The Sun
... • Gases in sun are in constant motion • Energy and gravity are main reason • Sun also rotates on its axis • Parts of the sun rotate at different speeds • Equator rotates faster than the poles – Equator ~25 days – Poles ~33 days ...
... • Gases in sun are in constant motion • Energy and gravity are main reason • Sun also rotates on its axis • Parts of the sun rotate at different speeds • Equator rotates faster than the poles – Equator ~25 days – Poles ~33 days ...
THE SUN - rgreenbergscience
... Two types of explosive solar events impact Earthlings most severely: SOLAR FLARE – small area above the solar surface suddenly roars to tens of millions of degrees, throwing off a surge of radiation that can cause communication blackouts, disable satellites, or kill a spacewalking astronaut CME ...
... Two types of explosive solar events impact Earthlings most severely: SOLAR FLARE – small area above the solar surface suddenly roars to tens of millions of degrees, throwing off a surge of radiation that can cause communication blackouts, disable satellites, or kill a spacewalking astronaut CME ...
Solar Cycle: Observations
... • Active regions appear as bipoles, which implies they are the tops of large Omega-shaped loops which have risen through the solar convection zone and emerged into the photosphere. • On average, bipoles are oriented nearly parallel to the E-W direction (Hale’s law 1919) indicating that the underlyin ...
... • Active regions appear as bipoles, which implies they are the tops of large Omega-shaped loops which have risen through the solar convection zone and emerged into the photosphere. • On average, bipoles are oriented nearly parallel to the E-W direction (Hale’s law 1919) indicating that the underlyin ...
Data Processing and Display Challenges for Solar Dynamics
... Sudden or sustained intrusion of chromospheric material well into the corona ...
... Sudden or sustained intrusion of chromospheric material well into the corona ...
solar photosphere and chromosphere
... “5-min oscillations” = acoustic waves in solar interior (resonator), evanescent in atmosphere • gravity waves do exist, very likely (e.g. Al et al [1]), generated by granular up- and downflows • acoustic waves: important (see e.g. Ulmschneider et al. 1991 [21], Ulmschneider et al. 2001 [22]), expect ...
... “5-min oscillations” = acoustic waves in solar interior (resonator), evanescent in atmosphere • gravity waves do exist, very likely (e.g. Al et al [1]), generated by granular up- and downflows • acoustic waves: important (see e.g. Ulmschneider et al. 1991 [21], Ulmschneider et al. 2001 [22]), expect ...
The Sun`s Magnetic Field Twisting Magnetic Fields PRS: Sunspots
... Calculating the Sun’s Luminosity Imagine completely surrounding the Sun with a sphere of radius 1 AU (1.5 x 1011 m), to capture all of its power output. Each square meter would receive 1300 Watts because the Sun’s radiation is the same in all directions. The Sun’s luminosity is therefore: ...
... Calculating the Sun’s Luminosity Imagine completely surrounding the Sun with a sphere of radius 1 AU (1.5 x 1011 m), to capture all of its power output. Each square meter would receive 1300 Watts because the Sun’s radiation is the same in all directions. The Sun’s luminosity is therefore: ...
THE SUN - Mother Teresa Regional School
... light from the photosphere and it no longer produces the glare that keeps you from seeing the sun’s faint, outer layers. The glow that you see during a solar eclipse is from the chromosphere, which is the middle layer of the sun. The Greek word “chroma” means color. So the chromosphere is the colo ...
... light from the photosphere and it no longer produces the glare that keeps you from seeing the sun’s faint, outer layers. The glow that you see during a solar eclipse is from the chromosphere, which is the middle layer of the sun. The Greek word “chroma” means color. So the chromosphere is the colo ...
Document
... particles (Ions) and the photons can be easily absorbed. This decreases the radiative conductivity and increases the temperature gradient. Where this occurs a volume of material moved upward will be warmer than its surroundings and will continue to rise further. These convective motions carry heat q ...
... particles (Ions) and the photons can be easily absorbed. This decreases the radiative conductivity and increases the temperature gradient. Where this occurs a volume of material moved upward will be warmer than its surroundings and will continue to rise further. These convective motions carry heat q ...
larger PDF file
... dim outer atmosphere? 7. Where does the solar wind come from? 8. What are sunspots? Why do they appear dark? 9. What is the connection between sunspots and the Sun’s magnetic field? 10. What causes eruptions in the Sun’s atmosphere? ...
... dim outer atmosphere? 7. Where does the solar wind come from? 8. What are sunspots? Why do they appear dark? 9. What is the connection between sunspots and the Sun’s magnetic field? 10. What causes eruptions in the Sun’s atmosphere? ...
The Sun to the Earth - Stanford Solar Center
... Sun’s surface boils up with heat, then crashes down ...
... Sun’s surface boils up with heat, then crashes down ...
Solar Interior 2 (Petrie)
... • is a process by which the magnetic field in an electrically conducting solar plasma is maintained against Ohmic dissipation. ...
... • is a process by which the magnetic field in an electrically conducting solar plasma is maintained against Ohmic dissipation. ...
Research - Clarion University
... Astronomy Research might accompany her to obtain more measurements. ...
... Astronomy Research might accompany her to obtain more measurements. ...
SolarActivity
... • The numbers and positions of sunspots vary in a cycle that lasts about 11 years. • Sunspots initially appear in groups about midway between the sun’s equator and poles. The number of sunspots increases over the next few until it reaches a peak of 100 of more sunspots. • After the peak, the number ...
... • The numbers and positions of sunspots vary in a cycle that lasts about 11 years. • Sunspots initially appear in groups about midway between the sun’s equator and poles. The number of sunspots increases over the next few until it reaches a peak of 100 of more sunspots. • After the peak, the number ...
The Sun PPT
... • A ball of gas, which can be generally thought of as having four “layers”: – Solar interior (core, radiation zone, convection zone) – visible surface (photosphere) • ‘visible’ ‘layer’ ...
... • A ball of gas, which can be generally thought of as having four “layers”: – Solar interior (core, radiation zone, convection zone) – visible surface (photosphere) • ‘visible’ ‘layer’ ...
The Sun
... become a red giant, then a white dwarf. Sun gets brighter with time. It has brightened 20-40% since the origin of the solar system. It brightens by about 0.7% every 100 million years. Variable features on the Sun (a small fraction of total energy) Sunspots, flares, corona (visible during eclipses) S ...
... become a red giant, then a white dwarf. Sun gets brighter with time. It has brightened 20-40% since the origin of the solar system. It brightens by about 0.7% every 100 million years. Variable features on the Sun (a small fraction of total energy) Sunspots, flares, corona (visible during eclipses) S ...
The Sun
... A coronal mass ejection is a much larger eruption that involves immense amounts of gas from the corona. Solar flares and coronal mass ejections ionize the atmosphere, create geomagnetic storms, disrupting electronics, radio communication, and endangering satellites and astronauts, even electrical po ...
... A coronal mass ejection is a much larger eruption that involves immense amounts of gas from the corona. Solar flares and coronal mass ejections ionize the atmosphere, create geomagnetic storms, disrupting electronics, radio communication, and endangering satellites and astronauts, even electrical po ...
The Sun is our local star.
... and composition and the way it produces energy. The Sun is far larger than any of the planets. It contains 99.9 percent of the mass of the entire solar system. For comparison, imagine that Earth had the mass of a sparrow; then the Sun would have the mass of ...
... and composition and the way it produces energy. The Sun is far larger than any of the planets. It contains 99.9 percent of the mass of the entire solar system. For comparison, imagine that Earth had the mass of a sparrow; then the Sun would have the mass of ...
Lecture 23 - Empyrean Quest Publishers
... Sunspots: Maximum every 11 years. 1. Sun's magn. pole also flips every 11 years. ...
... Sunspots: Maximum every 11 years. 1. Sun's magn. pole also flips every 11 years. ...
Sun Test Answers
... 28. The balance between the outward pressure of nuclear reactions in the core and inward pressure of gravity. a) stellar equilibrium b) hydromorpic equilibrium c) hydroponic equilibrium d) hydrostatic equilibrium 29. The second layer moving outward from the sun’s core. a) radiative zone b) chromosp ...
... 28. The balance between the outward pressure of nuclear reactions in the core and inward pressure of gravity. a) stellar equilibrium b) hydromorpic equilibrium c) hydroponic equilibrium d) hydrostatic equilibrium 29. The second layer moving outward from the sun’s core. a) radiative zone b) chromosp ...
The Sun (Nearest Star to us)
... An H-alpha filtergram reveals that the chromosphere contain complex structure which is invisible in normal ...
... An H-alpha filtergram reveals that the chromosphere contain complex structure which is invisible in normal ...
Worksheet 1
... G. The lower part of the Sun’s outer atmosphere that lies directly above the Sun’s visible surface H. The outflow of low-density, hot gas from the Sun’s upper atmosphere I. Tiny neutral particles with little or no mass and immense penetrating power J. A dark, cool region on the Sun’s visible surface ...
... G. The lower part of the Sun’s outer atmosphere that lies directly above the Sun’s visible surface H. The outflow of low-density, hot gas from the Sun’s upper atmosphere I. Tiny neutral particles with little or no mass and immense penetrating power J. A dark, cool region on the Sun’s visible surface ...
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.