X-Ray Astronomy Poster_Final
... The first technology useful for research above the atmosphere was that of the V2 rockets available after World War II. With these, scientist revealed that Sun is a powerful source of UV and Xradiation. This is only because Sun is extremely close to us. But this discovery caused many scientist to los ...
... The first technology useful for research above the atmosphere was that of the V2 rockets available after World War II. With these, scientist revealed that Sun is a powerful source of UV and Xradiation. This is only because Sun is extremely close to us. But this discovery caused many scientist to los ...
Numerical modeling of plasma structures and turbulence transport in
... coronal holes become ever less pronounced towards solar maximum and eventually the predominant polarity of the northern and southern hemisphere changes sign. A magnetic- or Hale-cycle therefore takes about 22 years. In the more active phases around solar maximum the coronal field exhibits a more com ...
... coronal holes become ever less pronounced towards solar maximum and eventually the predominant polarity of the northern and southern hemisphere changes sign. A magnetic- or Hale-cycle therefore takes about 22 years. In the more active phases around solar maximum the coronal field exhibits a more com ...
Slides from Lecture19 - Department of Physics & Astronomy
... Determining Size of MW Galaxy • We have not always known that the diameter of our Galaxy is ~ 50 kpc (as illustrated in following slide) • For example, Herschel’s map of our Galaxy (1785) based on star counts … – Thin disk not much more than 1 kpc across – Sun approximately at center of disk ...
... Determining Size of MW Galaxy • We have not always known that the diameter of our Galaxy is ~ 50 kpc (as illustrated in following slide) • For example, Herschel’s map of our Galaxy (1785) based on star counts … – Thin disk not much more than 1 kpc across – Sun approximately at center of disk ...
Abstract: - Laboratory for Atmospheric and Space Physics
... expected for a near-equatorial interchange flux tube, in that the field interior to the event is larger ...
... expected for a near-equatorial interchange flux tube, in that the field interior to the event is larger ...
magnetospheres of the outer planets
... of mechanisms, including a cascade of elastic collisions resulting from penetration of the incident ion into the target and the excitation of target electrons to antibonding states (causing the ejection of target species). Chemical decomposition of the target can result. A schematic of sputtering an ...
... of mechanisms, including a cascade of elastic collisions resulting from penetration of the incident ion into the target and the excitation of target electrons to antibonding states (causing the ejection of target species). Chemical decomposition of the target can result. A schematic of sputtering an ...
Solar Weather Event Modelling and Prediction
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
Determination of the distance to the Andromeda Galaxy using variable stars U
... Flare activity in cool stars is a very common phenomenon. Flares in stars with spectral type earlier than M are observed mainly in UV and X-rays and optical flares (like the most energetic white light flares in the Sun; Hudson et al., 2006) are rare. However, in the less luminous low mass dM stars o ...
... Flare activity in cool stars is a very common phenomenon. Flares in stars with spectral type earlier than M are observed mainly in UV and X-rays and optical flares (like the most energetic white light flares in the Sun; Hudson et al., 2006) are rare. However, in the less luminous low mass dM stars o ...
M. Sc. Atmospheric Space
... The final assessment for theory courses will be in the form of written examination for the whole course. As the courses are for smaller credits and if a particular course is completed well before the term ends then teacher concerned need not wait for the end of term examination to conduct the final ...
... The final assessment for theory courses will be in the form of written examination for the whole course. As the courses are for smaller credits and if a particular course is completed well before the term ends then teacher concerned need not wait for the end of term examination to conduct the final ...
astronomy - Jiri Brezina Teaching
... relationship between heat and other forms of energy), ELECTROSTATICS & ELECTRODYNAMICS, MAGNETOSTATICS and MAGNETODYNAMICS. Modern physics is concerned with the behavior of matter and energy under extreme conditions or on the very large or very small scale. For example, atomic and nuclear physics st ...
... relationship between heat and other forms of energy), ELECTROSTATICS & ELECTRODYNAMICS, MAGNETOSTATICS and MAGNETODYNAMICS. Modern physics is concerned with the behavior of matter and energy under extreme conditions or on the very large or very small scale. For example, atomic and nuclear physics st ...
Nobel Prize in Physics 2002: Riccardo Giaconni
... Earth, as the atmosphere acts like an absorbing layer. It may sound strange since X-rays easily pass through our body (except the bones). Although the atmosphere is very tenuous compared to our body, the total thickness offered by it is much larger and X-rays suffer considerable absorption in it. Th ...
... Earth, as the atmosphere acts like an absorbing layer. It may sound strange since X-rays easily pass through our body (except the bones). Although the atmosphere is very tenuous compared to our body, the total thickness offered by it is much larger and X-rays suffer considerable absorption in it. Th ...
CHP 10
... c. using radio telescopes to observe the CO emission from the clouds. d. by looking for blue wispy regions near star clusters. e. by looking for the 21-cm radiation from hydrogen. 6. Coronal gas a. causes stars to look bluer than they normally would. b. causes the stars to twinkle. c. emits 21 cm ra ...
... c. using radio telescopes to observe the CO emission from the clouds. d. by looking for blue wispy regions near star clusters. e. by looking for the 21-cm radiation from hydrogen. 6. Coronal gas a. causes stars to look bluer than they normally would. b. causes the stars to twinkle. c. emits 21 cm ra ...
The Interstellar Medium
... c. using radio telescopes to observe the CO emission from the clouds. d. by looking for blue wispy regions near star clusters. e. by looking for the 21-cm radiation from hydrogen. 6. Coronal gas a. causes stars to look bluer than they normally would. b. causes the stars to twinkle. c. emits 21 cm ra ...
... c. using radio telescopes to observe the CO emission from the clouds. d. by looking for blue wispy regions near star clusters. e. by looking for the 21-cm radiation from hydrogen. 6. Coronal gas a. causes stars to look bluer than they normally would. b. causes the stars to twinkle. c. emits 21 cm ra ...
Fermi energy of electrons in neutron stars with strong magnetic field
... ergs, where m(3 P2 ) is the total mass of the superfluid region with anisotropic 3 P2 neutrons, and q is the ratio of the number of neutron in 3 P2 Cooper neutron pairs to the total number of neutron in the superfluid region (about 8.7%)[8]. According to the current x-ray observations (LX ∼ 1034 − 103 ...
... ergs, where m(3 P2 ) is the total mass of the superfluid region with anisotropic 3 P2 neutrons, and q is the ratio of the number of neutron in 3 P2 Cooper neutron pairs to the total number of neutron in the superfluid region (about 8.7%)[8]. According to the current x-ray observations (LX ∼ 1034 − 103 ...
How the Sun Shines - Department of Earth and Planetary Sciences
... impact of meteors falling onto its surface. Kelvin was forced by astronomical evidence to modify his hypothesis and he then argued that the primary source of the energy available to the sun was the gravitational energy of the primordial meteors from which it was formed. ...
... impact of meteors falling onto its surface. Kelvin was forced by astronomical evidence to modify his hypothesis and he then argued that the primary source of the energy available to the sun was the gravitational energy of the primordial meteors from which it was formed. ...
Winds of Main-Sequence Stars - Harvard
... The solar wind mass los rate • The sphere-averaged “M” isn’t usually considered by solar physicists! • Wang (1998, CS10) used empirical relationships between B-field, wind speed, and density to reconstruct M over two solar cycles. ...
... The solar wind mass los rate • The sphere-averaged “M” isn’t usually considered by solar physicists! • Wang (1998, CS10) used empirical relationships between B-field, wind speed, and density to reconstruct M over two solar cycles. ...
Fluid Instabilities
... hydrogen atom per cm3 at temperature 100K, we obtain a Jeans mass of about 8×1038 g. ...
... hydrogen atom per cm3 at temperature 100K, we obtain a Jeans mass of about 8×1038 g. ...
Stars PowerPoint
... • The Sun contains most of the mass in the solar system and is made up primarily of hydrogen and helium. • Astronomers learn about conditions inside the Sun by a combination of observation and theoretical models. • The Sun’s atmosphere consists of the photosphere, the chromosphere, and the corona. • ...
... • The Sun contains most of the mass in the solar system and is made up primarily of hydrogen and helium. • Astronomers learn about conditions inside the Sun by a combination of observation and theoretical models. • The Sun’s atmosphere consists of the photosphere, the chromosphere, and the corona. • ...
NEW PARTICLES FROM NUCLEAR REACTIONS IN THE SUN Max
... from the quiet sun are rare, this method will be sensitive to even relatively low fluxes of new particles. Furthermore, restriction to very light masses is not necessary if we consider production in nuclear reactions in the center of the star, where MeV energies are involved. In this note, then, we ...
... from the quiet sun are rare, this method will be sensitive to even relatively low fluxes of new particles. Furthermore, restriction to very light masses is not necessary if we consider production in nuclear reactions in the center of the star, where MeV energies are involved. In this note, then, we ...
The Sun - challenge for scientists
... ♦ Difference in speed between various areas on the Sun (SOHO/MDI) Spatial and temporal variation of the solar rotational flows speed ...
... ♦ Difference in speed between various areas on the Sun (SOHO/MDI) Spatial and temporal variation of the solar rotational flows speed ...
Observations
... configuration near dusk that is different from the other magnetospheric regions? Can the differences explain the dramatic dawn-dusk asymmetry in Jupiter’s aurora? How significant is the influence of Jupiter’s magnetosphere on the ...
... configuration near dusk that is different from the other magnetospheric regions? Can the differences explain the dramatic dawn-dusk asymmetry in Jupiter’s aurora? How significant is the influence of Jupiter’s magnetosphere on the ...
Efficiency of gas cooling and accretion at the disc-corona
... travels through the coronal gas and eventually falls back to the disc in a time-scale of ∼80–100 Myr. Fraternali & Binney (2006) built a dynamical model of fountain clouds that follow ballistic trajectories into the galactic halo and applied it to the extraplanar H I observations of two nearby galax ...
... travels through the coronal gas and eventually falls back to the disc in a time-scale of ∼80–100 Myr. Fraternali & Binney (2006) built a dynamical model of fountain clouds that follow ballistic trajectories into the galactic halo and applied it to the extraplanar H I observations of two nearby galax ...
VELOCITIES MEASURED IN SMALL-SCALE SOLAR MAGNETIC ELEMENTS Øystein Langangen, Mats Carlsson, and
... The spectra were obtained using the Swedish 1-m Solar Telescope (SST) (Scharmer et al. 2003a) together with the AO system (Scharmer et al. 2003b) and the TRI-Port Polarimetric EchelleLittrow ( TRIPPEL) spectrograph. As indicated by the name, the TRIPPEL spectrograph is a Littrow spectrograph with an ...
... The spectra were obtained using the Swedish 1-m Solar Telescope (SST) (Scharmer et al. 2003a) together with the AO system (Scharmer et al. 2003b) and the TRI-Port Polarimetric EchelleLittrow ( TRIPPEL) spectrograph. As indicated by the name, the TRIPPEL spectrograph is a Littrow spectrograph with an ...
FP11: DRAKE et al. - Astronomical Institute WWW Homepage
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
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.