The Sun Times
... cooler than the rest of the sun’s surface. Solar flares are spectacular discharges of magnetic energy from the corona. These discharges send streams of protons and electrons outward into space. Solar flares can interrupt the communications network here on Earth. Solar winds are the result of gas exp ...
... cooler than the rest of the sun’s surface. Solar flares are spectacular discharges of magnetic energy from the corona. These discharges send streams of protons and electrons outward into space. Solar flares can interrupt the communications network here on Earth. Solar winds are the result of gas exp ...
PHY2505S Atmospheric Radiation & Remote Sensing Lecture 3 23
... Galileo’s 1610 observations showed a foreshortening of the images over some days from which he interpreted correctly that the blobs must be on the surface of the sun http://www.exploratorium.edu/sunspots http://science.msfc.nasa.gov/ssl/pad/solar/ ...
... Galileo’s 1610 observations showed a foreshortening of the images over some days from which he interpreted correctly that the blobs must be on the surface of the sun http://www.exploratorium.edu/sunspots http://science.msfc.nasa.gov/ssl/pad/solar/ ...
The Main Features of the X
... The Virgo Cluster: the cluster of galaxies at the center of the local supercluster Galactic Bulge: not well understood, but definitely consists of some component beyond the NPS LMC: a nearby dwarf irregular galaxy Vela/Puppis SNRs: Vela SNR ~ 1,500 ly away, 11,000 y old and 230 ly in diameter; where ...
... The Virgo Cluster: the cluster of galaxies at the center of the local supercluster Galactic Bulge: not well understood, but definitely consists of some component beyond the NPS LMC: a nearby dwarf irregular galaxy Vela/Puppis SNRs: Vela SNR ~ 1,500 ly away, 11,000 y old and 230 ly in diameter; where ...
Astronomy 2 Relativity and Gravitation
... Now the number of H atoms in corona NH is almost exactly equal to the mass of the corona divided by the mass of a proton, 1016/1.7x10-27 . Number of Fe atoms NFe = NH x abundance by number = NH x 7 x 10-5. Number of Fe atoms with electron in upper level 2 is NFe x 10-4. Thus A21 [4 (1.5 1011) ...
... Now the number of H atoms in corona NH is almost exactly equal to the mass of the corona divided by the mass of a proton, 1016/1.7x10-27 . Number of Fe atoms NFe = NH x abundance by number = NH x 7 x 10-5. Number of Fe atoms with electron in upper level 2 is NFe x 10-4. Thus A21 [4 (1.5 1011) ...
Stars II. Stellar Physics
... granulation. At the bright (high-T) center of each granule, gas is rising upward, and at the darker (lowerT) granule boundaries, it is sinking down again. The size of a granule seen from the Earth is typically 1”, corresponding to about 1000 km on the solar surface. There is also a larger scale conv ...
... granulation. At the bright (high-T) center of each granule, gas is rising upward, and at the darker (lowerT) granule boundaries, it is sinking down again. The size of a granule seen from the Earth is typically 1”, corresponding to about 1000 km on the solar surface. There is also a larger scale conv ...
Solar Radiation Objectives • explain how the Sun produces radiation
... photosphere(surface) of the Sun. Bright areas are the hot gas rising while the dark areas surrounding the bright spots are the cool gas falling back toward the centre. Each granule is between 1000km and 5000km in diameter, and only lasts a few minutes before moving or changing shape, due to the cons ...
... photosphere(surface) of the Sun. Bright areas are the hot gas rising while the dark areas surrounding the bright spots are the cool gas falling back toward the centre. Each granule is between 1000km and 5000km in diameter, and only lasts a few minutes before moving or changing shape, due to the cons ...
transparencies
... has observed the quiet Sun and the Moon Preliminary fluxes has been calculated with different methods We need more statistics for accurate spectra determinations Exciting physics expected: ...
... has observed the quiet Sun and the Moon Preliminary fluxes has been calculated with different methods We need more statistics for accurate spectra determinations Exciting physics expected: ...
The sun, yellow dwarf star at the heart of the solar system
... The sun and the rest of the solar system formed from a giant, rotating cloud of gas and dust called a solar nebula about 4.5 billion years ago. As the nebula collapsed because of its overwhelming gravity, it spun faster and flattened into a disk. Most of the material was pulled toward the center to f ...
... The sun and the rest of the solar system formed from a giant, rotating cloud of gas and dust called a solar nebula about 4.5 billion years ago. As the nebula collapsed because of its overwhelming gravity, it spun faster and flattened into a disk. Most of the material was pulled toward the center to f ...
BLynchTalk3
... Effects of CMEs September 1, 1859 More Recent CME effects Very Recent CME & Solar Flare effects October 29, 2003 ...
... Effects of CMEs September 1, 1859 More Recent CME effects Very Recent CME & Solar Flare effects October 29, 2003 ...
HIGHLIGHTS: this week in A&A Volume 462-3 (February II 2007)
... “The widest ultracool binary”, by J.A. Caballero A&A 462, p. L61 The leading scenario for the formation of brown dwarfs and very low-mass stars is that they are ejected from their formation region before they have a chance to accrete more mass, and it predicts that pairs of very low mass stars must ...
... “The widest ultracool binary”, by J.A. Caballero A&A 462, p. L61 The leading scenario for the formation of brown dwarfs and very low-mass stars is that they are ejected from their formation region before they have a chance to accrete more mass, and it predicts that pairs of very low mass stars must ...
Lecture 1 - X-ray and Observational Astronomy Group
... the chromospheric network, filaments, plages, prominences and spicules. ...
... the chromospheric network, filaments, plages, prominences and spicules. ...
lecture_1_mbu - X-ray and Observational Astronomy Group
... the chromospheric network, filaments, plages, prominences and spicules. ...
... the chromospheric network, filaments, plages, prominences and spicules. ...
ARTEMIS writeup
... slight variations, which could be related either to crustal fields, fluctuations due to the density depletion region, and/or variations of the solar wind IMF. This is contrasted with the right figure, which shows the Moon in the Earth's magnetotail plasma sheet. While there appear to be some density ...
... slight variations, which could be related either to crustal fields, fluctuations due to the density depletion region, and/or variations of the solar wind IMF. This is contrasted with the right figure, which shows the Moon in the Earth's magnetotail plasma sheet. While there appear to be some density ...
Solar wind`s oxygen content to be analyzed by UCSD chemists as
... "In this manner, we hope to unravel at a new level how all the planets and the solar system in general were created," he said. The Genesis mission is part of the NASA's Discovery program of lower-cost, highly focused scientific spacecraft. During its two-year excursion, the spacecraft will travel ab ...
... "In this manner, we hope to unravel at a new level how all the planets and the solar system in general were created," he said. The Genesis mission is part of the NASA's Discovery program of lower-cost, highly focused scientific spacecraft. During its two-year excursion, the spacecraft will travel ab ...
Lecture 7: The Sun - Department of Physics and Astronomy
... Magnetic Activity on the Sun Corona appears bright in X-ray photos in places where magnetic fields trap hot gas. Dark spots are coronal holes which eject fast solar wind. solar flares are explosions that send bursts of X-rays and charged particles into space. Energy of the flares can reach billion’ ...
... Magnetic Activity on the Sun Corona appears bright in X-ray photos in places where magnetic fields trap hot gas. Dark spots are coronal holes which eject fast solar wind. solar flares are explosions that send bursts of X-rays and charged particles into space. Energy of the flares can reach billion’ ...
Study Guide – Midterm 3
... • So far we have found several hundred planets circling other stars. Most are similar to Jupiter. • Why are we interested in finding other Earth-like planets? • How many have we found so far that definitely are habitable? • How does the “wobble technique” work? (what is the basic idea?) • What sort ...
... • So far we have found several hundred planets circling other stars. Most are similar to Jupiter. • Why are we interested in finding other Earth-like planets? • How many have we found so far that definitely are habitable? • How does the “wobble technique” work? (what is the basic idea?) • What sort ...
300 MHz - 3 GHz Yes, we`re interested
... • HI wrt young stars: HI outflows, and Zeeman splitting (also OH) - importance of magnetic fields vs. turbulence • Continuum: extragalactic - cosmic magnetism (Faraday rotation). Galactic magnetic fields, cluster magnetic fields, the cosmic web itself? ...
... • HI wrt young stars: HI outflows, and Zeeman splitting (also OH) - importance of magnetic fields vs. turbulence • Continuum: extragalactic - cosmic magnetism (Faraday rotation). Galactic magnetic fields, cluster magnetic fields, the cosmic web itself? ...
Astrophysics
... Solar eruptions are the most spectacular events in our solar system and are associated with many different features and signatures of energy release such as solar flares, coronal mass ejections, global waves, radio emission, accelerated particles and many more. Although each of these signatures prov ...
... Solar eruptions are the most spectacular events in our solar system and are associated with many different features and signatures of energy release such as solar flares, coronal mass ejections, global waves, radio emission, accelerated particles and many more. Although each of these signatures prov ...
PDF
... of solar coronal processes. Direct measurement of the coronal magnetic field is the most challenging problem in observational solar physics. A major progress here was reached with the deployment of the Coronal Multichannel Polarimeter (CoMP) (Tomczyk et al., 2007, 2008). In order to interpret such t ...
... of solar coronal processes. Direct measurement of the coronal magnetic field is the most challenging problem in observational solar physics. A major progress here was reached with the deployment of the Coronal Multichannel Polarimeter (CoMP) (Tomczyk et al., 2007, 2008). In order to interpret such t ...
Document
... loops) • Electrons accelerate down the magnetic field lines toward the lower atmosphere, producing microwave emission • Electrons collide with ions, producing hard x-rays, white light emission from chromosphere • Chromospheric plasma heated to coronal temperatures, hot plasma flows up into the coron ...
... loops) • Electrons accelerate down the magnetic field lines toward the lower atmosphere, producing microwave emission • Electrons collide with ions, producing hard x-rays, white light emission from chromosphere • Chromospheric plasma heated to coronal temperatures, hot plasma flows up into the coron ...
Part II: Ideas in Conflict.
... Sun’s magnetic field. These gases have been cooled, and are thus not as bright as the surface gases. When observed from above the Sun’s surface they appear darker than the rest of the surface. However, when observed from the side (above the edge of the Sun) they appear quite bright, and are called p ...
... Sun’s magnetic field. These gases have been cooled, and are thus not as bright as the surface gases. When observed from above the Sun’s surface they appear darker than the rest of the surface. However, when observed from the side (above the edge of the Sun) they appear quite bright, and are called p ...
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.