Accretion
... – mostly in X-rays • The magnetic field also transfers angular momentum out of the disk system ...
... – mostly in X-rays • The magnetic field also transfers angular momentum out of the disk system ...
Coupling from the Photosphere to the Chromosphere and the
... Observations of the solar atmosphere reveal a wealth of different phenomena, which occur over an extended range of different temporal and spatial scales. This is not surprising, considering the fact that already basic parameters such as gas density and temperature span many orders of magnitude, from ...
... Observations of the solar atmosphere reveal a wealth of different phenomena, which occur over an extended range of different temporal and spatial scales. This is not surprising, considering the fact that already basic parameters such as gas density and temperature span many orders of magnitude, from ...
Class 1 and 2 lecture slides (Solar System Formation)
... • As the nebula collapses, it forms a spinning disk (due to conservation of angular momentum) • The collapse releases gravitational energy, which heats the centre; this central hot portion forms a star • The outer, cooler particles suffer repeated collisions, building planet-sized bodies from dust g ...
... • As the nebula collapses, it forms a spinning disk (due to conservation of angular momentum) • The collapse releases gravitational energy, which heats the centre; this central hot portion forms a star • The outer, cooler particles suffer repeated collisions, building planet-sized bodies from dust g ...
The Solar System and its Place in the Galaxy
... Stars in the galactic disk have different characteristic velocities as a function of their stellar classification, and hence age. Low-mass, older stars, like the Sun, have relatively high random velocities and as a result c an move farther out of the galactic plane. Younger, more massive stars have ...
... Stars in the galactic disk have different characteristic velocities as a function of their stellar classification, and hence age. Low-mass, older stars, like the Sun, have relatively high random velocities and as a result c an move farther out of the galactic plane. Younger, more massive stars have ...
astro-ph/0502206 PDF
... most of the "smoke" from the nuclear furnace before it exits the flue. Hydrogen pouring from the Sun's surface is "smoke" from the furnace that powers the Sun. Each year 50 trillion metric tons of protons (Hydrogen ions) reach the Sun's surface and are flung out into space by the solar wind. This is ...
... most of the "smoke" from the nuclear furnace before it exits the flue. Hydrogen pouring from the Sun's surface is "smoke" from the furnace that powers the Sun. Each year 50 trillion metric tons of protons (Hydrogen ions) reach the Sun's surface and are flung out into space by the solar wind. This is ...
Research Essay “On the Origin of the Solar System”
... perpendicular to the axis of the ecliptic, this was confirmed spectroscopically. Herschel did not think that the retrograde motion of Uranus and its moons seriously compromised the general uniformity of motions in the Solar System; in 1806 he wrote that while they deviated from the motion of other ...
... perpendicular to the axis of the ecliptic, this was confirmed spectroscopically. Herschel did not think that the retrograde motion of Uranus and its moons seriously compromised the general uniformity of motions in the Solar System; in 1806 he wrote that while they deviated from the motion of other ...
Order-of-Magnitude Physics – Solution Set 4
... To avoid a singularity inside the sphere we have to set A = 0. Thus, for a sphere the only possible distribution is T = constant . Voilà, the white dwarf is isothermal. One may criticize the above approach for being too mathy and lacking physical insight (our lecturer is no fan). It’s also, strictl ...
... To avoid a singularity inside the sphere we have to set A = 0. Thus, for a sphere the only possible distribution is T = constant . Voilà, the white dwarf is isothermal. One may criticize the above approach for being too mathy and lacking physical insight (our lecturer is no fan). It’s also, strictl ...
Sun’s size vs. other stars some, smaller than others
... Filaments/Prominences This image is taken through a filter centered on a spectral line of Hydrogen (H , wavelength Å) that forms above the surface of the Sun Interesting new features seen on this image are filaments, dark string-like structures visible on the disk, and prominences, bright struc ...
... Filaments/Prominences This image is taken through a filter centered on a spectral line of Hydrogen (H , wavelength Å) that forms above the surface of the Sun Interesting new features seen on this image are filaments, dark string-like structures visible on the disk, and prominences, bright struc ...
Discrimination of exoplanetary and stellar radio flux
... density variations of a factor of two in the decimetric and centimetric wavelength range with 27 days period (due to the solar rotation). It is frequently circularly polarized. Noise storms During solar maximum, noise storms frequently occur (about 10% of the time). The typical duration is between a ...
... density variations of a factor of two in the decimetric and centimetric wavelength range with 27 days period (due to the solar rotation). It is frequently circularly polarized. Noise storms During solar maximum, noise storms frequently occur (about 10% of the time). The typical duration is between a ...
Chapter 6 Coupling between the ionosphere and the
... evening sector. It is connected to a downward field-aligned current in the south and to an upward field-aliged current in the north. In the morning sector the currents flow in opposite directions.q A downward field-aligned current flows at the polar cap boundary. It is divided into a current flowing ...
... evening sector. It is connected to a downward field-aligned current in the south and to an upward field-aliged current in the north. In the morning sector the currents flow in opposite directions.q A downward field-aligned current flows at the polar cap boundary. It is divided into a current flowing ...
ng - CAPCA
... • Filament separation leaves behind electron “driver”-- a second field generation mechanism: – Displaces plasma electrons – Plasma ions try to restore neutrality: space charge oscillation ...
... • Filament separation leaves behind electron “driver”-- a second field generation mechanism: – Displaces plasma electrons – Plasma ions try to restore neutrality: space charge oscillation ...
The Sun
... of light in the night sky. As stars go, however, the Sun is rather mediocre. It is classed as a yellow dwarf star, because because its visible radiation is most intense in the yellow-green portion of the spectrum. The Sun lies about 32,000 light years from the center of our galaxy and takes 225 mill ...
... of light in the night sky. As stars go, however, the Sun is rather mediocre. It is classed as a yellow dwarf star, because because its visible radiation is most intense in the yellow-green portion of the spectrum. The Sun lies about 32,000 light years from the center of our galaxy and takes 225 mill ...
Circumstellar interaction of supernovae and gamma-ray bursts
... Shock velocity of typical SNe are ~1000 times the velocity of the (red supergiant) wind. Hence, SNe observed few years after explosion can probe the history of the progenitor star thousands of years back. ...
... Shock velocity of typical SNe are ~1000 times the velocity of the (red supergiant) wind. Hence, SNe observed few years after explosion can probe the history of the progenitor star thousands of years back. ...
angular momentum in the solar system
... of space permeated by gases (called the solar wind) emanating from the sun to a distance of several hundred billion miles out; (3) at the location of the hypothetical "Oort cloud" of comets, believed to be about 2 light-years out. The Oort cloud is an evolutionary construct and has not been shown to ...
... of space permeated by gases (called the solar wind) emanating from the sun to a distance of several hundred billion miles out; (3) at the location of the hypothetical "Oort cloud" of comets, believed to be about 2 light-years out. The Oort cloud is an evolutionary construct and has not been shown to ...
Kinetic Studies of Nonrelativistic Young Supernova Remnant
... In the unmagnetized case, small-scale electrostatic and filamentation-like instabilities operate in parallel and heat the electrons. Eventually, strong fluctuations arise in the density of electrons and ions that lead to the formation of the double-shock structure. Thus, electron dynamics play an im ...
... In the unmagnetized case, small-scale electrostatic and filamentation-like instabilities operate in parallel and heat the electrons. Eventually, strong fluctuations arise in the density of electrons and ions that lead to the formation of the double-shock structure. Thus, electron dynamics play an im ...
Syllabus - Experimental Space Plasma Group
... shock waves: at planetary magnetospheres and comets, in the transition from high to low speed solar wind, at coronal mass ejections, and at the heliospheric boundary. Shock waves are known as very efficient particle accelerators in the cosmos. A wide variety of them can be studied insitu within the ...
... shock waves: at planetary magnetospheres and comets, in the transition from high to low speed solar wind, at coronal mass ejections, and at the heliospheric boundary. Shock waves are known as very efficient particle accelerators in the cosmos. A wide variety of them can be studied insitu within the ...
Slide 1 - Cloudfront.net
... the sun’s rotation results in magnetic fields. 2. The magnetic fields slow down convection and cause the sun to have cooler areas that can be up to 3,000°C cooler than surrounding regions. 3. These cooler areas of the sun appear darker than the warmer areas that surround them. 4. Cool, dark areas of ...
... the sun’s rotation results in magnetic fields. 2. The magnetic fields slow down convection and cause the sun to have cooler areas that can be up to 3,000°C cooler than surrounding regions. 3. These cooler areas of the sun appear darker than the warmer areas that surround them. 4. Cool, dark areas of ...
photosphere
... • Region of sun’s atmosphere just above the photosphere • Visible, UV, and X-ray lines ...
... • Region of sun’s atmosphere just above the photosphere • Visible, UV, and X-ray lines ...
An Even More Precise View of Aluminum-26 in the Solar Nebula
... injection of 26Al (and some other short-lived isotopes) from an active star that spewed material into interstellar space. For example, formation of the Sun might have been preceded by formation and rapid life (only 4 million years) of a massive star, 20 times more massive than the Sun. Astronomical ...
... injection of 26Al (and some other short-lived isotopes) from an active star that spewed material into interstellar space. For example, formation of the Sun might have been preceded by formation and rapid life (only 4 million years) of a massive star, 20 times more massive than the Sun. Astronomical ...
The Sun
... 4 x pi x (1 A.U.)2, or approximately 2.8 x 1023 m2. Multiplying the rate at which solar energy falls on each square meter of the sphere (i.e., the solar constant) by the total surface area of our imaginary sphere, we can determine the total rate at which energy leaves the Sun's surface. This quantit ...
... 4 x pi x (1 A.U.)2, or approximately 2.8 x 1023 m2. Multiplying the rate at which solar energy falls on each square meter of the sphere (i.e., the solar constant) by the total surface area of our imaginary sphere, we can determine the total rate at which energy leaves the Sun's surface. This quantit ...
The Sun
... 4 x pi x (1 A.U.)2, or approximately 2.8 x 1023 m2. Multiplying the rate at which solar energy falls on each square meter of the sphere (i.e., the solar constant) by the total surface area of our imaginary sphere, we can determine the total rate at which energy leaves the Sun's surface. This quantit ...
... 4 x pi x (1 A.U.)2, or approximately 2.8 x 1023 m2. Multiplying the rate at which solar energy falls on each square meter of the sphere (i.e., the solar constant) by the total surface area of our imaginary sphere, we can determine the total rate at which energy leaves the Sun's surface. This quantit ...
2 Solar magnetic fields. - High Altitude Observatory
... When asked to review this subject for this Winter School, I confess to being a little surprised, for there are many solar physicists more qualified than I, owing to their particular areas of specialization, who can discuss both observations and theory relating to solar magnetism. In recent years I h ...
... When asked to review this subject for this Winter School, I confess to being a little surprised, for there are many solar physicists more qualified than I, owing to their particular areas of specialization, who can discuss both observations and theory relating to solar magnetism. In recent years I h ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... The geometry and viewing angle are relatively well established for this star. There is a 45tilt between the rotation axis and both the magnetic axis and the direction of the Earth: we see a full range of viewing angles of the magnetosphere, and have Chandra observations for four of ...
... The geometry and viewing angle are relatively well established for this star. There is a 45tilt between the rotation axis and both the magnetic axis and the direction of the Earth: we see a full range of viewing angles of the magnetosphere, and have Chandra observations for four of ...
chapter5 - Homework Market
... • Yellow-hot is hotter than red-hot but not as hot as white-hot. • Different parts of the sun’s surface also glow slightly different colors depending on their temperatures. ...
... • Yellow-hot is hotter than red-hot but not as hot as white-hot. • Different parts of the sun’s surface also glow slightly different colors depending on their temperatures. ...
Sunstruck
... The areas of the Sun can be broken up into five broad categories; the atmosphere, the photosphere, the convective zone, the radiative zone, and the core. The atmosphere is broken up into sub regions like most of the categories of the Sun. The atmosphere varies wildly in temperature, from about 4,100 ...
... The areas of the Sun can be broken up into five broad categories; the atmosphere, the photosphere, the convective zone, the radiative zone, and the core. The atmosphere is broken up into sub regions like most of the categories of the Sun. The atmosphere varies wildly in temperature, from about 4,100 ...
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.