A search for kilogauss magnetic fields in white dwarfs and hot
... to consider dynamo-induced magnetic fields in these systems, suggesting a non-fossil field origin in their magnetic white dwarf decendants. For these reasons, we are carrying out an observational program with the 6 m and 8 m Russian and European telescopes. The main goal of the project is the accumu ...
... to consider dynamo-induced magnetic fields in these systems, suggesting a non-fossil field origin in their magnetic white dwarf decendants. For these reasons, we are carrying out an observational program with the 6 m and 8 m Russian and European telescopes. The main goal of the project is the accumu ...
The High Resolution Camera CXC Newsletter
... IR excess due a a massive debris disk surrounding the star, made up from dust and cometary bodies. There are at least three scenarios for the origin of this X-ray emission: (i) a stellar corona, (ii) a boundary layer where mass is accreted from the disk or (iii) charge-exchange between the stellar w ...
... IR excess due a a massive debris disk surrounding the star, made up from dust and cometary bodies. There are at least three scenarios for the origin of this X-ray emission: (i) a stellar corona, (ii) a boundary layer where mass is accreted from the disk or (iii) charge-exchange between the stellar w ...
Solutions for Midterm
... moons around a Vegan Jupiter. We can either use the result from (d), or note from (c) that the fraction TJ4/L ~ TJ4/R*2T*4, so both imply scaling TJ with T*R*1/2 will preserve a ratio of unity ...
... moons around a Vegan Jupiter. We can either use the result from (d), or note from (c) that the fraction TJ4/L ~ TJ4/R*2T*4, so both imply scaling TJ with T*R*1/2 will preserve a ratio of unity ...
A self-consistent model of isolated neutron stars: the case of the X
... Bonazzola & Gourgoulhon (1996) for the fully non-linear case. For the general case with both poloidal and toroidal components, a similar non-linear (although Newtonian) analysis is presented in Tomimura & Eriguchi (2005) where Eq. (1) is generalized by considering µ = µ(x) as a general function of x ...
... Bonazzola & Gourgoulhon (1996) for the fully non-linear case. For the general case with both poloidal and toroidal components, a similar non-linear (although Newtonian) analysis is presented in Tomimura & Eriguchi (2005) where Eq. (1) is generalized by considering µ = µ(x) as a general function of x ...
The strongest magnetic fields in the universe: how strong can they
... electrodynamic range in the presence of the superstrong magnetic fields in the electro-weak and chromodynamic ranges. The problem remains that magnetic fields must have to be generated either at those small scales, or at much larger electrodynamic scales from where they collapse down to those small ...
... electrodynamic range in the presence of the superstrong magnetic fields in the electro-weak and chromodynamic ranges. The problem remains that magnetic fields must have to be generated either at those small scales, or at much larger electrodynamic scales from where they collapse down to those small ...
The strongest magnetic fields in the universe: how strong
... electrodynamic range in the presence of the superstrong magnetic fields in the electro-weak and chromodynamic ranges. The problem remains that magnetic fields must have to be generated either at those small scales, or at much larger electrodynamic scales from where they collapse down to those small ...
... electrodynamic range in the presence of the superstrong magnetic fields in the electro-weak and chromodynamic ranges. The problem remains that magnetic fields must have to be generated either at those small scales, or at much larger electrodynamic scales from where they collapse down to those small ...
The Time Evolution of Faculae and Plage
... of dark faculae and plage at the red and blue wavelengths decreases slightly whereas the bright faculae and plage show an increase. Decreasing numbers of dark faculae and plage act to increase irradiance because there are less of these structures inhibiting radiation. Similarly, the increase in brig ...
... of dark faculae and plage at the red and blue wavelengths decreases slightly whereas the bright faculae and plage show an increase. Decreasing numbers of dark faculae and plage act to increase irradiance because there are less of these structures inhibiting radiation. Similarly, the increase in brig ...
The energetics of relativistic magnetic reconnection: ion
... of strong motional electric fields, particles can gain energy there without necessarily turning around the whole island. Liu et al. (2011) report that in their relativistic pair plasma simulations, most particles are energized in this way. Jaroschek et al. (2004) also find that this scenario is impo ...
... of strong motional electric fields, particles can gain energy there without necessarily turning around the whole island. Liu et al. (2011) report that in their relativistic pair plasma simulations, most particles are energized in this way. Jaroschek et al. (2004) also find that this scenario is impo ...
Mars Express - The Scientific Investigations: ASPERA-3
... elliptical orbit, the power varies between ~90 and 720 W m–2. The corpuscular (particle flux) power from the solar wind is up to six orders of magnitude less than that. Yet, it is known that the solar wind plays an important, if not the major, role in the erosion of the martian atmosphere. The heati ...
... elliptical orbit, the power varies between ~90 and 720 W m–2. The corpuscular (particle flux) power from the solar wind is up to six orders of magnitude less than that. Yet, it is known that the solar wind plays an important, if not the major, role in the erosion of the martian atmosphere. The heati ...
Highlights in astronomical polarimetry
... Kramers-Heisenberg equation for Rayleigh scattering, but such kind of phenomena are impossible to observe in laboratory plasmas due to the very little absorption coefficient in the far wings. Similar phenomena were later found around the Na D lines ...
... Kramers-Heisenberg equation for Rayleigh scattering, but such kind of phenomena are impossible to observe in laboratory plasmas due to the very little absorption coefficient in the far wings. Similar phenomena were later found around the Na D lines ...
Low energy Electron Collision with Polar Molecules HCl and HBr in
... ionized gas and is usually considered to be a distinct phase of matter. “Ionized” in this case means that at least one of electron has been dissociated from a proportion of the atoms or molecules. The free electric charges make the plasma electrically conductive, so that it responds strongly to elec ...
... ionized gas and is usually considered to be a distinct phase of matter. “Ionized” in this case means that at least one of electron has been dissociated from a proportion of the atoms or molecules. The free electric charges make the plasma electrically conductive, so that it responds strongly to elec ...
Cosmic Rays 3 - zainab
... they are also affected by the interplanetary magnetic field embedded in the solar wind (the plasma of ions and electrons blowing from the solar corona at about 400 km/sec), and therefore have difficulty reaching the inner solar system. Spacecraft venturing out towards the boundary of the solar syste ...
... they are also affected by the interplanetary magnetic field embedded in the solar wind (the plasma of ions and electrons blowing from the solar corona at about 400 km/sec), and therefore have difficulty reaching the inner solar system. Spacecraft venturing out towards the boundary of the solar syste ...
1 kg coal - Lick Observatory
... Magnetic field stops convection where it comes up through the photosphere. Where field lines bunch up, get dark patches = sunspots Sunspots are cooler than the rest of the surface of the sun: 4000 K in the sunspots vs. 5800 K everywhere else. Why cooler? Convection is not carrying blobs of hot gas t ...
... Magnetic field stops convection where it comes up through the photosphere. Where field lines bunch up, get dark patches = sunspots Sunspots are cooler than the rest of the surface of the sun: 4000 K in the sunspots vs. 5800 K everywhere else. Why cooler? Convection is not carrying blobs of hot gas t ...
File
... fusion, and that this fusion occurs under the extreme temperatures and densities found deep in the Sun’s core. But exactly how does fusion occur and release energy? And how can we claim to know about something taking place out of sight in the Sun’s interior? Before we begin to answer these questions ...
... fusion, and that this fusion occurs under the extreme temperatures and densities found deep in the Sun’s core. But exactly how does fusion occur and release energy? And how can we claim to know about something taking place out of sight in the Sun’s interior? Before we begin to answer these questions ...
A new view on the solar wind interaction with the Moon | Geoscience
... of the backscattered hydrogen ENAs is Maxwellian (Fig. 3) and that the ENA characteristic energies are correlated with the solar wind velocity (rather than solar wind energy). This implied that the ENA emission is a momentum-driven process and the impacting solar wind protons experience multiple col ...
... of the backscattered hydrogen ENAs is Maxwellian (Fig. 3) and that the ENA characteristic energies are correlated with the solar wind velocity (rather than solar wind energy). This implied that the ENA emission is a momentum-driven process and the impacting solar wind protons experience multiple col ...
Observations and analysis of phase scintillation of spacecraft signal
... (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its speed. Fast winds are seen above coronal holes and can las ...
... (1991). The acceleration of the solar wind is attributed to the heating of the corona shell of the Sun. However, the physical processes of this phenomenon are not understood very well. One method of classifying the solar wind is based on its speed. Fast winds are seen above coronal holes and can las ...
Chapter 1 (Lectures 1
... • Normal atoms in fields of B < 50 kG (5T) are mostly described by the Zeeman effect. • Fine structure splitting varies greatly from one atomic configuration to another, so a few spectral lines may be in the Paschen-Back limit at much smaller fields than normal. This occurs when two fine structure l ...
... • Normal atoms in fields of B < 50 kG (5T) are mostly described by the Zeeman effect. • Fine structure splitting varies greatly from one atomic configuration to another, so a few spectral lines may be in the Paschen-Back limit at much smaller fields than normal. This occurs when two fine structure l ...
Proposal submitted to ISSI
... considered without a more general characterization of the observed planets. It is thus necessary to study the potential signatures of life in the context of the expected diversity of planets and the evolution or modification of their atmospheres due to the interaction with energetic particles (cosmi ...
... considered without a more general characterization of the observed planets. It is thus necessary to study the potential signatures of life in the context of the expected diversity of planets and the evolution or modification of their atmospheres due to the interaction with energetic particles (cosmi ...
Ten Years Of XMM-Newton: Scientific Achievements And Future Prospects Norbert Schartel
... connecting clusters of galaxies in form of low density gas with temperatures of 105
... connecting clusters of galaxies in form of low density gas with temperatures of 105
The Sun
... • The photosphere is the visible surface of the Sun. – This is the visible surface of the Sun because most of the light emitted by the Sun comes from this layer. – The average temperature of the photosphere is about ...
... • The photosphere is the visible surface of the Sun. – This is the visible surface of the Sun because most of the light emitted by the Sun comes from this layer. – The average temperature of the photosphere is about ...
Leverhulme lectures on stellar magnetism. 1. Overview
... 1012 G. Pulsing occurs because field axis is not parallel to rotation axis Nature of pulsed radio radiation is still not very clear, but seems to involve acceleration of electrons from surface which then spiral in strong circumstellar field lines. Energy comes from neutron star rotational energy Sho ...
... 1012 G. Pulsing occurs because field axis is not parallel to rotation axis Nature of pulsed radio radiation is still not very clear, but seems to involve acceleration of electrons from surface which then spiral in strong circumstellar field lines. Energy comes from neutron star rotational energy Sho ...
Current Systems in Planetary Magnetospheres and Ionospheres
... which is the distance at which the magnetic pressure of the planetary field on the sun-planet line (taking into account the additional effect of currents flowing on the magnetopause) balances the total solar wind pressure. In this formula R P represents the planetary radius. The different types of o ...
... which is the distance at which the magnetic pressure of the planetary field on the sun-planet line (taking into account the additional effect of currents flowing on the magnetopause) balances the total solar wind pressure. In this formula R P represents the planetary radius. The different types of o ...
–1– 1. Introduction for AY 219 The periodic table of the elements
... X-ray photons from very hot gas (thermal source) such as might be found in a cluster of galaxies, as well as from various non-thermal sources such as SN, accreting black holes in the nuclei of galaxies, various types of energetic binaies, etc. Discrete line transitions are of very high energy and re ...
... X-ray photons from very hot gas (thermal source) such as might be found in a cluster of galaxies, as well as from various non-thermal sources such as SN, accreting black holes in the nuclei of galaxies, various types of energetic binaies, etc. Discrete line transitions are of very high energy and re ...
space telescope imaging spectrograph survey of far
... and an absolute wavelength calibration compared with using the Chandra or XMM-Newton grating spectrometers to observe permitted transitions of the same ion stages in the kilovolt X-ray region. Fe xii 1242, 1349 (T 2 106 K) and Fe xxi 1354 (107 K) are well known from solar studies and have bee ...
... and an absolute wavelength calibration compared with using the Chandra or XMM-Newton grating spectrometers to observe permitted transitions of the same ion stages in the kilovolt X-ray region. Fe xii 1242, 1349 (T 2 106 K) and Fe xxi 1354 (107 K) are well known from solar studies and have bee ...
scholer-shocks-ii
... Move along shock surface with Alfven velocity given by magnetic field in overshoot ...
... Move along shock surface with Alfven velocity given by magnetic field in overshoot ...
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.