UCLA 2004
... probably all but at least half of 10Be is trapped GCRs •Trapped GCRs do not explain any other SLR, but 10Be is known to be decoupled from other SLRs (Marhas et al. 2002) ...
... probably all but at least half of 10Be is trapped GCRs •Trapped GCRs do not explain any other SLR, but 10Be is known to be decoupled from other SLRs (Marhas et al. 2002) ...
Fusion: A true challenge for an enormous reward
... Fusion of heavier nuclei in stars will occur at higher temperatures. From the formula above, it is immediately clear that a contraction of the star under its own gravity will further raise the central temperature. Fusion in heavy stars will continue to keep the star alive as long as the reactions ar ...
... Fusion of heavier nuclei in stars will occur at higher temperatures. From the formula above, it is immediately clear that a contraction of the star under its own gravity will further raise the central temperature. Fusion in heavy stars will continue to keep the star alive as long as the reactions ar ...
Propagation of Supernova Blast Waves through the ISM
... SNRs are the most bright radio sources detected, featuring a steep nonthermal spectrum: Sν ∝ ν α , α − 0,5 ⇒ cosmic-ray particles and synchroton radiation (Shklovskii 1953) Shock heating to ∼ 106 K → Chandra and XMM-Newton perform X-ray observations of SNRs and emission line spectrum of heavy metal ...
... SNRs are the most bright radio sources detected, featuring a steep nonthermal spectrum: Sν ∝ ν α , α − 0,5 ⇒ cosmic-ray particles and synchroton radiation (Shklovskii 1953) Shock heating to ∼ 106 K → Chandra and XMM-Newton perform X-ray observations of SNRs and emission line spectrum of heavy metal ...
Theoretical Predictions for Mass Loss Rates: Rotation & Pulsation
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible. ...
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible. ...
Jets in Active Galactic Nuclei Alan P. Marscher
... roughly self-similar over several orders of magnitude in distance from the black hole. This is easiest to understand if the jets are mainly fluid phenomena so that they are governed by the laws of gas dynamics and magnetohydrodynamics. Images of jets contain a bright, nearly unresolved “core” at the ...
... roughly self-similar over several orders of magnitude in distance from the black hole. This is easiest to understand if the jets are mainly fluid phenomena so that they are governed by the laws of gas dynamics and magnetohydrodynamics. Images of jets contain a bright, nearly unresolved “core” at the ...
New Mass Loss Measurements from Astrospheric Lyα Absorption
... In order to measure a mass-loss rate from the observed astrospheric absorption, it is necessary to know the ISM wind velocity seen by the star (VISM) and the orientation of the astrosphere relative to our line of sight (v), which are both listed in Table 1. The orientation angle, v, is the angle bet ...
... In order to measure a mass-loss rate from the observed astrospheric absorption, it is necessary to know the ISM wind velocity seen by the star (VISM) and the orientation of the astrosphere relative to our line of sight (v), which are both listed in Table 1. The orientation angle, v, is the angle bet ...
The Sun
... • The corona is very hot, but it is not very bright. – Its density is very low, only 106 atoms/cm3 in its lower regions. – That is about a trillion times less dense than the air you breathe. – In its outer layers, the corona contains only 1 to 10 atoms/cm3, less dense than the best vacuum on Earth. ...
... • The corona is very hot, but it is not very bright. – Its density is very low, only 106 atoms/cm3 in its lower regions. – That is about a trillion times less dense than the air you breathe. – In its outer layers, the corona contains only 1 to 10 atoms/cm3, less dense than the best vacuum on Earth. ...
Grand Minima of Solar Activity and the Mean
... of the 17th and the beginning of the 18th centuries. It is far from being obvious a priori that such long-term dynamics can be related to solar dynamo action. A mechanism that can in principle produce the long-term dynamics of the solar cycle in the form of Grand Minima has been suggested by Hoyng ( ...
... of the 17th and the beginning of the 18th centuries. It is far from being obvious a priori that such long-term dynamics can be related to solar dynamo action. A mechanism that can in principle produce the long-term dynamics of the solar cycle in the form of Grand Minima has been suggested by Hoyng ( ...
X-Ray and Extreme Ultraviolet Emission from Comets
... Astrophysical X-ray emission is generally found to originate from hot collisional plasmas, such as the million-degree gas found in the solar corona (e.g., Foukal, 1990), the 100million-degree gas observed in supernova remnants (e.g., Cioffi, 1990), or the accretion disks around neutron stars and bla ...
... Astrophysical X-ray emission is generally found to originate from hot collisional plasmas, such as the million-degree gas found in the solar corona (e.g., Foukal, 1990), the 100million-degree gas observed in supernova remnants (e.g., Cioffi, 1990), or the accretion disks around neutron stars and bla ...
the magnetic field properties of radio galaxies in different
... supporting AGN jet powering through extraction of spin energy of SMBH by dynamically important magnetic fields Magnetic field properties of radio-loud AGN in different accretion modes ...
... supporting AGN jet powering through extraction of spin energy of SMBH by dynamically important magnetic fields Magnetic field properties of radio-loud AGN in different accretion modes ...
Part 3
... Now, it is known (See Part 1, [8, 13]) that several decades ago the Space started to exert a powerful influence upon the Solar System. However, the scientifically proved manifestations of this influence, that can be seen in geophysical, climatic and social alterations, were not so evident (at least ...
... Now, it is known (See Part 1, [8, 13]) that several decades ago the Space started to exert a powerful influence upon the Solar System. However, the scientifically proved manifestations of this influence, that can be seen in geophysical, climatic and social alterations, were not so evident (at least ...
$doc.title
... Correlations between variations in Solar EUV and soft X-‐ray irradiance and photoelectron energy spectra observed on Mars and Earth ...
... Correlations between variations in Solar EUV and soft X-‐ray irradiance and photoelectron energy spectra observed on Mars and Earth ...
Energetic neutral atoms around HD 209458b
... to account for the larger photon fluxes at the orbital distance of HD 209458b. The stellar wind density and temperature have also been scaled from average solar conditions for our Sun using relations given by Russell et al. (1988). Given the close proximity of HD 209458b to its host star the choice ...
... to account for the larger photon fluxes at the orbital distance of HD 209458b. The stellar wind density and temperature have also been scaled from average solar conditions for our Sun using relations given by Russell et al. (1988). Given the close proximity of HD 209458b to its host star the choice ...
Solar Rotation - Stanford Solar Physics
... approximately 20 latitude, and is often used as a reference. The surface rotational velocity at this latitude is approximately 19 103 m s 1 . It is found that the rotation rate of individual sunspots may vary depending their size, age and relative position to other sunspots of the same group. ...
... approximately 20 latitude, and is often used as a reference. The surface rotational velocity at this latitude is approximately 19 103 m s 1 . It is found that the rotation rate of individual sunspots may vary depending their size, age and relative position to other sunspots of the same group. ...
Magnetic field structure in single late
... Bl estimates stay with a positive sign for the whole observational period (see Table 1 and Fig. 1). Thanks to a typical error bar as low as 0.5 G, significant variations are observed in the interval 0.1–8.2 G in 2010 and 1.3–6.7 G in 2011/2012. The smaller amplitude of variations observed in 2011/20 ...
... Bl estimates stay with a positive sign for the whole observational period (see Table 1 and Fig. 1). Thanks to a typical error bar as low as 0.5 G, significant variations are observed in the interval 0.1–8.2 G in 2010 and 1.3–6.7 G in 2011/2012. The smaller amplitude of variations observed in 2011/20 ...
parte ii - NivelesDeIngles
... colder, and has lower–density plasmathan average. These were found when X– ray telescopes in the Skylab mission were flown above theearth's atmosphere to reveal the structure of the corona. coronal mass ejection (CME) – eyección coronal de masa– (sol. phys.) A massive burst of solar wind, other ligh ...
... colder, and has lower–density plasmathan average. These were found when X– ray telescopes in the Skylab mission were flown above theearth's atmosphere to reveal the structure of the corona. coronal mass ejection (CME) – eyección coronal de masa– (sol. phys.) A massive burst of solar wind, other ligh ...
Evolution of inflation-generated magnetic field through
... was generated prior to or during big bang nucleosynthesis, and was not damped or amplified by a magnetohydrodynamic (MHD) or some other process and so stays frozen into the plasma [15]. In addition to the CMB temperature anisotropies that a primordial magnetic field induces (as mentioned above), suc ...
... was generated prior to or during big bang nucleosynthesis, and was not damped or amplified by a magnetohydrodynamic (MHD) or some other process and so stays frozen into the plasma [15]. In addition to the CMB temperature anisotropies that a primordial magnetic field induces (as mentioned above), suc ...
THE THERMAL INSTABILITY OF SOLAR PROMINENCE THREADS
... for coronal and PCTR temperatures, whereas cool prominence plasmas may be considered optically thick. Some authors (e.g., Rosner et al. 1978; Milne et al. 1979) have proposed corrections to the values of χ ∗ and α in the range of cool prominence temperatures, i.e., T < 15,000 K, in order to represen ...
... for coronal and PCTR temperatures, whereas cool prominence plasmas may be considered optically thick. Some authors (e.g., Rosner et al. 1978; Milne et al. 1979) have proposed corrections to the values of χ ∗ and α in the range of cool prominence temperatures, i.e., T < 15,000 K, in order to represen ...
THE EVOLUTION OF SOLAR FLUX FROM 0.1 nm TO 160μm
... in the Sun by a rotational dynamo (Parker 1970), couples to the solar wind out to the solar Alfvén radius, approximately 20 Solar radii. This coupling of internal rotational energy to the outer reaches of the stellar atmosphere enables the stellar wind to shed angular momentum over the solar lifeti ...
... in the Sun by a rotational dynamo (Parker 1970), couples to the solar wind out to the solar Alfvén radius, approximately 20 Solar radii. This coupling of internal rotational energy to the outer reaches of the stellar atmosphere enables the stellar wind to shed angular momentum over the solar lifeti ...
Magnetic-Island Contraction and Particle Acceleration in Simulated
... emission is gyrosynchrotron from accelerated electrons that spiral the coronal magnetic field (White et al. 2011). On the other hand, extreme ultraviolet (EUV), coronal soft X-ray, and other secondary emissions result from the thermalization of flare energy in the ambient atmosphere (see reviews by ...
... emission is gyrosynchrotron from accelerated electrons that spiral the coronal magnetic field (White et al. 2011). On the other hand, extreme ultraviolet (EUV), coronal soft X-ray, and other secondary emissions result from the thermalization of flare energy in the ambient atmosphere (see reviews by ...
SOLAR HARD X-RAY AND GAMMA-RAY OBSERVATIONS FROM
... e.g., Ramaty & Murphy 1987 for a review). If the spectrum of accelerated ions extends above a few hundred MeV nucleons -1 , the energetic neutrons produced in nuclear reactions ...
... e.g., Ramaty & Murphy 1987 for a review). If the spectrum of accelerated ions extends above a few hundred MeV nucleons -1 , the energetic neutrons produced in nuclear reactions ...
PDF only - at www.arxiv.org.
... 1960, I was pleased to accept the invitation to review evidence of neutron repulsion and its implications for the evolution of life. It will be shown that life [1] and atomic nuclei have evolved together on opposite sides of the Sun’s opaque photosphere. My conclusions do not support Fowler's concer ...
... 1960, I was pleased to accept the invitation to review evidence of neutron repulsion and its implications for the evolution of life. It will be shown that life [1] and atomic nuclei have evolved together on opposite sides of the Sun’s opaque photosphere. My conclusions do not support Fowler's concer ...
Plasma Seminar, April 13, 2015 "The Magnetized Dusty Plasmas
... • micron size pieces of material (Be, Fe, C, Ni, W) ablated and re-condensed from device walls usually during disruptions and then recirculated by device shaking. Can be detrimental to plasma, and poses critical safety issue (absorption of tritium). • ITER – toroidal field 13 T “dust” will have gy ...
... • micron size pieces of material (Be, Fe, C, Ni, W) ablated and re-condensed from device walls usually during disruptions and then recirculated by device shaking. Can be detrimental to plasma, and poses critical safety issue (absorption of tritium). • ITER – toroidal field 13 T “dust” will have gy ...
... The idea behind organizing nation-wide activities around the celestial events is not simply to explain the science behind these phenomena but to make the audience familiar with the method of science and lead them on the path of scientific exploration by encouraging them to ask questions and to searc ...
Formation of high-field magnetic white dwarfs from common envelopes
... two classes: AM Herculis (AM Her) (polars) and DQ Herculis (DQ Her) (intermediate polars). For reviews on AM Her and DQ Her systems, see refs. 9 and 10. Generally, AM Her systems are those in which both components of the binary are synchronously rotating at the orbital period. In this scenario, the ...
... two classes: AM Herculis (AM Her) (polars) and DQ Herculis (DQ Her) (intermediate polars). For reviews on AM Her and DQ Her systems, see refs. 9 and 10. Generally, AM Her systems are those in which both components of the binary are synchronously rotating at the orbital period. In this scenario, the ...
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.