Pattern Recognition in Physics The complex planetary
... Sun is just a fraction of millimeter (Scafetta, 2012c). Therefore, tidal forcing appears too small to effect the Sun. However, as discussed above, the magnitude of the tidal elongation induced by the Earth’s gravity on Venus is also a fraction of millimeter. Thus, if the Earth’s gravity or some othe ...
... Sun is just a fraction of millimeter (Scafetta, 2012c). Therefore, tidal forcing appears too small to effect the Sun. However, as discussed above, the magnitude of the tidal elongation induced by the Earth’s gravity on Venus is also a fraction of millimeter. Thus, if the Earth’s gravity or some othe ...
Synchrotron and inverse-Compton emission from
... Jamrozy et al. 2008). If N(E) is initially a power law in energy as a result of the acceleration process, then at some later time t > 0 we expect N(E) to have a characteristic form depending on t. Since for synchrotron radiation the characteristic time-scale for energy losses goes as 1/E, N(E) at t ...
... Jamrozy et al. 2008). If N(E) is initially a power law in energy as a result of the acceleration process, then at some later time t > 0 we expect N(E) to have a characteristic form depending on t. Since for synchrotron radiation the characteristic time-scale for energy losses goes as 1/E, N(E) at t ...
Spatially resolved STIS Spectroscopy of Betelgeuse: Evidence for
... shown in Fig. 1. In the upper left panel of Fig. 3 its (GHRS) disk-integrated selfabsorption core of 1992 September reveals a blue-shift of ∼10 km s−1 . The red emission component exceeds the blue one, while the latter becomes stronger in 1998 September. We determine the chromospheric velocity struc ...
... shown in Fig. 1. In the upper left panel of Fig. 3 its (GHRS) disk-integrated selfabsorption core of 1992 September reveals a blue-shift of ∼10 km s−1 . The red emission component exceeds the blue one, while the latter becomes stronger in 1998 September. We determine the chromospheric velocity struc ...
Chapter 3 (Lectures 7
... in general, such fields rather rapidly evolve to a configuration in which there is both a “poloidal” (dipole-like) component, which emerges from the surface, and a comparably strong toroidal component (a sort of large tube of magnetic flux wrapped around some of the dipolar field lines deep inside t ...
... in general, such fields rather rapidly evolve to a configuration in which there is both a “poloidal” (dipole-like) component, which emerges from the surface, and a comparably strong toroidal component (a sort of large tube of magnetic flux wrapped around some of the dipolar field lines deep inside t ...
the fragmentation of magnetized, massive star-forming
... that a ∼40 AU Keplerian disk is able to form in our simulations, despite the braking effect caused by the strong magnetic field. Key words: ISM: clouds – magnetohydrodynamics (MHD) – radiative transfer – stars: formation – stars: luminosity function, mass function – turbulence Online-only material: ...
... that a ∼40 AU Keplerian disk is able to form in our simulations, despite the braking effect caused by the strong magnetic field. Key words: ISM: clouds – magnetohydrodynamics (MHD) – radiative transfer – stars: formation – stars: luminosity function, mass function – turbulence Online-only material: ...
Optical Spectroscopy of a Flare on Barnard`s Star
... present in F1 and is unmeasurable in F2. The He I lines are broad lines and the contamination of the narrow I2 lines in this region does not affect the detection of the broad He feature. Because we see the He feature in F1 and not F2, the flare was probably quite energetic but the impulsive heating ...
... present in F1 and is unmeasurable in F2. The He I lines are broad lines and the contamination of the narrow I2 lines in this region does not affect the detection of the broad He feature. Because we see the He feature in F1 and not F2, the flare was probably quite energetic but the impulsive heating ...
Borexino …..bla bla bla
... it is possible to obtain a spectrum energy and hence to distinguish the different neutrino contribution. Furthermore, thank to the fact that the scattered electron conserves the direction of the impinging neutrino, it is possible to infer the direction of the origin of the incoming neutrino and henc ...
... it is possible to obtain a spectrum energy and hence to distinguish the different neutrino contribution. Furthermore, thank to the fact that the scattered electron conserves the direction of the impinging neutrino, it is possible to infer the direction of the origin of the incoming neutrino and henc ...
PreAP Waves and Sound
... Energy produced by the oscillation of an electric charge which produces electric and magnetic fields ...
... Energy produced by the oscillation of an electric charge which produces electric and magnetic fields ...
Estimation of the Sun`s rotation through the tracking of Sunspots
... Granulation is a blotchy pattern on the sun that forms and disappears over several minutes. Sunspots are regions in the photosphere that appear dark. This is because they are cooler than the rest of the Suns lower atmosphere. This is because the magnetic field of the sun disrupts the surface and sl ...
... Granulation is a blotchy pattern on the sun that forms and disappears over several minutes. Sunspots are regions in the photosphere that appear dark. This is because they are cooler than the rest of the Suns lower atmosphere. This is because the magnetic field of the sun disrupts the surface and sl ...
Slide 1
... given by the equation shown. The ‘dimension’ in the case of a neutron star is assumed to be the radius of the polar cap where the magnetic field lines are concentrated. This is ~2% of the total surface of the neutron star thus for a radius of 10,000m is about 3000m. The conductivity, , can be found ...
... given by the equation shown. The ‘dimension’ in the case of a neutron star is assumed to be the radius of the polar cap where the magnetic field lines are concentrated. This is ~2% of the total surface of the neutron star thus for a radius of 10,000m is about 3000m. The conductivity, , can be found ...
High Resolution Chandra Spectroscopy of Gamma Cassiopeia (B0
... thermal spectrum of the X-rays. However, while the star is now established as part of a binary system (see Harmanec et al. 2000; Miroshnichenko, Bjorkman, & Krugov 2002), the wide separation (P ≈ 204 days, with low to moderate eccentricity) makes it difficult to understand the high Lx if the compani ...
... thermal spectrum of the X-rays. However, while the star is now established as part of a binary system (see Harmanec et al. 2000; Miroshnichenko, Bjorkman, & Krugov 2002), the wide separation (P ≈ 204 days, with low to moderate eccentricity) makes it difficult to understand the high Lx if the compani ...
A model of slingshot prominences in rapidly rotating stars
... stars but rather a very common property in rapidly rotating latetype stars (Collier Cameron & Woods 1992; Jeffries 1993). Recent observations of two rapidly rotating stars, HK Aquarii (Byrne, Eibe & Rolleston 1996) and He 699 (Barnes et al. 1998) indicate the presence of low-lying absorption feature ...
... stars but rather a very common property in rapidly rotating latetype stars (Collier Cameron & Woods 1992; Jeffries 1993). Recent observations of two rapidly rotating stars, HK Aquarii (Byrne, Eibe & Rolleston 1996) and He 699 (Barnes et al. 1998) indicate the presence of low-lying absorption feature ...
galactic cosmic radiation and solar energetic particles
... as the inverse of the solar sunspot number cycle. This is discussed more fully in Section 6.2.2.1. The isotropic flux exposure to galactic cosmic radiation in space at sunspot minimum is - 4 protons cm 2 s' resulting in a yearly integrated exposure of - 1.3 x 108 protons/cm2. The isotropic flux expo ...
... as the inverse of the solar sunspot number cycle. This is discussed more fully in Section 6.2.2.1. The isotropic flux exposure to galactic cosmic radiation in space at sunspot minimum is - 4 protons cm 2 s' resulting in a yearly integrated exposure of - 1.3 x 108 protons/cm2. The isotropic flux expo ...
Diffusion of cosmic rays at EeV energies in
... second knee marks the end of the galactic cosmic ray spectrum, one would need a new class of sources accelerating light elements to fill the gap between second knee and ankle, and still be consistent with the measurements [2–4, 12]. Regardless of the energy where the transition from galactic to extr ...
... second knee marks the end of the galactic cosmic ray spectrum, one would need a new class of sources accelerating light elements to fill the gap between second knee and ankle, and still be consistent with the measurements [2–4, 12]. Regardless of the energy where the transition from galactic to extr ...
Plasmoid-induced-reconnection and fractal reconnection Kazunari Shibata and Syuniti Tanuma
... In this section, we examine the physical mechanism of the plasmoid-induced-reconnection in more detail. We consider a situation where reconnection has just begun and a plasmoid, with a length L p and a width W p , has just started to form. The reconnection generates a jet (with the Alfvén speed V A ...
... In this section, we examine the physical mechanism of the plasmoid-induced-reconnection in more detail. We consider a situation where reconnection has just begun and a plasmoid, with a length L p and a width W p , has just started to form. The reconnection generates a jet (with the Alfvén speed V A ...
Sunspots: from small-scale inhomogeneities towards a global theory
... The umbra of a sunspot harbors dynamic inhomogeneities. They are observed as dot-like bright spots with typical sizes of half an arcsec or less, embedded in a more uniform and darker background. These umbral dots seem to be present in all sunspots, although their intensity varies a lot. In some spot ...
... The umbra of a sunspot harbors dynamic inhomogeneities. They are observed as dot-like bright spots with typical sizes of half an arcsec or less, embedded in a more uniform and darker background. These umbral dots seem to be present in all sunspots, although their intensity varies a lot. In some spot ...
Hydrostatic equilibrium in a magnetized, warped Galactic disc
... synchrotron intensity as Btot . 6 mG (Beck 2001). With observations of synchrotron polarization showing B0 / Btot . 0:6, as described below, this gives B0 . 4 mG (Beck 2001); if anisotropic turbulent magnetic fields are present this is an upper limit on B0. Observations of Faraday rotation measures ...
... synchrotron intensity as Btot . 6 mG (Beck 2001). With observations of synchrotron polarization showing B0 / Btot . 0:6, as described below, this gives B0 . 4 mG (Beck 2001); if anisotropic turbulent magnetic fields are present this is an upper limit on B0. Observations of Faraday rotation measures ...
Exospheres and Atmospheric Escape
... Those processes occurring in the upper atmosphere of a planet or planetary satellite that determine the structure of the corona and lead to molecular escape are considered in this paper. A planet’s atmosphere decreases in density with increasing altitude, thus an altitude is eventually reached above ...
... Those processes occurring in the upper atmosphere of a planet or planetary satellite that determine the structure of the corona and lead to molecular escape are considered in this paper. A planet’s atmosphere decreases in density with increasing altitude, thus an altitude is eventually reached above ...
![The dependence of the [FUV-MUV] colour index on solar cycle](http://s1.studyres.com/store/data/021819603_1-71914b6b41ba57717c9aa126236e24f5-300x300.png)
The dependence of the [FUV-MUV] colour index on solar cycle
... colour is introduced to study the solar UV spectral slope during the cycle. The calculated colour is corrected for aging effects due to an efficiency reduction of SOLSTICE FUV irradiance. In order to extract the 11-year scale variation, the Empirical Mode Decomposition (EMD) is applied to the data s ...
... colour is introduced to study the solar UV spectral slope during the cycle. The calculated colour is corrected for aging effects due to an efficiency reduction of SOLSTICE FUV irradiance. In order to extract the 11-year scale variation, the Empirical Mode Decomposition (EMD) is applied to the data s ...
Effects of Thomson-Scattering Geometry on White-Light
... determination of CME kinematics, in particular the propagation direction, can be ambiguous. The assumptions that one is always observing the same part of a CME can lead to large errors in the estimated height of the CME’s leading edge. The structure of a CME affects the derivation of its kinematic p ...
... determination of CME kinematics, in particular the propagation direction, can be ambiguous. The assumptions that one is always observing the same part of a CME can lead to large errors in the estimated height of the CME’s leading edge. The structure of a CME affects the derivation of its kinematic p ...
Surface temperature distribution and absorption features in Isolated
... the crust, develops extending about 1 to 2 km. It is made of a Coulomb lattice of nuclei and a free gas of ultra-relativistic degenerate electrons; the neutron drip density ρd ∼ 1011 g cm−3 defines the boundary between the outer and the inner crust. In the latter it is energetically favourable for n ...
... the crust, develops extending about 1 to 2 km. It is made of a Coulomb lattice of nuclei and a free gas of ultra-relativistic degenerate electrons; the neutron drip density ρd ∼ 1011 g cm−3 defines the boundary between the outer and the inner crust. In the latter it is energetically favourable for n ...
Solar Convection Zone
... zone(CZ), as revealed by supercomputer simulations. One class of models, covering roughly the rst half of the logarithmic mass density interval from the photosphere to the bottom of the convection zone, is an accurate representation of the solar surface layers. These models provide quantitative inf ...
... zone(CZ), as revealed by supercomputer simulations. One class of models, covering roughly the rst half of the logarithmic mass density interval from the photosphere to the bottom of the convection zone, is an accurate representation of the solar surface layers. These models provide quantitative inf ...
- Repository of the Academy`s Library
... conditions of broad interest. In particular, there are conditions directly relevant to the efforts in controlled fusion. Also, the corona and magnetosphere are priceless for the investigation of fundamental physical processes operating in natural and laboratory plasmas (e.g. magnetic reconnection, w ...
... conditions of broad interest. In particular, there are conditions directly relevant to the efforts in controlled fusion. Also, the corona and magnetosphere are priceless for the investigation of fundamental physical processes operating in natural and laboratory plasmas (e.g. magnetic reconnection, w ...
Periodic Spectral Line Asymmetries In Solar Coronal Structures From Slow Magnetoacoustic Waves
... ...are slow magnetoacoustic waves These perturbations have been interpreted as slow magnetoacoustic waves propagating along plume/loop structures. [De Moortel et al. 2000, Nakariakov et al. 2000, Robbrecht et al. 2001, ..., ...]. ...
... ...are slow magnetoacoustic waves These perturbations have been interpreted as slow magnetoacoustic waves propagating along plume/loop structures. [De Moortel et al. 2000, Nakariakov et al. 2000, Robbrecht et al. 2001, ..., ...]. ...
The magnetic field configuration of a solar prominence inferred from
... compatible with the present, low-resolution observational constraints. The local magnetic field in prominences has also been investigated by interpreting the dynamics of rising plumes using magnetohydrodynamic models (Hillier et al. 2012a,b). Here we present the results of the analysis of ground-bas ...
... compatible with the present, low-resolution observational constraints. The local magnetic field in prominences has also been investigated by interpreting the dynamics of rising plumes using magnetohydrodynamic models (Hillier et al. 2012a,b). Here we present the results of the analysis of ground-bas ...
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.