RADIO RELICS AND MAGNETIC FIELDS IN GALAXY CLUSTERS
... the non-detection of inverse Compton emission from these sources. These limits will be combined with the constraints obtained from the analysis of the thickness of relics. The spatial profile of the magnetic field in GCs is still poorly known. In this respect constraints on magnetic fields at the di ...
... the non-detection of inverse Compton emission from these sources. These limits will be combined with the constraints obtained from the analysis of the thickness of relics. The spatial profile of the magnetic field in GCs is still poorly known. In this respect constraints on magnetic fields at the di ...
Shock structure and ion dynamics
... the ion distributions parallel and perpendicular to the interplanetary magnetic field (the mean magnetic field orientation is indicated by arrows) are shown for three different locations: downstream, at the ramp, and upstream of the bow shock. The dark blue shaded areas in the plot of the magnetic f ...
... the ion distributions parallel and perpendicular to the interplanetary magnetic field (the mean magnetic field orientation is indicated by arrows) are shown for three different locations: downstream, at the ramp, and upstream of the bow shock. The dark blue shaded areas in the plot of the magnetic f ...
Venus express: Highlights of the nominal mission - HAL
... slowly changes from orbit to orbit. Since the nominal mission lasted for two Venus sidereal days, all local times on tte planet were observed twice. About 30 UV bright stars were used by SPICAV for occultation studies of the upper atmosphere. Since the satellite orbit is fixed relative to motionless ...
... slowly changes from orbit to orbit. Since the nominal mission lasted for two Venus sidereal days, all local times on tte planet were observed twice. About 30 UV bright stars were used by SPICAV for occultation studies of the upper atmosphere. Since the satellite orbit is fixed relative to motionless ...
Spectral and Hydrodynamic Modeling of X-Ray Michael Rosenberg
... ionization parameter is the sole determinant of the amount of ionization that takes place as a result of photoionization versus collisional ionization [5]. Logically, a more luminous radiation source will generate more photoinization in a plasma, as will a source that is closer to the plasma. A plas ...
... ionization parameter is the sole determinant of the amount of ionization that takes place as a result of photoionization versus collisional ionization [5]. Logically, a more luminous radiation source will generate more photoinization in a plasma, as will a source that is closer to the plasma. A plas ...
Chandra Characterization of X-ray Emission in the Young F
... s-1. On the other hand, in the optical/IR, the system is very interesting. With two component stars of nearly identical age characterized by F spectral types in the Sco-Cen star-forming association, attention had been called to this system since its association with object IRAS 13037–4545 in the IRA ...
... s-1. On the other hand, in the optical/IR, the system is very interesting. With two component stars of nearly identical age characterized by F spectral types in the Sco-Cen star-forming association, attention had been called to this system since its association with object IRAS 13037–4545 in the IRA ...
Stellar Wind Mechanisms and Instabilities
... One of the great astronomical discoveries of the latter half of the past century was the realization that nearly all stars lose mass through a more or less continuous surface outflow called a “stellar wind”. While it was long apparent that stars could eject material in dramatic outburts like novae o ...
... One of the great astronomical discoveries of the latter half of the past century was the realization that nearly all stars lose mass through a more or less continuous surface outflow called a “stellar wind”. While it was long apparent that stars could eject material in dramatic outburts like novae o ...
Magnetic cycles of Sun-like stars with different levels of coronal and
... The HK-project of Mount Wilson observatory is one of the first and still the most outstanding program of observations of Sun-like stars (see Baliunas et al. 1995; Lockwood et al. 2007). One of the most important results of the HK-project was the discovery of ”11-yr” cycles of activity in Sun-like st ...
... The HK-project of Mount Wilson observatory is one of the first and still the most outstanding program of observations of Sun-like stars (see Baliunas et al. 1995; Lockwood et al. 2007). One of the most important results of the HK-project was the discovery of ”11-yr” cycles of activity in Sun-like st ...
Nonlinear shear-current dynamo and magnetic helicity transport in
... dynamical nonlinearity in the mean-field dynamo which determines the evolution of small-scale magnetic helicity, is of great importance due to the conservation law for the total (large and small scales) magnetic helicity in turbulence with very large magnetic Reynolds numbers (see, e.g. Kleeorin and ...
... dynamical nonlinearity in the mean-field dynamo which determines the evolution of small-scale magnetic helicity, is of great importance due to the conservation law for the total (large and small scales) magnetic helicity in turbulence with very large magnetic Reynolds numbers (see, e.g. Kleeorin and ...
CLUSTER MAGNETIC FIELDS - NED
... between the existence of a cluster radio halo and the existence of substructure in X-ray images of the hot cluster atmosphere, indicative of merging clusters, and a corresponding anticorrelation between cluster radio halos and clusters with relaxed morphologies, e.g., cooling flows (Govoni et al. 20 ...
... between the existence of a cluster radio halo and the existence of substructure in X-ray images of the hot cluster atmosphere, indicative of merging clusters, and a corresponding anticorrelation between cluster radio halos and clusters with relaxed morphologies, e.g., cooling flows (Govoni et al. 20 ...
Magnetic fluctuations and formation of large-scale inhomogeneous magnetic structures
... elements 共contrary to the descending fluid elements兲 are disconnected from one another. This causes a topological magnetic pumping effect, allowing downward transport of the mean horizontal magnetic field to the bottom of a cell, but impeding its upward return 关4,13,23兴. Turbulence may form inhomoge ...
... elements 共contrary to the descending fluid elements兲 are disconnected from one another. This causes a topological magnetic pumping effect, allowing downward transport of the mean horizontal magnetic field to the bottom of a cell, but impeding its upward return 关4,13,23兴. Turbulence may form inhomoge ...
Presolar Cloud Collapse and the Formation and Early Evolution of
... While precollapse clouds often have a complicated appearance, attempts have been made to approximate their shapes with simple geometries. Triaxial spheroids seem to be required in general (Kerton et al., 2003), although most lower-mass clouds appear to be more nearly oblate than prolate (Jones et al ...
... While precollapse clouds often have a complicated appearance, attempts have been made to approximate their shapes with simple geometries. Triaxial spheroids seem to be required in general (Kerton et al., 2003), although most lower-mass clouds appear to be more nearly oblate than prolate (Jones et al ...
bob_neutrino_EPS04
... problem. Neutrino interactions with matter are usually considered as non self-consistent single particle processes. We describe neutrino streaming instabilities within supernovæ plasmas, resulting in longitudinal and transverse waves using coupled kinetic equations for both neutrinos and plasma part ...
... problem. Neutrino interactions with matter are usually considered as non self-consistent single particle processes. We describe neutrino streaming instabilities within supernovæ plasmas, resulting in longitudinal and transverse waves using coupled kinetic equations for both neutrinos and plasma part ...
ultraviolet radiation in the solar system
... 5.3 Long–term Evolution of Ozone and UV Radiation . . 5.3.1 Oxygen and Ozone Variation . . . . . . . . . . 5.3.2 Early UV Surface Fluxes and the Origin of Life 5.4 Ozone and UV Fluxes in Planets around Other Stars . 5.5 The Ozone Hole . . . . . . . . . . . . . . . . . . . . . . 5.5.1 The Chlorofluoro ...
... 5.3 Long–term Evolution of Ozone and UV Radiation . . 5.3.1 Oxygen and Ozone Variation . . . . . . . . . . 5.3.2 Early UV Surface Fluxes and the Origin of Life 5.4 Ozone and UV Fluxes in Planets around Other Stars . 5.5 The Ozone Hole . . . . . . . . . . . . . . . . . . . . . . 5.5.1 The Chlorofluoro ...
the chandra deep field–north survey. xvii. evolution of
... characterize the X-ray emission from old high-latitude main-sequence Galactic stars. Our principal goal is to investigate the expected long-term decay of magnetic activity of late-type stars due to the gradual spin-down of stellar rotation from a magnetized stellar wind. Thirteen X-ray sources are a ...
... characterize the X-ray emission from old high-latitude main-sequence Galactic stars. Our principal goal is to investigate the expected long-term decay of magnetic activity of late-type stars due to the gradual spin-down of stellar rotation from a magnetized stellar wind. Thirteen X-ray sources are a ...
Conceptual Design of the International Axion Observatory (IAXO)
... of plasma photons into axions in the Coulomb field of charged particles via the generic aγγ vertex. The Primakoff solar axion flux peaks at 4.2 keV and exponentially decreases for higher energies [18]. This spectral shape is a robust prediction depending only on well known solar physics, while the o ...
... of plasma photons into axions in the Coulomb field of charged particles via the generic aγγ vertex. The Primakoff solar axion flux peaks at 4.2 keV and exponentially decreases for higher energies [18]. This spectral shape is a robust prediction depending only on well known solar physics, while the o ...
Full Paper - PDF - Armagh Observatory
... temperatures and in some cases the most significant magnetic field detection was obtained for a temperature somewhat hotter than that given by the photometric data. This occured several times for the hottest sample stars - this can be seen in Table 1. In the case of the cool Ap star EP UMa, a solar ...
... temperatures and in some cases the most significant magnetic field detection was obtained for a temperature somewhat hotter than that given by the photometric data. This occured several times for the hottest sample stars - this can be seen in Table 1. In the case of the cool Ap star EP UMa, a solar ...
Estimation of picked-up lunar ions for future compositional remote SIMS
... thought to be the cornerstone on which to build studies of the other celestial bodies. The lunar atmosphere is called ‘surface-bounded exosphere’ because it is thin enough to be regarded as an exosphere and it bounds on the solid surface differently from the Earth’s atmosphere-bounded exosphere. Rar ...
... thought to be the cornerstone on which to build studies of the other celestial bodies. The lunar atmosphere is called ‘surface-bounded exosphere’ because it is thin enough to be regarded as an exosphere and it bounds on the solid surface differently from the Earth’s atmosphere-bounded exosphere. Rar ...
as a PDF - Living Reviews in Solar Physics
... flares) are key factors in the formation and evolution of the planets and eventually the biosphere on Earth. The Sun is, like almost all cool stars, a “magnetic star” that produces magnetic fields through dynamo operation in the interior. These fields reach the surface where their presence is notice ...
... flares) are key factors in the formation and evolution of the planets and eventually the biosphere on Earth. The Sun is, like almost all cool stars, a “magnetic star” that produces magnetic fields through dynamo operation in the interior. These fields reach the surface where their presence is notice ...
X-Ray Properties of Young Stars and Stellar Clusters
... Star and planet formation is generally viewed as a hydrodynamic process involving gravitational collapse of interstellar material at low temperatures, 10–100 K in molecular cloud cores and 100–1500 K in protoplanetary disks. If thermodynamical equilibrium holds, this material should be neutral excep ...
... Star and planet formation is generally viewed as a hydrodynamic process involving gravitational collapse of interstellar material at low temperatures, 10–100 K in molecular cloud cores and 100–1500 K in protoplanetary disks. If thermodynamical equilibrium holds, this material should be neutral excep ...
Starspots: A Key to the Stellar Dynamo | SpringerLink
... sunspots, plages, network, etc. They further expand into the outer atmosphere and exhibit themselves as highly dynamic coronal loops. Thus, a detailed study of solar activity phenomena reveals the structure of underlying magnetic fields and provides valuable constraints for solar dynamo theory. Thes ...
... sunspots, plages, network, etc. They further expand into the outer atmosphere and exhibit themselves as highly dynamic coronal loops. Thus, a detailed study of solar activity phenomena reveals the structure of underlying magnetic fields and provides valuable constraints for solar dynamo theory. Thes ...
Cycles of magnetic activity in solar-type stars. The place of the Sun
... The evolution of active regions on the star on a time scale of about 10 years determines the cyclic activity similar to the Sun. For 111 HK-project stars the, periodograms were computed for each stellar record in order to search for activity cycles, see (Baliunas et al. 1995). The significance of the ...
... The evolution of active regions on the star on a time scale of about 10 years determines the cyclic activity similar to the Sun. For 111 HK-project stars the, periodograms were computed for each stellar record in order to search for activity cycles, see (Baliunas et al. 1995). The significance of the ...
Current status of turbulent dynamo theory
... can be dissipated by viscosity or by driving turbulent motions. Thus it becomes hard to make a convincing case for purely primordial magnetic fields, without any dynamo action, to explain observed cosmic magnetism. An exception is perhaps the space between clusters of galaxies, in particular the voi ...
... can be dissipated by viscosity or by driving turbulent motions. Thus it becomes hard to make a convincing case for purely primordial magnetic fields, without any dynamo action, to explain observed cosmic magnetism. An exception is perhaps the space between clusters of galaxies, in particular the voi ...
Decay and Amplification of Magnetic Fields
... enough, any arbitrarily complex magnetic field in the sun or stars will eventually end up looking dipolar. Conversely, a fluid flow acting as a dynamo in a sphere and trying to “beat” Ohmic dissipation can be expected to preferentially produce a magnetic field approximating diffusive eigenmodes of l ...
... enough, any arbitrarily complex magnetic field in the sun or stars will eventually end up looking dipolar. Conversely, a fluid flow acting as a dynamo in a sphere and trying to “beat” Ohmic dissipation can be expected to preferentially produce a magnetic field approximating diffusive eigenmodes of l ...
The Plasma Physics Processes that Drive Ring Current
... me that anything is possible with enough planning, creativity, organization and determination. ...
... me that anything is possible with enough planning, creativity, organization and determination. ...
web page pre-post test questions
... The following questions are part of a pretest survey we would like you to complete before you participate in the seminar on space weather. We intend to use the answers as a measure of your knowledge about the topics to be discussed in the seminar. You will be asked to retake this survey again after ...
... The following questions are part of a pretest survey we would like you to complete before you participate in the seminar on space weather. We intend to use the answers as a measure of your knowledge about the topics to be discussed in the seminar. You will be asked to retake this survey again after ...
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.