Special Session 11 From solar physics to astrophysics: the Sun as
... addition to the expected AGWs with upward energy and downward phase direction at frequencies below the Lamb frequency, there is also growing observational evidence for waves in the Sun’s atmosphere with downward energy and upward phase propagation, i.e. with the signature of downward propagating int ...
... addition to the expected AGWs with upward energy and downward phase direction at frequencies below the Lamb frequency, there is also growing observational evidence for waves in the Sun’s atmosphere with downward energy and upward phase propagation, i.e. with the signature of downward propagating int ...
Solar Wind Heliosphere
... emissions, traveling along interplanetary magnetic field lines and interacting with Earth’s magnetic field in near-Earth space. • Although the far-UV and X-ray emissions of the Sun are only a small percentage of its total output, they are responsible for creating the Earth’s ionosphere by ionization ...
... emissions, traveling along interplanetary magnetic field lines and interacting with Earth’s magnetic field in near-Earth space. • Although the far-UV and X-ray emissions of the Sun are only a small percentage of its total output, they are responsible for creating the Earth’s ionosphere by ionization ...
Unit 2 The Solar System Vocabulary Review
... A DISK OF MATTER THAT ENCIRCLES A PLANET AND THAT CONSISTS OF NUMEROUS PARTICLES IN ORBIT, WHICH RANGE IN SIZE FROM DUST GRAINS TO OBJECTS TENS OF METERS ACROSS ...
... A DISK OF MATTER THAT ENCIRCLES A PLANET AND THAT CONSISTS OF NUMEROUS PARTICLES IN ORBIT, WHICH RANGE IN SIZE FROM DUST GRAINS TO OBJECTS TENS OF METERS ACROSS ...
MHD Simulations of Line-Driven Hot-Star Winds
... models with same magnetic confinement parameter, *, but for three different stars: standard Pup, factor-ten lower mass loss rate Pup, and Q1 Ori C. Overall similarity: global configuration of field and flow depends mainly on the combination of stellar, wind, and magnetic properties that define ...
... models with same magnetic confinement parameter, *, but for three different stars: standard Pup, factor-ten lower mass loss rate Pup, and Q1 Ori C. Overall similarity: global configuration of field and flow depends mainly on the combination of stellar, wind, and magnetic properties that define ...
8.2 Solar Nebula Theory and the Sun
... • Radiative zone: 86% of sun’s energy radiates outward from core • Convective zone: outer layer transfers energy in convection currents back in towards sun • Photosphere: “surface” layer of sun ...
... • Radiative zone: 86% of sun’s energy radiates outward from core • Convective zone: outer layer transfers energy in convection currents back in towards sun • Photosphere: “surface” layer of sun ...
Earth`s magnetic field – what is it good for?
... How does this work? When either or both magnetic fields is weak (as when the Sun sported fewer sunspots during the Maunder Minimum), more cosmic rays reach our atmosphere, creating muons (heavy electrons) that produce the condensation nuclei for cloud formation. An increase in cloudiness results in ...
... How does this work? When either or both magnetic fields is weak (as when the Sun sported fewer sunspots during the Maunder Minimum), more cosmic rays reach our atmosphere, creating muons (heavy electrons) that produce the condensation nuclei for cloud formation. An increase in cloudiness results in ...
Summary of Cool Stars 13 - JILA - University of Colorado Boulder
... coronal abundances? • Marc Audard: Important to compare coronal abundances with measured stellar photospheric abundances. Abundance changes must occur in the chromosphere where FIP <10 eV elements are ionized, but the physical process not well understood. • David Garcia-Alvarez: Existance of very ho ...
... coronal abundances? • Marc Audard: Important to compare coronal abundances with measured stellar photospheric abundances. Abundance changes must occur in the chromosphere where FIP <10 eV elements are ionized, but the physical process not well understood. • David Garcia-Alvarez: Existance of very ho ...
Can you write numbers in scientific notation
... Do you understand how the star formation process begins? How well you understand what processes are going on during the protostar stage of a star’s life? What needs to happen for a protostar to become a main sequence star? What are the properties of a main sequence star? How does a star’s mass effec ...
... Do you understand how the star formation process begins? How well you understand what processes are going on during the protostar stage of a star’s life? What needs to happen for a protostar to become a main sequence star? What are the properties of a main sequence star? How does a star’s mass effec ...
Chapter 5 Lesson 1: The Sun
... • What is the largest object in our solar system? • An object in the solar system that produces heat and light is a _______________. • What causes energy to be released inside the sun? • How would earth be affected if the sun stopped producing energy? • Why are the planets not stars? • Why do you th ...
... • What is the largest object in our solar system? • An object in the solar system that produces heat and light is a _______________. • What causes energy to be released inside the sun? • How would earth be affected if the sun stopped producing energy? • Why are the planets not stars? • Why do you th ...
APSU_1000_35 Liberal Arts Univ. Life
... The temperature from the photosphere up A) Decreases uniformly as you get higher above the photosphere. B) Increases uniformly as you get higher above the photosphere. C) Increases slowly in the chromosphere then jumps rapidly in the corona. D) Decreases slowly in the chromosphere then jumps rapidly ...
... The temperature from the photosphere up A) Decreases uniformly as you get higher above the photosphere. B) Increases uniformly as you get higher above the photosphere. C) Increases slowly in the chromosphere then jumps rapidly in the corona. D) Decreases slowly in the chromosphere then jumps rapidly ...
MHD Simulations of Line-Driven Hot-Star Winds
... models with same magnetic confinement parameter, *, but for three different stars: standard Pup, factor-ten lower mass loss rate Pup, and Q1 Ori C. Overall similarity: global configuration of field and flow depends mainly on the combination of stellar, wind, and magnetic properties that define ...
... models with same magnetic confinement parameter, *, but for three different stars: standard Pup, factor-ten lower mass loss rate Pup, and Q1 Ori C. Overall similarity: global configuration of field and flow depends mainly on the combination of stellar, wind, and magnetic properties that define ...
Layers of the Sun
... also very thin, only extending into space for millions of kilometers. Scientists are still trying to figure out why it is hotter than other parts of the Sun. This is a big mystery… Sometimes when the Sun is very active, the hot gases shooting out of the Sun are so powerful that they blow away from t ...
... also very thin, only extending into space for millions of kilometers. Scientists are still trying to figure out why it is hotter than other parts of the Sun. This is a big mystery… Sometimes when the Sun is very active, the hot gases shooting out of the Sun are so powerful that they blow away from t ...
Fusion in the Sun
... They are caused by strong magnetic fields that slow down convection so less energy is released. ...
... They are caused by strong magnetic fields that slow down convection so less energy is released. ...
Chapter 8
... The sun is the source of light and warmth in our solar system, so it is a natural object of human curiosity. It is also the star that is most easily visible from Earth. The interaction of light and matter, which you studied in Chapter 7, can reveal the secrets of the sun and introduce you to the sta ...
... The sun is the source of light and warmth in our solar system, so it is a natural object of human curiosity. It is also the star that is most easily visible from Earth. The interaction of light and matter, which you studied in Chapter 7, can reveal the secrets of the sun and introduce you to the sta ...
Chapter 3 - BITS Pilani
... Solar wind means Sun is not able to hold on to some of its mass --- charged particles escape Sun’s gravity and fly away from Sun. Considering again a balance between pressure and gravity, if the ...
... Solar wind means Sun is not able to hold on to some of its mass --- charged particles escape Sun’s gravity and fly away from Sun. Considering again a balance between pressure and gravity, if the ...
Space is Big…
... You just won’t believe how vastly, hugely, mindbogglingly big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that’s just peanuts to space.” ...
... You just won’t believe how vastly, hugely, mindbogglingly big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that’s just peanuts to space.” ...
Summary of work for Period 1 - Research Center for Astronomy
... • Establishment of a reliable calculation of magnetic connectivity in the solar atmosphere by using only the observed photospheric vertical magnetic‐field component. • Preliminary development of a novel, operational NLFF magnetic field extrapolation method that does not ...
... • Establishment of a reliable calculation of magnetic connectivity in the solar atmosphere by using only the observed photospheric vertical magnetic‐field component. • Preliminary development of a novel, operational NLFF magnetic field extrapolation method that does not ...
Space Weather User Needs Related to Solar Observations
... (depending on the type of event). • Free-space/near-Earth measurements or reliable models of higherenergy (~100-1000MeV) proton/ion spectra. • ACE type data/models on mission termination. • Be able to predict magnitude / duration / characteristics of SPE from information received at onset of event – ...
... (depending on the type of event). • Free-space/near-Earth measurements or reliable models of higherenergy (~100-1000MeV) proton/ion spectra. • ACE type data/models on mission termination. • Be able to predict magnitude / duration / characteristics of SPE from information received at onset of event – ...
The Sun`s Size, Heat, and Structure
... famous equation E ⫽ mc2 (energy is equal to mass times the speed of light squared). This equation expresses that matter can be converted into energy, which is what happens during fusion. A star is a place of intense heat and pressure—so intense that atoms are torn apart into their component nuclei a ...
... famous equation E ⫽ mc2 (energy is equal to mass times the speed of light squared). This equation expresses that matter can be converted into energy, which is what happens during fusion. A star is a place of intense heat and pressure—so intense that atoms are torn apart into their component nuclei a ...
Document
... After this, my salary was also kept back from me, and scholars of most eminent rank were violently kept from me, contrary to their own wills, the masters persuading them that their brains were not able to endure it." ...
... After this, my salary was also kept back from me, and scholars of most eminent rank were violently kept from me, contrary to their own wills, the masters persuading them that their brains were not able to endure it." ...
Astro 101-001 Summer 2013 (Howard) Assignment #3 Due: Wed
... surrounding areas of the Sun; (d) They are solid bodies floating on the surface of the Sun; (e) They are associated with areas of very low magnetic fields. 6. The primary source of the Sun's energy is: (a) oxidation of carbon in the core; (b) gravitational collapse of the helium coreward; (c) dark e ...
... surrounding areas of the Sun; (d) They are solid bodies floating on the surface of the Sun; (e) They are associated with areas of very low magnetic fields. 6. The primary source of the Sun's energy is: (a) oxidation of carbon in the core; (b) gravitational collapse of the helium coreward; (c) dark e ...
Solar Wind - International School of Space Science
... • Stereo data show ions and electrons becomes field-aligned close to the Sun. • The picture of SW based on frozen in field model needs to be re-examined! • We have applied the Earth’s auroral model to solar coronal atmosphere. are suggesting that SW field-aligned beams are produced by E||. ...
... • Stereo data show ions and electrons becomes field-aligned close to the Sun. • The picture of SW based on frozen in field model needs to be re-examined! • We have applied the Earth’s auroral model to solar coronal atmosphere. are suggesting that SW field-aligned beams are produced by E||. ...
Ch 22 The Sun & It’s Solar System
... Colored Red by glowing Hydrogen Radiates mostly X-rays & UV Area of prominences ...
... Colored Red by glowing Hydrogen Radiates mostly X-rays & UV Area of prominences ...
photosphere - Blackboard
... (1 million oK) gas • Coronal gas is heated through motions of magnetic fields anchored in the photosphere below (“magnetic carpet”) ...
... (1 million oK) gas • Coronal gas is heated through motions of magnetic fields anchored in the photosphere below (“magnetic carpet”) ...
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.