The sun, the earth, and the moon
... deep in Sun It extends far out into space Very powerful ...
... deep in Sun It extends far out into space Very powerful ...
Magnetic field induced transition rates in Ne- and Be
... Be-like In beryllium-like ions, the lowest lying excited state is the metastable state 2s2p 3 P0◦ which for isotopes with zero nuclear spin, only can decay through higher order transitions where the strongest one is the E1M1 two-photon transition. The lifetime of the 2s2p 3 P0 level has recently bee ...
... Be-like In beryllium-like ions, the lowest lying excited state is the metastable state 2s2p 3 P0◦ which for isotopes with zero nuclear spin, only can decay through higher order transitions where the strongest one is the E1M1 two-photon transition. The lifetime of the 2s2p 3 P0 level has recently bee ...
Homework 2 key: Radiation processes, Larmor formula
... surrounded by an ionized sphere shell of HII gas of radius 0.1 pc. Assuming the tempera the gas is 10,000K. (a) What fraction of the star's radiation is capable of ionizing neutral hydrogen? Plot the Planck function vs. frequency; indicate the region of ionizing photons with a vertical line (use the ...
... surrounded by an ionized sphere shell of HII gas of radius 0.1 pc. Assuming the tempera the gas is 10,000K. (a) What fraction of the star's radiation is capable of ionizing neutral hydrogen? Plot the Planck function vs. frequency; indicate the region of ionizing photons with a vertical line (use the ...
solar-activity-ref
... The core is the central region of the Sun and has a temperature of 15 million degrees. From here comes the star’s power; every second 564 million tons of hydrogen are fused, through thermonuclear reactions, to 560 million tons of helium. Hydrogen nuclei (protons) become helium nuclei at a rate of f ...
... The core is the central region of the Sun and has a temperature of 15 million degrees. From here comes the star’s power; every second 564 million tons of hydrogen are fused, through thermonuclear reactions, to 560 million tons of helium. Hydrogen nuclei (protons) become helium nuclei at a rate of f ...
THE SUN - OoCities
... with a very small number of molecules. As a result, there is no fixed surface. The surface viewed from Earth, called the photosphere, is the layer from which most of the radiation reaches us; the radiation from below is absorbed and reradiated, and the emission from overlying layers drops sharply, b ...
... with a very small number of molecules. As a result, there is no fixed surface. The surface viewed from Earth, called the photosphere, is the layer from which most of the radiation reaches us; the radiation from below is absorbed and reradiated, and the emission from overlying layers drops sharply, b ...
the planets - St John Brebeuf
... -release huge quantities of energy as light and heat through the process of thermonuclear fusion. ...
... -release huge quantities of energy as light and heat through the process of thermonuclear fusion. ...
the planets - St John Brebeuf
... -release huge quantities of energy as light and heat through the process of thermonuclear fusion. ...
... -release huge quantities of energy as light and heat through the process of thermonuclear fusion. ...
Our Star - U of L Class Index
... estimated that the Sun will “only” last another 5-6 billion years. ...
... estimated that the Sun will “only” last another 5-6 billion years. ...
Minor Members of the Solar System
... 23.4 Minor Members of the Solar System Asteroids: Microplanets An asteroid is a small, rocky body whose diameter can range from a few hundred kilometers to less than a kilometer. Most asteroids lie between the orbits of Mars and Jupiter. They have orbital periods of three to six years. ...
... 23.4 Minor Members of the Solar System Asteroids: Microplanets An asteroid is a small, rocky body whose diameter can range from a few hundred kilometers to less than a kilometer. Most asteroids lie between the orbits of Mars and Jupiter. They have orbital periods of three to six years. ...
Other Solar System Bodies
... that the moon spends part of its orbit inside the terrestrial magnetosphere, such that its interaction at these times is with the various magnetospheric fields and plasma populations discussed above, rather than the solar wind. Comets A comet nucleus is a relatively small body (~ a few 10’s of kilom ...
... that the moon spends part of its orbit inside the terrestrial magnetosphere, such that its interaction at these times is with the various magnetospheric fields and plasma populations discussed above, rather than the solar wind. Comets A comet nucleus is a relatively small body (~ a few 10’s of kilom ...
Lesson 2 | The Sun and Other Stars
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
MIT
... the Solar System extends out to 125,000 astronomical units (2 light years). • Since the nearest star is 4.22 light-years away, the Solar System size could extend almost half-way to the nearest star. • Astronomers think that the Sun's gravitational field dominates the gravitational forces of the othe ...
... the Solar System extends out to 125,000 astronomical units (2 light years). • Since the nearest star is 4.22 light-years away, the Solar System size could extend almost half-way to the nearest star. • Astronomers think that the Sun's gravitational field dominates the gravitational forces of the othe ...
No Slide Title - Harvard-Smithsonian Center for Astrophysics
... Ansatz: accretion stream impacts make waves • The impact of inhomogeneous “clumps” on the stellar surface can generate MHD waves that propagate out horizontally and enhance existing surface turbulence. ...
... Ansatz: accretion stream impacts make waves • The impact of inhomogeneous “clumps” on the stellar surface can generate MHD waves that propagate out horizontally and enhance existing surface turbulence. ...
Saturn`s icy satellites
... out by the moon should have had sufficient time (more than a corotation period) to fill in. However, for the penetrating particles a significant drop-out is observed, as in figure 1. This can be explained by considering the motion of electrons at these energies (MeV). They have a drift velocity grea ...
... out by the moon should have had sufficient time (more than a corotation period) to fill in. However, for the penetrating particles a significant drop-out is observed, as in figure 1. This can be explained by considering the motion of electrons at these energies (MeV). They have a drift velocity grea ...
Sun as an Energy Source
... • The sun releases a lot of ultraviolet energy each day. This energy can cause you to have a sunburn. ...
... • The sun releases a lot of ultraviolet energy each day. This energy can cause you to have a sunburn. ...
Chapter 3 Section 2 (pgs 68-73) the sun`s outer atmosphere – this is
... How long does the energy from the sun’s internal process take to reach the outer layers of the photosphere? It takes around a million years for the sun’s energy to reach the ...
... How long does the energy from the sun’s internal process take to reach the outer layers of the photosphere? It takes around a million years for the sun’s energy to reach the ...
ML_FoG_revisions_050509_v2 - Stanford Solar Observatories
... observations of the corona and nearSun acceleration regions Models to quantify the interaction of multiple acceleration mechanisms in key regions ...
... observations of the corona and nearSun acceleration regions Models to quantify the interaction of multiple acceleration mechanisms in key regions ...
Key words: Magnetic field, Sunspot, Polarisation, Stellar magnetism
... generate and sustain these magnetic fields. We now know that these magnetic fields in turn have a big impact on how stars behave throughout their lives. They play an important role in the complex processes of star formation. And at the other end of stellar lives, they are vital to explaining the biz ...
... generate and sustain these magnetic fields. We now know that these magnetic fields in turn have a big impact on how stars behave throughout their lives. They play an important role in the complex processes of star formation. And at the other end of stellar lives, they are vital to explaining the biz ...
Altair - the hottest `cool` star in X-rays
... 2.4 MK and its emission measure distribution (EMD) is dominated by rather cool plasma at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quie ...
... 2.4 MK and its emission measure distribution (EMD) is dominated by rather cool plasma at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quie ...
Chapter 27 Stars and Galaxies
... only seen during an eclipse huge cloud of gas that keeps the atomic particles from the surface from escaping into space ...
... only seen during an eclipse huge cloud of gas that keeps the atomic particles from the surface from escaping into space ...
Stellar Winds and Hydrodynamic Atmospheres
... 4. Additional forces: radiation Pressure driven winds can explain solar wind (note: that in reality you need magnetic fields to explain coronal heating) but… can winds of hot stars be driven by pressure only? ...
... 4. Additional forces: radiation Pressure driven winds can explain solar wind (note: that in reality you need magnetic fields to explain coronal heating) but… can winds of hot stars be driven by pressure only? ...
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.