8.1 Radio Emission from Solar System objects
... emission arises from the corona and is a 2 million K blackbody. All this also means that the size of the sun measured at the different wavelengths will vary. The other two components are related to the sunspot activity on the sun. The slowly varying component is also thermal in origin and arises fro ...
... emission arises from the corona and is a 2 million K blackbody. All this also means that the size of the sun measured at the different wavelengths will vary. The other two components are related to the sunspot activity on the sun. The slowly varying component is also thermal in origin and arises fro ...
volume 86 part 3 - Australian ITER Forum
... exploration by means of rockets with ion thrusters; (ii) closer to earth, plasma physics is required for lightning studies, and communications (e.g. the propagation of electromagnetic waves in the ionosphere); and (iii) on earth, plasma physics is required for studies of MHD energy conversion, solid ...
... exploration by means of rockets with ion thrusters; (ii) closer to earth, plasma physics is required for lightning studies, and communications (e.g. the propagation of electromagnetic waves in the ionosphere); and (iii) on earth, plasma physics is required for studies of MHD energy conversion, solid ...
Discovery of a strong magnetic field in the rapidly rotating B2 Vn star
... We used the multiline analysis method of least-squares deconvolution (LSD; Donati et al. 1997) to produce mean Stokes I and V profiles from our spectra. These profiles are illustrated in Fig. 1. The details of the LSD method as applied to B stars are described by Silvester et al. (2009). The LSD lin ...
... We used the multiline analysis method of least-squares deconvolution (LSD; Donati et al. 1997) to produce mean Stokes I and V profiles from our spectra. These profiles are illustrated in Fig. 1. The details of the LSD method as applied to B stars are described by Silvester et al. (2009). The LSD lin ...
Discovery of a strong magnetic field in the rapidly rotating B2Vn star
... We used the multiline analysis method of least-squares deconvolution (LSD; Donati et al. 1997) to produce mean Stokes I and V profiles from our spectra. These profiles are illustrated in Fig. 1. The details of the LSD method as applied to B stars are described by Silvester et al. (2009). The LSD lin ...
... We used the multiline analysis method of least-squares deconvolution (LSD; Donati et al. 1997) to produce mean Stokes I and V profiles from our spectra. These profiles are illustrated in Fig. 1. The details of the LSD method as applied to B stars are described by Silvester et al. (2009). The LSD lin ...
Cluster mission and data analysis for the March 2001
... measurements of both large and small scale phenomena in the Earth’s magnetosphere are being obtained for the first time. It is a misfortune that the CIS instruments on Salsa and the HIA instrument on Tango are not operating properly, but nevertheless the analysis of the data sent by the Cluster sate ...
... measurements of both large and small scale phenomena in the Earth’s magnetosphere are being obtained for the first time. It is a misfortune that the CIS instruments on Salsa and the HIA instrument on Tango are not operating properly, but nevertheless the analysis of the data sent by the Cluster sate ...
release history and transport parameters of relativistic solar
... to the acceleration site), is essential to understand the mechanisms of SEP acceleration and release (e.g., McComas et al. 2007). The science goals of the next generation of spacecraft traveling close to the Sun (i.e. Solar Orbiter and Solar Probe Plus) include the exploration of the mechanisms that ...
... to the acceleration site), is essential to understand the mechanisms of SEP acceleration and release (e.g., McComas et al. 2007). The science goals of the next generation of spacecraft traveling close to the Sun (i.e. Solar Orbiter and Solar Probe Plus) include the exploration of the mechanisms that ...
Properties of small-scale magnetism of stellar
... Three-dimensional stellar atmospheric simulations including magnetic fields are still rare, unlike the case of solar MHD models. This state of affairs is certainly due to the fact that magnetic fields of granular spatial scale can nowadays be detected and measured in great detail and with high preci ...
... Three-dimensional stellar atmospheric simulations including magnetic fields are still rare, unlike the case of solar MHD models. This state of affairs is certainly due to the fact that magnetic fields of granular spatial scale can nowadays be detected and measured in great detail and with high preci ...
Neutrino Physics M. SPURIO University of Bologna and INFN
... of the core does not ignite nuclear fusion and the star is unable to thermodynamically support its outer envelope. As the surrounding matter falls inward under gravity, the temperature of the core rises and iron dissociates into α particles and nucleons. Electron capture on protons becomes heavil ...
... of the core does not ignite nuclear fusion and the star is unable to thermodynamically support its outer envelope. As the surrounding matter falls inward under gravity, the temperature of the core rises and iron dissociates into α particles and nucleons. Electron capture on protons becomes heavil ...
Discovery Of A Magnetic Field In The O9 Sub-Giant Star HD
... are unable to unambiguously determine the rotational period of HD 57682. However, using an upper limit on our inferred radius of 9.4 R and the inferred rotational broadening of 15 km s−1 , we estimate that the maximum (rigid) rotation period P rot is equal to about 31.5 d. The observed variations o ...
... are unable to unambiguously determine the rotational period of HD 57682. However, using an upper limit on our inferred radius of 9.4 R and the inferred rotational broadening of 15 km s−1 , we estimate that the maximum (rigid) rotation period P rot is equal to about 31.5 d. The observed variations o ...
Origin of the Solar System
... The embedded IR sources are regions with a large concentration of warm dust, which emit important quantities of thermal radiation. The source of energy that must feed this emission by keeping the dust grains warm enough is not seen, however, being obscured by the dust. With the aid of the IR emissio ...
... The embedded IR sources are regions with a large concentration of warm dust, which emit important quantities of thermal radiation. The source of energy that must feed this emission by keeping the dust grains warm enough is not seen, however, being obscured by the dust. With the aid of the IR emissio ...
“And God Said, Let There Be Lights in the Firmament of Heaven”
... intensity with the sunspot cycle which lasts roughly eleven years superimposed on this cyclic variation are short lived flares of more intense radiation occurring most frequently near the peak of the sunspot cycle from earth we see the effects of the x rays and particles as unusual displays of the n ...
... intensity with the sunspot cycle which lasts roughly eleven years superimposed on this cyclic variation are short lived flares of more intense radiation occurring most frequently near the peak of the sunspot cycle from earth we see the effects of the x rays and particles as unusual displays of the n ...
Propagation of cosmic rays in the solar wind
... galactic cosmic-ray intensity in antiphase with solar activity. This effect was first reportedby Forbu.sh[1954] and is now known to consistof a cyclic, elevenyear, solar-cycle variation upon which are superposedshorter-term irregular fluctuations (called Forbush decreases). This modulation is strong ...
... galactic cosmic-ray intensity in antiphase with solar activity. This effect was first reportedby Forbu.sh[1954] and is now known to consistof a cyclic, elevenyear, solar-cycle variation upon which are superposedshorter-term irregular fluctuations (called Forbush decreases). This modulation is strong ...
Computer Modeling the Line of Sight Column Densities of Polars
... Polars are a type of CV that has a strong magnetic field around 100 million times earths magnetic field. The plasma is not allowed to form an accretion disc because it follows the magnetic field lines. The stream takes a more direct path toward the white dwarf. The high speeds of the impacting parti ...
... Polars are a type of CV that has a strong magnetic field around 100 million times earths magnetic field. The plasma is not allowed to form an accretion disc because it follows the magnetic field lines. The stream takes a more direct path toward the white dwarf. The high speeds of the impacting parti ...
SOLAR ECLIPSES
... Total solar eclipses can be visible only from the Earth, because of certain weird coincidences within the ”Sun–Earth–Moon“ system. Thus, though the orbits of the Moon and Earth are elliptic, Sun and Moon’s apparent dimensions (noticed on the Earth) vary a little with time. The Moon is about 400 time ...
... Total solar eclipses can be visible only from the Earth, because of certain weird coincidences within the ”Sun–Earth–Moon“ system. Thus, though the orbits of the Moon and Earth are elliptic, Sun and Moon’s apparent dimensions (noticed on the Earth) vary a little with time. The Moon is about 400 time ...
croston
... • Magnetic field strengths: can’t be directly measured from radio synchrotron emission, so equipartition ( min. total energy) commonly assumed • Particle content: electron-positron or electron-proton? • Dynamics: – FRIs: missing pressure? – FRIIs: supersonic or not? ...
... • Magnetic field strengths: can’t be directly measured from radio synchrotron emission, so equipartition ( min. total energy) commonly assumed • Particle content: electron-positron or electron-proton? • Dynamics: – FRIs: missing pressure? – FRIIs: supersonic or not? ...
From the Sun`s atmosphere to the Earth`s atmosphere
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
... and coronal mass ejections (CMEs) – result from the presence of a dominant magnetic field. Eruptive events correspond to a liberation of magnetic energy stored in the solar corona. This energy is then converted into: – heating of the environment associated with UV/EUV and X beams; – particle acceler ...
Naming the 2008-2009 Minimum and Responding to Temperature Declines
... There would be significant areas of the world frozen then. And some of the world’s oceans would freeze as well with unclear effects. I have seen the Seine River in Paris during a rare 2003 snowstorm. There was some talk of a flood risk while there. With severe decreases in temperature related to sol ...
... There would be significant areas of the world frozen then. And some of the world’s oceans would freeze as well with unclear effects. I have seen the Seine River in Paris during a rare 2003 snowstorm. There was some talk of a flood risk while there. With severe decreases in temperature related to sol ...
P41
... arcade. As a results, we found that the flux rope is unstable to the kink mode instability, as the system approach to the lossof-equilibrium state. The 3D simulation shows that when the flux rope is long enough, it can escape from the arcade with almost constant speed after the accelerated launching ...
... arcade. As a results, we found that the flux rope is unstable to the kink mode instability, as the system approach to the lossof-equilibrium state. The 3D simulation shows that when the flux rope is long enough, it can escape from the arcade with almost constant speed after the accelerated launching ...
Document
... The flare-CME relationship Pre-SOHO conclusions “The flare and CME are both consequences of the same magnetic ‘disease’. They do not cause one another but are closely related. Their characteristics are the results of local conditions, and thus we may witness a spectrum of flare and CME properties w ...
... The flare-CME relationship Pre-SOHO conclusions “The flare and CME are both consequences of the same magnetic ‘disease’. They do not cause one another but are closely related. Their characteristics are the results of local conditions, and thus we may witness a spectrum of flare and CME properties w ...
The role of emerging bipoles in the formation of a sunspot penumbra
... small-scale flux emergence contributes to the growth of the sunspot. Zwaan (1992) reviews the observations of the sunspot formation. He shows that a sunspot forms by coalescence of pores. Here we present an alternative way of flux accumulation to form a sunspot. The small-scale bipolar loops that a ...
... small-scale flux emergence contributes to the growth of the sunspot. Zwaan (1992) reviews the observations of the sunspot formation. He shows that a sunspot forms by coalescence of pores. Here we present an alternative way of flux accumulation to form a sunspot. The small-scale bipolar loops that a ...
3. Solar Neutrinos
... Population I: heavy element rich star temperature in the core: up to 15.7 million K on the surface: ≈ 5,800K ...
... Population I: heavy element rich star temperature in the core: up to 15.7 million K on the surface: ≈ 5,800K ...
A breath of oxygen for the Sun
... allows to derive the 3D temperature structure and velocity field in the solar surface layers where the spectral lines are formed. The oxygen abundance they found are in much better agreement with helioseismology than the one by Asplund et al. (2004), but the oxygen abundance is still a bit too low t ...
... allows to derive the 3D temperature structure and velocity field in the solar surface layers where the spectral lines are formed. The oxygen abundance they found are in much better agreement with helioseismology than the one by Asplund et al. (2004), but the oxygen abundance is still a bit too low t ...
Atomic Emission Spectrometry
... Scanning instruments can detect multiple elements. Many lines detected so sometimes it is a quantitatively ...
... Scanning instruments can detect multiple elements. Many lines detected so sometimes it is a quantitatively ...
Plasma in ionosphere
... wavelength of 121.5 nanometer (nm) ionizing nitric oxide (NO). In addition, when the sun is active with 50 or more sunspots, hard X-rays (λ < 1 nm) ionize the air (N 2, O2). During the night time, cosmic rays produce a residual amount of ionization. Recombination is high in the D layer, thus the net ...
... wavelength of 121.5 nanometer (nm) ionizing nitric oxide (NO). In addition, when the sun is active with 50 or more sunspots, hard X-rays (λ < 1 nm) ionize the air (N 2, O2). During the night time, cosmic rays produce a residual amount of ionization. Recombination is high in the D layer, thus the net ...
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.