S.V. Berdyugina, I.G. Usoskin, Preferred Longitudes in Sunspot
... time and find that the regions migrate in phase as rigid structures. When a region reaches ϕ = 1, it appears again near ϕ = 0. In such cases we add an integer to the phase and unfold continuous migration of the regions. An example for the solar cycle 18 is shown in Fig. 2. The migration results in a ...
... time and find that the regions migrate in phase as rigid structures. When a region reaches ϕ = 1, it appears again near ϕ = 0. In such cases we add an integer to the phase and unfold continuous migration of the regions. An example for the solar cycle 18 is shown in Fig. 2. The migration results in a ...
An exceptionally bright flare from SGR 1806–20 and the origins of
... Soft-g-ray repeaters (SGRs) are galactic X-ray stars that emit numerous short-duration (about 0.1 s) bursts of hard X-rays during sporadic active periods. They are thought to be magnetars: strongly magnetized neutron stars with emissions powered by the dissipation of magnetic energy. Here we report ...
... Soft-g-ray repeaters (SGRs) are galactic X-ray stars that emit numerous short-duration (about 0.1 s) bursts of hard X-rays during sporadic active periods. They are thought to be magnetars: strongly magnetized neutron stars with emissions powered by the dissipation of magnetic energy. Here we report ...
Probability of Solar Flares Turn Out to Form a Coronal Mass
... The main theme of this work is to investigate the dynamical structure of solar radio burst type III and II burst in the low frequency radio region. The region from 45 - 870 MHz will be focused. In this case, how large solar flares can relate to the Coronal Mass Ejections (CMEs) events will be highli ...
... The main theme of this work is to investigate the dynamical structure of solar radio burst type III and II burst in the low frequency radio region. The region from 45 - 870 MHz will be focused. In this case, how large solar flares can relate to the Coronal Mass Ejections (CMEs) events will be highli ...
Dennett-Thorpe-deBruyn,2002
... scintillation induced variations. We have evidence however that the source is remarkably stable over a period of many months with only a slow increase in brightness over the last two years (Dennett-Thorpe & de Bruyn, in prep). Scintillation in known variable sources and those with slower variations ...
... scintillation induced variations. We have evidence however that the source is remarkably stable over a period of many months with only a slow increase in brightness over the last two years (Dennett-Thorpe & de Bruyn, in prep). Scintillation in known variable sources and those with slower variations ...
Dating the Earliest Solids in our Solar System
... Chondritic meteorites (chondrites), the oldest rocks in our solar system, provide a significant record of the processes that transformed a disk of gas and dust into a collection of planets, moons, asteroids, and comets. They are considered to be the building blocks of the inner planets, Mercury, Ven ...
... Chondritic meteorites (chondrites), the oldest rocks in our solar system, provide a significant record of the processes that transformed a disk of gas and dust into a collection of planets, moons, asteroids, and comets. They are considered to be the building blocks of the inner planets, Mercury, Ven ...
Long-term evolution of a dipolar-type magnetosphere interacting
... an additional inflow of a stellar wind is prescribed. Hayashi et al. (1996) and GWB97 already demonstrated that a stellar magnetic dipole connected to a disk is deformed within some Keplerian periods. However, the fate of such a field geometry over many rotational periods has not been investigated. ...
... an additional inflow of a stellar wind is prescribed. Hayashi et al. (1996) and GWB97 already demonstrated that a stellar magnetic dipole connected to a disk is deformed within some Keplerian periods. However, the fate of such a field geometry over many rotational periods has not been investigated. ...
Astronomy Astrophysics Pulsar timing irregularities and the imprint of magnetic field evolution
... 105 yr. The only general fact that we can expect is that, for lowfield middle-aged neutron stars (104 –105 yr), this is expected to be the dominant process, thus resulting in n > 3. 3.3. Hall drift oscillatory modes ...
... 105 yr. The only general fact that we can expect is that, for lowfield middle-aged neutron stars (104 –105 yr), this is expected to be the dominant process, thus resulting in n > 3. 3.3. Hall drift oscillatory modes ...
PPT
... • A linear pinched discharge in the laboratory is a cylindrical plasma column (radius a) that is confined (or pinched) by toroidal magnetic field due to current ( ) flowing along its surface or through its interior • This configuration is similar to magnetic flux tubes present in the solar atmospher ...
... • A linear pinched discharge in the laboratory is a cylindrical plasma column (radius a) that is confined (or pinched) by toroidal magnetic field due to current ( ) flowing along its surface or through its interior • This configuration is similar to magnetic flux tubes present in the solar atmospher ...
Solar flux variation of the electron temperature morning
... plasma drift velocities further decrease the local ion density, which increases Te. As the ion density builds up after sunrise, Te decreases to daytime values that are reached at about 09 LT. The neutral density and the electron‐neutral cooling rate also build up after sunrise but it has a smaller e ...
... plasma drift velocities further decrease the local ion density, which increases Te. As the ion density builds up after sunrise, Te decreases to daytime values that are reached at about 09 LT. The neutral density and the electron‐neutral cooling rate also build up after sunrise but it has a smaller e ...
Magnetar-driven Hypernovae
... envelope phase (e.g. Tutukov & Yungelson 1979 ). In both cases the hydrogen envelope is dispersed leaving a bare helium core. ...
... envelope phase (e.g. Tutukov & Yungelson 1979 ). In both cases the hydrogen envelope is dispersed leaving a bare helium core. ...
Credit: X-ray: NASA/CXC/UMass/D. Wang et al.; Optical: Caltech/SSC/S.Stolovy
... NEILSEN ET AL. 2013B ...
... NEILSEN ET AL. 2013B ...
Chapter 30: Stars
... prominence, shown in Figure 30-6B, which is an arc of gas that is ejected from the chromosphere, or gas that condenses in the inner corona and rains back to the surface. Prominences can reach temperatures greater than 50 000 K and can last from a few hours to a few months. Like flares, prominences a ...
... prominence, shown in Figure 30-6B, which is an arc of gas that is ejected from the chromosphere, or gas that condenses in the inner corona and rains back to the surface. Prominences can reach temperatures greater than 50 000 K and can last from a few hours to a few months. Like flares, prominences a ...
EFFECTS OF STRONG STRATIFICATION ON EQUATORWARD DYNAMO WAVE PROPAGATION ¨ P
... configurations deduced from observations of rapidly rotating late-type stars. Subject headings: Magnetohydrodynamics – convection – turbulence – Sun: dynamo, rotation, activity 1. INTRODUCTION ...
... configurations deduced from observations of rapidly rotating late-type stars. Subject headings: Magnetohydrodynamics – convection – turbulence – Sun: dynamo, rotation, activity 1. INTRODUCTION ...
PDF Full-text
... the photodissociation rate for H2 O in exoplanets with solar-type and M dwarf host stars including the observed UV fluxes and Lyman-α corrected for interstellar absorption to evaluate the H2 O loss rate. At this time, however, there are very few disequilibrium chemistry calculations that include obs ...
... the photodissociation rate for H2 O in exoplanets with solar-type and M dwarf host stars including the observed UV fluxes and Lyman-α corrected for interstellar absorption to evaluate the H2 O loss rate. At this time, however, there are very few disequilibrium chemistry calculations that include obs ...
the amplitude of solar oscillations using stellar techniques
... than that measured by BiSON, by a factor of 1:07 0:04. The error bar comes from the uncertainty in fitting the background to the HARPS spectrum. However, we must keep in mind that our observations of the Sun were made over only a few hours, and at a single epoch during the 11 yr solar cycle. To co ...
... than that measured by BiSON, by a factor of 1:07 0:04. The error bar comes from the uncertainty in fitting the background to the HARPS spectrum. However, we must keep in mind that our observations of the Sun were made over only a few hours, and at a single epoch during the 11 yr solar cycle. To co ...
Analytical estimates of the resistivity due to ion
... Cusp-shaped soft X-ray structure on the northeast limb of the Sun observed by the soft X-ray telescope on the Yohkoh spacecraft. Reconnection above the cusp structure may drive a coronal mass ejection and eruptive flare. ...
... Cusp-shaped soft X-ray structure on the northeast limb of the Sun observed by the soft X-ray telescope on the Yohkoh spacecraft. Reconnection above the cusp structure may drive a coronal mass ejection and eruptive flare. ...
The Salpeter plasma correction for solar fusion reactions
... Shaviv & Shaviv (1997, 2000) state that a significant dynamic effect on screening does exist. We have not been able to extract from their work a single definitive analytic formula to compare with the Salpeter result, or with the various results of the rest of the heterodox “screening” literature. We ...
... Shaviv & Shaviv (1997, 2000) state that a significant dynamic effect on screening does exist. We have not been able to extract from their work a single definitive analytic formula to compare with the Salpeter result, or with the various results of the rest of the heterodox “screening” literature. We ...
1. INTRODUCTION - Stanford University
... from 108 runs of the Homestake experiment are divided into four quartiles, sorted according to latitude, we Ðnd that the northernmost quartile exhibits a larger variance than the other three. By applying the shuffle test, we estimate the probability that this could have occurred by chance to be in t ...
... from 108 runs of the Homestake experiment are divided into four quartiles, sorted according to latitude, we Ðnd that the northernmost quartile exhibits a larger variance than the other three. By applying the shuffle test, we estimate the probability that this could have occurred by chance to be in t ...
plasma/tokamak (alex/steve)new - General Atomics Fusion Education
... electron. The electron gives up its energy, moving to a lower orbit, when recombining with the ion. The release of this energy is through a photon at a specific visible light frequency (red). (See the chapter on the electromagnetic spectrum for a more detailed description.) One of the uses for highe ...
... electron. The electron gives up its energy, moving to a lower orbit, when recombining with the ion. The release of this energy is through a photon at a specific visible light frequency (red). (See the chapter on the electromagnetic spectrum for a more detailed description.) One of the uses for highe ...
The fraction of DA white dwarfs with kilo
... errors cannot completely be ruled out at this level of accuracy. We also observed the sdO star EC 11481-2303 but could not detect a magnetic field. Conclusions. VLT observations with uncertainties typically of 1000 G or less suggest that 15−20% of WDs have kG fields. Together with previous investiga ...
... errors cannot completely be ruled out at this level of accuracy. We also observed the sdO star EC 11481-2303 but could not detect a magnetic field. Conclusions. VLT observations with uncertainties typically of 1000 G or less suggest that 15−20% of WDs have kG fields. Together with previous investiga ...
The on quilibrium ISIS
... Characteristics of our spectral code (Ji PhD thesis 2006) based on the updated atomic data (CHIANTI , APED) the atomic data and the code are separate ...
... Characteristics of our spectral code (Ji PhD thesis 2006) based on the updated atomic data (CHIANTI , APED) the atomic data and the code are separate ...
Magnetic Doppler imaging of the roAp star HD 24712⋆
... the 2.56 m Nordic Optical Telescope (NOT), La Palma, Spain. The spectrograph is equipped with three different cameras, and to obtain observations in the spectropolarimetric mode, the second camera was used. For MDI we used 49 different spectral lines from seven spectral orders, each covering about 4 ...
... the 2.56 m Nordic Optical Telescope (NOT), La Palma, Spain. The spectrograph is equipped with three different cameras, and to obtain observations in the spectropolarimetric mode, the second camera was used. For MDI we used 49 different spectral lines from seven spectral orders, each covering about 4 ...
ASTR 330: The Solar System Dr Conor Nixon Fall 2006
... • The near 30-day cycle of lunar phases gives us the basic period of one ‘monath’, or month. • We can then simply divide the year (solar cycle) into 12 months (lunar cycles), with some extra days being added to some of the months. • We already know where the idea of ‘day’ comes from… … but where doe ...
... • The near 30-day cycle of lunar phases gives us the basic period of one ‘monath’, or month. • We can then simply divide the year (solar cycle) into 12 months (lunar cycles), with some extra days being added to some of the months. • We already know where the idea of ‘day’ comes from… … but where doe ...
The complex planetary synchronization structure of the solar system
... Newtonian mechanics calculates that the theoretical tidal elongation induced by the gravity of the planets inside the Sun is just a fraction of millimeter (Scafetta, 2012c). Therefore, tidal forcing appears too small to effect the Sun. However, as discussed above, also the magnitude of the tidal elo ...
... Newtonian mechanics calculates that the theoretical tidal elongation induced by the gravity of the planets inside the Sun is just a fraction of millimeter (Scafetta, 2012c). Therefore, tidal forcing appears too small to effect the Sun. However, as discussed above, also the magnitude of the tidal elo ...
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.