trillion years to cool off completely. The Sun's period of rotation at the surface varies from approximately 25 days at the equator to 36 days at the poles. Deep down, below the convective zone, ...
... giant. After a billion years as a red giant, it will suddenly collapse into a white dwarf. It may take a trillion years to cool off completely. The Sun's period of rotation at the surface varies from approximately 25 days at the equator to 36 days at the poles. Deep down, below the convective zone, ...
sunspots
... • streaming electrically charged atomic particles that constantly escape from the Sun through coronal holes, which are weak spots in the Sun’s magnetic field. • It is faster and much hotter than Earth’s wind. • Solar wind is traveling at about 1 million miles an hour by the time it gets close to Ear ...
... • streaming electrically charged atomic particles that constantly escape from the Sun through coronal holes, which are weak spots in the Sun’s magnetic field. • It is faster and much hotter than Earth’s wind. • Solar wind is traveling at about 1 million miles an hour by the time it gets close to Ear ...
SolarDermatology
... Prominence: an elongated structure full of material 100x cooler and denser than the corona (like cool clouds). Held up by magnetic structures, they can live for weeks/months, and are seen as bright against the black background of space. They can reach heights of several 100,000 km above the limb. ...
... Prominence: an elongated structure full of material 100x cooler and denser than the corona (like cool clouds). Held up by magnetic structures, they can live for weeks/months, and are seen as bright against the black background of space. They can reach heights of several 100,000 km above the limb. ...
27Oct_2014
... • Just below the photosphere is the convection zone. – Energy is transported from deeper in the Sun by convection, in patterns similar to those found in a pot of boiling water (hot gas rises, dumps its energy into the photosphere, and then sinks) ...
... • Just below the photosphere is the convection zone. – Energy is transported from deeper in the Sun by convection, in patterns similar to those found in a pot of boiling water (hot gas rises, dumps its energy into the photosphere, and then sinks) ...
The Sun as We See It Lecture 10, September 17, 2003
... • The age of the Sun (how could we know this?) • Comparison of other objects (M4, Arcturus) ...
... • The age of the Sun (how could we know this?) • Comparison of other objects (M4, Arcturus) ...
Electromagnetic Radiation
... • Sunspots appear dark because of their temperature, which is about 1500 K less than that of the surrounding solar surface. Prominences • Prominences are huge cloudlike structures consisting of chromospheric gases. • Prominences are ionized gases trapped by magnetic fields that extend from regions ...
... • Sunspots appear dark because of their temperature, which is about 1500 K less than that of the surrounding solar surface. Prominences • Prominences are huge cloudlike structures consisting of chromospheric gases. • Prominences are ionized gases trapped by magnetic fields that extend from regions ...
The Easily Visible Sky Tools of Astronomy Stars Galaxies Cosmology
... Each Granule is about the size of Texas and lasts for only 10-20 minutes before fading away! ...
... Each Granule is about the size of Texas and lasts for only 10-20 minutes before fading away! ...
The Sun - University of Minnesota
... Nuclear fusion • E=mc2 • Cloud of gas collapsed, releasing potential energy • Gas heats • Gravity creates high pressure • High pressure and temperature allow nuclear fusion ...
... Nuclear fusion • E=mc2 • Cloud of gas collapsed, releasing potential energy • Gas heats • Gravity creates high pressure • High pressure and temperature allow nuclear fusion ...
Our Sun is a Star:
... picture? (Hint: they are not sunspots.) ___ Coronal Holes ___ Plumes ___ Active Regions ...
... picture? (Hint: they are not sunspots.) ___ Coronal Holes ___ Plumes ___ Active Regions ...
The Sun as the prime example of stellar structure and evolution
... • Photosphere • Chromosphere • Corona ...
... • Photosphere • Chromosphere • Corona ...
Advanced Solar Theory (MT5810)
... see as long, thin structures Dark - cutting out light from below ...
... see as long, thin structures Dark - cutting out light from below ...
summary of key concepts: week #1
... 2. A galaxy is an `island of stars’ held together by gravity. Our own galaxy, called the Milky Way, has about 100 billion stars. On the largest scale (of the whole observable Universe) the galaxy is the basic building block. Galaxies often collide with each other (very very slowly, over billions of ...
... 2. A galaxy is an `island of stars’ held together by gravity. Our own galaxy, called the Milky Way, has about 100 billion stars. On the largest scale (of the whole observable Universe) the galaxy is the basic building block. Galaxies often collide with each other (very very slowly, over billions of ...
The Sun: close-up of a spectral class G main sequence star
... The Sun: close-up of a spectral class G main sequence star ...
... The Sun: close-up of a spectral class G main sequence star ...
Lecture Notes - NMSU Astronomy
... • Photosphere is dense enough to radiate light but not too dense so that photons can escape; thus it is where spectrum of star is emitted and where the absorption lines arise. • Chromosphere is active, hotter and lower density than photosphere is where emission occurs (hot, low density gas). This ...
... • Photosphere is dense enough to radiate light but not too dense so that photons can escape; thus it is where spectrum of star is emitted and where the absorption lines arise. • Chromosphere is active, hotter and lower density than photosphere is where emission occurs (hot, low density gas). This ...
Extreme Ultraviolet
... These images correspond to the layers of the Sun discussed in the Features of the Sun – 3D Sun lesson. ...
... These images correspond to the layers of the Sun discussed in the Features of the Sun – 3D Sun lesson. ...
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.