Andrés Muñoz-Jaramillo, PhD - Solar Cycle and Solar Dynamo
... 7. Helioseismic perspective of the solar dynamo. A. Muñoz-Jaramillo, P. C. H. Martens, & D. Nandy, ASP Conference Series, 478 (2013). 8. Using the dipolar and quadrupolar moments to improve solar cycle predictions based on the polar magnetic fields. A. Muñoz-Jaramillo, L. A. Balmaceda, & E. E. DeLuca ...
... 7. Helioseismic perspective of the solar dynamo. A. Muñoz-Jaramillo, P. C. H. Martens, & D. Nandy, ASP Conference Series, 478 (2013). 8. Using the dipolar and quadrupolar moments to improve solar cycle predictions based on the polar magnetic fields. A. Muñoz-Jaramillo, L. A. Balmaceda, & E. E. DeLuca ...
15. Our Star - Astrophysics & Space Science at UMBC
... • T = 1 – 5 x 104 K; depth = 2,500 km • A thin layer above the photosphere where most of the Sun’s UV light is emitted. • UV image of the Sun • light emitted from neutral Helium at 20,000 K ...
... • T = 1 – 5 x 104 K; depth = 2,500 km • A thin layer above the photosphere where most of the Sun’s UV light is emitted. • UV image of the Sun • light emitted from neutral Helium at 20,000 K ...
Chapter 8: Formation of the solar system 8.1 The Search for Origins
... methane (CH4) and ammonia (NH3) can solidify into ices at low temperatures (below about 150 K under the low pressure of the solar nebula) o Rock (0.4% of the solar nebula). Rocky material is gaseous at very high temperatures, but condenses into solid bits of mineral at temperatures between about 500 ...
... methane (CH4) and ammonia (NH3) can solidify into ices at low temperatures (below about 150 K under the low pressure of the solar nebula) o Rock (0.4% of the solar nebula). Rocky material is gaseous at very high temperatures, but condenses into solid bits of mineral at temperatures between about 500 ...
script
... • stellar wind is coupled to magnetic field lines and thus to stellar rotation • therefore, stellar wind takes away angular momentum and the stellar rotation is braked ...
... • stellar wind is coupled to magnetic field lines and thus to stellar rotation • therefore, stellar wind takes away angular momentum and the stellar rotation is braked ...
- 1 - Ulysses Observations of Solar Energetic Particles From the July
... particles at the Earth, both protons and electrons, started to increase almost immediately after the solar event at 1024UT on day 196, but energetic particles did not show up at Ulysses until several hours later and the increases were gradual. The peaks of the particle intensities at Ulysses were mu ...
... particles at the Earth, both protons and electrons, started to increase almost immediately after the solar event at 1024UT on day 196, but energetic particles did not show up at Ulysses until several hours later and the increases were gradual. The peaks of the particle intensities at Ulysses were mu ...
Document
... degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
... degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
How the Sun Shines - How It Began - A Time
... out the basic nuclear processes by which hydrogen is burned (fused) into helium in stellar interiors. Hydrogen is the most abundant constituent of the Sun and similar stars, and indeed the most abundant element in the Universe. Bethe described the results of his calculations in a 1939 paper entitled ...
... out the basic nuclear processes by which hydrogen is burned (fused) into helium in stellar interiors. Hydrogen is the most abundant constituent of the Sun and similar stars, and indeed the most abundant element in the Universe. Bethe described the results of his calculations in a 1939 paper entitled ...
On the electron temperature downstream of the solar wind
... of stochastic processes. In this paper we shall therefore not only consider shocks that conserve magnetic particle moments and thereby strongly heat particles, but also pay attention to the very different influence this has on electrons compared to ions, as we shall show. Another encouragement for p ...
... of stochastic processes. In this paper we shall therefore not only consider shocks that conserve magnetic particle moments and thereby strongly heat particles, but also pay attention to the very different influence this has on electrons compared to ions, as we shall show. Another encouragement for p ...
PPT
... Planets develop ‘feeding zones’ within the disk Eventually they exhaust the ‘food’ supply ...
... Planets develop ‘feeding zones’ within the disk Eventually they exhaust the ‘food’ supply ...
Sun - eyes-on-the-skies.org a Robotic Solar telescope
... convective motion in the sun. The magnetic field is formed below the sun's surface, and extends out into the sun's corona." ...
... convective motion in the sun. The magnetic field is formed below the sun's surface, and extends out into the sun's corona." ...
Plasma Seminar 4/23/07 "Negative Ion Plasmas"
... photosphere - what you see when you look at the sun about 400 km thick, cool ~ 4400K – 5800K, mostly H remarkably opaque at infrared and shorter wavelengths most H in ground state and thus does not contribute much to absorption need 13.6 eV (121.6 nm) to get H in first excited state 1939- about one ...
... photosphere - what you see when you look at the sun about 400 km thick, cool ~ 4400K – 5800K, mostly H remarkably opaque at infrared and shorter wavelengths most H in ground state and thus does not contribute much to absorption need 13.6 eV (121.6 nm) to get H in first excited state 1939- about one ...
Zeeman observations: Measuring magnetic fields in the atomic and
... In Astrophysics, the only way to directly measure magnetic fields is through polarimetric observations. In the case of interstellar medium (ISM) studies, the polarization can be detected from the following mechanisms (see [27] for a description of these mechanisms): synchrotron radiation, thermal du ...
... In Astrophysics, the only way to directly measure magnetic fields is through polarimetric observations. In the case of interstellar medium (ISM) studies, the polarization can be detected from the following mechanisms (see [27] for a description of these mechanisms): synchrotron radiation, thermal du ...
assessing the massive young sun hypothesis to solve the warm
... 1982). Assuming that each of these rates have remained constant over time, the total amount of mass lost by the Sun over its 4.56 Gyr history is only about 0.05% of the total solar mass. However, the physical processes that set the rate of mass loss due to solar wind and coronal mass ejections are p ...
... 1982). Assuming that each of these rates have remained constant over time, the total amount of mass lost by the Sun over its 4.56 Gyr history is only about 0.05% of the total solar mass. However, the physical processes that set the rate of mass loss due to solar wind and coronal mass ejections are p ...
The dramatic change of the fossil magnetic field of HD 190073
... Herbig Ae/Be stars plotted in a Hertzsprung-Russell diagram. The red square with error bars corresponds to HD 190073. The CESAM pre-MS evolutionary tracks for 1.5, 2, 3, 4, and 6 M⊙ (black full lines), 0.01, 0.1, 1 and 10 Myr isochrones (blue thin dashed lines), and the zero-age main-sequence (black ...
... Herbig Ae/Be stars plotted in a Hertzsprung-Russell diagram. The red square with error bars corresponds to HD 190073. The CESAM pre-MS evolutionary tracks for 1.5, 2, 3, 4, and 6 M⊙ (black full lines), 0.01, 0.1, 1 and 10 Myr isochrones (blue thin dashed lines), and the zero-age main-sequence (black ...
The Magnetic Universe
... Sun’s magnetism is responsible for a whole range of phenomena, such as sunspots, solar flares and coronal mass ejections. On average the Sun’s magnetism has about the same strength as the Earth’s, but in sunspots the magnetic field is about 1000 times higher. Ingenious techniques have allowed astron ...
... Sun’s magnetism is responsible for a whole range of phenomena, such as sunspots, solar flares and coronal mass ejections. On average the Sun’s magnetism has about the same strength as the Earth’s, but in sunspots the magnetic field is about 1000 times higher. Ingenious techniques have allowed astron ...
Brown spots mark impact sites of Comet Shoemaker–Levy on
... stars. Rare hyperbolic comets pass once through the inner Solar System before being thrown out into interstellar space along hyperbolic trajectories. Comets are distinguished from asteroids by the presence of a coma or a tail. However, extinct comets that have passed close to the Sun many times have ...
... stars. Rare hyperbolic comets pass once through the inner Solar System before being thrown out into interstellar space along hyperbolic trajectories. Comets are distinguished from asteroids by the presence of a coma or a tail. However, extinct comets that have passed close to the Sun many times have ...
THE LUYINOSITY VARIABILITY OF SOLAR
... The solar atmosphere harbors a broad range of nonthermal phenomena collectively called activity. On the global scale, this activity is responsible for the sharp temperature increase above the solar photosphere. On the local scale it produces a variety of discrete features, including the dark sunspot ...
... The solar atmosphere harbors a broad range of nonthermal phenomena collectively called activity. On the global scale, this activity is responsible for the sharp temperature increase above the solar photosphere. On the local scale it produces a variety of discrete features, including the dark sunspot ...
Magnetic field generation in weak-line T Tauri stars
... Magnetic fields play an essential role in stellar angular momentum evolution because the only way to extract angular momentum from a single star is magnetic coupling to the surrounding gas. This mechanism is particularly important in classical T Tauri systems (CTTS), where the stellar magnetic field ...
... Magnetic fields play an essential role in stellar angular momentum evolution because the only way to extract angular momentum from a single star is magnetic coupling to the surrounding gas. This mechanism is particularly important in classical T Tauri systems (CTTS), where the stellar magnetic field ...
Solar Observing Curriculum Guide
... We know now that sunspots are actually cooler portions of the Sun’s surface, caused by twisted magnetic lines penetrating the surface. The Sun has a magnetic field, just like the Earth, but as it rotates its magnetic field lines get twisted and tangled, like a rubber band. These eventually “snap”, ...
... We know now that sunspots are actually cooler portions of the Sun’s surface, caused by twisted magnetic lines penetrating the surface. The Sun has a magnetic field, just like the Earth, but as it rotates its magnetic field lines get twisted and tangled, like a rubber band. These eventually “snap”, ...
Life of the Sun—15 Oct 10/15/2010
... – For this to occur, the protons must collide vary fast to overcome the electric repulsion. – Repulsion force depends on the product of the charges ...
... – For this to occur, the protons must collide vary fast to overcome the electric repulsion. – Repulsion force depends on the product of the charges ...
Quantum Science for Energy Healers: A Practical Guide
... I have divided each week’s presentation into 6 sections which overlap and build in a cumulative manner each week. If you miss a session it is strongly recommended that you listen to the recording in order to make sure you are not “lost” in the next session. Although I will most certainly endeavo ...
... I have divided each week’s presentation into 6 sections which overlap and build in a cumulative manner each week. If you miss a session it is strongly recommended that you listen to the recording in order to make sure you are not “lost” in the next session. Although I will most certainly endeavo ...
Turbulent kinetic energy spectra of solar convection from New Solar
... Stein and Nordlund [26]. In the high-resolution simulation spectrum (12.5 km, red curve), the inertial and dissipative subranges, expected from turbulence theories (e.g. [8]), can be identified. Because of the strong density stratification, the spectral properties change with depth below the surface ...
... Stein and Nordlund [26]. In the high-resolution simulation spectrum (12.5 km, red curve), the inertial and dissipative subranges, expected from turbulence theories (e.g. [8]), can be identified. Because of the strong density stratification, the spectral properties change with depth below the surface ...
Full text - terrapub
... the center in the draped field geometry (E × B drift) giving rise to the plasma sheet ion population. Dubinin et al. (1993a) have shown that magnetic shear stresses (i.e. j × B force) might be important for the ion dynamics. Lichtenegger et al. (1995) tried to take into consideration this force by i ...
... the center in the draped field geometry (E × B drift) giving rise to the plasma sheet ion population. Dubinin et al. (1993a) have shown that magnetic shear stresses (i.e. j × B force) might be important for the ion dynamics. Lichtenegger et al. (1995) tried to take into consideration this force by i ...
Folie 1
... masses. Why, then, don’t we get such massive stars? There are a number of reasons, but one is that as the density increases hugely. 375k 3 ...
... masses. Why, then, don’t we get such massive stars? There are a number of reasons, but one is that as the density increases hugely. 375k 3 ...
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.