THE MnI 539.47 nm LINE VARIATION IN SOLAR ACTIVE REGIONS
... Cyclic behavior was detected for several lines. As is expected chromospheric lines show a strong cycle response, while photospheric lines vary only slightly with the single exception of the Mn I 539.47 nm line. Its equivalent width varied from about 78.6 mÅ at maximum to about 79.8 mÅ at the minim ...
... Cyclic behavior was detected for several lines. As is expected chromospheric lines show a strong cycle response, while photospheric lines vary only slightly with the single exception of the Mn I 539.47 nm line. Its equivalent width varied from about 78.6 mÅ at maximum to about 79.8 mÅ at the minim ...
COSPAR WORKSHOP ON CAPACITY DEVELOPMENT
... • The dayside is obvious from UV dayglow on the left side of the figure, midnight is at the east coast of the US • Aurora is caused by charged particles hitting the atmosphere and exciting electrons to higher energy levels which decay producing light ...
... • The dayside is obvious from UV dayglow on the left side of the figure, midnight is at the east coast of the US • Aurora is caused by charged particles hitting the atmosphere and exciting electrons to higher energy levels which decay producing light ...
Lab 02: Determining the Solar and Sidereal Days
... has been color-inverted so that the sky appears white and the starlight appears gray or black. A long photographic exposure will show the apparent path of the stars as the earth spins. Thus, in exactly one sidereal day, a star would trail out a complete circle of 360°. By measuring the fraction of t ...
... has been color-inverted so that the sky appears white and the starlight appears gray or black. A long photographic exposure will show the apparent path of the stars as the earth spins. Thus, in exactly one sidereal day, a star would trail out a complete circle of 360°. By measuring the fraction of t ...
Gravitational redshifts
... • Plausible amount: 1 % of “general” line broadening = 0.5 – 1 km/s ? • Mapping 3-D structure from different shifts in different lines ! • Need line synthesis from 3-D hydrodynamic models ! • Lines closer to cluster centers gravitationally more redshifted ...
... • Plausible amount: 1 % of “general” line broadening = 0.5 – 1 km/s ? • Mapping 3-D structure from different shifts in different lines ! • Need line synthesis from 3-D hydrodynamic models ! • Lines closer to cluster centers gravitationally more redshifted ...
ppt
... similar to elemental abundances observed in their environment, suggesting that they have been accelerated from interstellar matter. The main difference is that the valleys are ...
... similar to elemental abundances observed in their environment, suggesting that they have been accelerated from interstellar matter. The main difference is that the valleys are ...
Friday April 21 , h 08:45, Polo Scientifico Tecnologico Fabio Ferrari
... Permutation Entropy: one tool, multiple applications ...
... Permutation Entropy: one tool, multiple applications ...
Fulltext PDF
... identified in the laboratory. It was to take another 70 years before the green line was properly identified as due to emission not from a neutral iron atom but from an iron atom which had 13 of its 26' electrons stripped off. The existence of such highly ionized atoms in the corona indicated that th ...
... identified in the laboratory. It was to take another 70 years before the green line was properly identified as due to emission not from a neutral iron atom but from an iron atom which had 13 of its 26' electrons stripped off. The existence of such highly ionized atoms in the corona indicated that th ...
Multidimensional and inhomogeneity effects on scattering
... He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the magnetic field, one usually assumes that the emergent spectral line is formed by single scattering (optically thin regime) of the incident continuum radiation, or, in a bi ...
... He1083 line as demonstrated by, for example, Asensio Ramos et al. (2008). To find the unknown magnitude and the orientation of the magnetic field, one usually assumes that the emergent spectral line is formed by single scattering (optically thin regime) of the incident continuum radiation, or, in a bi ...
The Sun The Sun is a very typical main sequence star. It contains 1000
... The apparent magnitude scale of ancient Greece was based on defining the brightest stars as having an apparent magnitude m=+1 and the dimmest stars (just visible to the naked eye) with a magnitude ...
... The apparent magnitude scale of ancient Greece was based on defining the brightest stars as having an apparent magnitude m=+1 and the dimmest stars (just visible to the naked eye) with a magnitude ...
One
... • Careful studies of motions on the sun’s surface have supplied more detail about what is happening inside the sun. The parts of the sun include the core, the radiative zone, and the convective zone. 1. 1. At the center of the sun is the core. The core makes up 25% of the sun’s total diameter of 1,3 ...
... • Careful studies of motions on the sun’s surface have supplied more detail about what is happening inside the sun. The parts of the sun include the core, the radiative zone, and the convective zone. 1. 1. At the center of the sun is the core. The core makes up 25% of the sun’s total diameter of 1,3 ...
Magnetic Fields in the ICM and IGM from Active Galaxies
... 1. Diffused Radio Emission: Distribution and strength of cosmic magnetic fields, seeding from first stars, dwarf galaxies, AGN feedbacks, or (turbulent) dynamo. 2. Differential FRM of jet pc-kpc scale: is there current? 3. Clusters as magnetic field laboratories: Structure formation, AGNs, heating, ...
... 1. Diffused Radio Emission: Distribution and strength of cosmic magnetic fields, seeding from first stars, dwarf galaxies, AGN feedbacks, or (turbulent) dynamo. 2. Differential FRM of jet pc-kpc scale: is there current? 3. Clusters as magnetic field laboratories: Structure formation, AGNs, heating, ...
The Sun and other Stars
... Just below the photosphere the Sun is so dense that movement of photons is so slow that convection currents begin to circulate the Sun’s energy. This is called the zone. ...
... Just below the photosphere the Sun is so dense that movement of photons is so slow that convection currents begin to circulate the Sun’s energy. This is called the zone. ...
The coronal temperatures of low-mass main
... The mass dependence of coronal temperature in the saturated regime is an interesting consequence of the fact that coronal temperature depends on FX and not RX and can have consequences for the influence of stellar high-energy radiation on the upper atmospheres of planets. Given that the location of ...
... The mass dependence of coronal temperature in the saturated regime is an interesting consequence of the fact that coronal temperature depends on FX and not RX and can have consequences for the influence of stellar high-energy radiation on the upper atmospheres of planets. Given that the location of ...
Coronal Mass Ejections and Angular Momentum Loss in Young Stars
... 2.1. Angular momentum loss In AA12, we extrapolate the solar CME mass/flare energy relationship (Fig. 1) to TTS flare energies and frequencies (Fig. 2) and construct a CME frequency distribution as a function of CME mass. Given the observational completeness limits on the flare distributions that we ...
... 2.1. Angular momentum loss In AA12, we extrapolate the solar CME mass/flare energy relationship (Fig. 1) to TTS flare energies and frequencies (Fig. 2) and construct a CME frequency distribution as a function of CME mass. Given the observational completeness limits on the flare distributions that we ...
HELIOSTAT II - MEASURING THE SOLAR ROTATION
... The Earth's and the Sun's axes of rotation are not aligned with each other: the Earth's north pole is aimed approximately towards Polaris in Ursa Minor, while the Sun's north pole is oriented about 26° away towards the star Delta Draconis. As a result, when we view the Sun from the Earth at differen ...
... The Earth's and the Sun's axes of rotation are not aligned with each other: the Earth's north pole is aimed approximately towards Polaris in Ursa Minor, while the Sun's north pole is oriented about 26° away towards the star Delta Draconis. As a result, when we view the Sun from the Earth at differen ...
Slide 1
... system. You can see the vertical green plasma jet which is guided by the star’s magnetic field. The white zones are gas and dust, being illuminated from inside by the young star. The dark central zone is where the dust is so optically thick that the light is not being transmitted. ...
... system. You can see the vertical green plasma jet which is guided by the star’s magnetic field. The white zones are gas and dust, being illuminated from inside by the young star. The dark central zone is where the dust is so optically thick that the light is not being transmitted. ...
The Rotational Period of the Sun (Higher Level)
... What can a spectrum tell us? Answer: the composition of an object such as a star, its temperature, its pressure, the abundance of elements in the star, its motion (velocity). How can we tell if the Sun is rotating? Answer: we look at its spectrum from different regions. If the lines are shifted towa ...
... What can a spectrum tell us? Answer: the composition of an object such as a star, its temperature, its pressure, the abundance of elements in the star, its motion (velocity). How can we tell if the Sun is rotating? Answer: we look at its spectrum from different regions. If the lines are shifted towa ...
Dynamic Martian magnetosphere: Transient - HAL
... outward from this boundary (E conv = V B) while in the opposite hemisphere, no evidence of magnetic field increase is seen. In the terminator plane the MPB is symmetric with respect to the magnetic equator (Bx 0 in the draping region). The recovery time of the MPB can be obtained by tracking the ...
... outward from this boundary (E conv = V B) while in the opposite hemisphere, no evidence of magnetic field increase is seen. In the terminator plane the MPB is symmetric with respect to the magnetic equator (Bx 0 in the draping region). The recovery time of the MPB can be obtained by tracking the ...
Transient events in the EUV transition region and chromosphere
... & Stein, 1997, Doyle et al., 1999). However it is likely that a large number of small-scale magnetic reconnections (Schrijver et al., 1998) which may be associated with events seen in extreme ultraviolet (EUV) and X-ray emission (Harrison, 1997, Berghmans et al., 1998, Preś & Phillips, 1999), are i ...
... & Stein, 1997, Doyle et al., 1999). However it is likely that a large number of small-scale magnetic reconnections (Schrijver et al., 1998) which may be associated with events seen in extreme ultraviolet (EUV) and X-ray emission (Harrison, 1997, Berghmans et al., 1998, Preś & Phillips, 1999), are i ...
stars - Chandra X
... α Cen AB: solar-like behavior (Ayres+ 2009) • cycles • rotational modulation, • slow changes in coronal T ...
... α Cen AB: solar-like behavior (Ayres+ 2009) • cycles • rotational modulation, • slow changes in coronal T ...
2 Galactic radiation fields
... • All but the most highly energetic cosmic rays are tied to the magnetic field of the galaxy and therefore scatter repeatedly within the disk, leading to the local energy density in CRs being relatively uniform. • The spectrum of the cosmic rays (i.e. the flux per unit energy) decreases sharply with ...
... • All but the most highly energetic cosmic rays are tied to the magnetic field of the galaxy and therefore scatter repeatedly within the disk, leading to the local energy density in CRs being relatively uniform. • The spectrum of the cosmic rays (i.e. the flux per unit energy) decreases sharply with ...
The Sunspots - Scientific Research Publishing
... known that the presence of Sunspots on the solar disk is related to a substantial increase in sun’s activity. The most important expression of that activity is the emission of large quantities of charged particles which conforms the so called solar wind. The strong interaction of the solar wind with ...
... known that the presence of Sunspots on the solar disk is related to a substantial increase in sun’s activity. The most important expression of that activity is the emission of large quantities of charged particles which conforms the so called solar wind. The strong interaction of the solar wind with ...
What is Beneath the Sunspots? Home Page ____________________________________________
... As an elongated plasma body detected by SOHO and shown in Fig.3 [4], and as suggested, in Fig.4-A, that an elongated plasma body links poles of opposite magnetic fields, and since the Maps of the travel-time anomalies showed the signatures of emerging flux that are mostly concentrated in circular ar ...
... As an elongated plasma body detected by SOHO and shown in Fig.3 [4], and as suggested, in Fig.4-A, that an elongated plasma body links poles of opposite magnetic fields, and since the Maps of the travel-time anomalies showed the signatures of emerging flux that are mostly concentrated in circular ar ...
9. Fascinating observations. But how much is well understood?
... sources which undergo repeted bursting of subsecond duration. Sometimes they exhibit luminous superflares lasting some 100 seconds but their repetition has not yet been observed. The other class of high field objects are the Anomalous X-ray Pulsars (AXP).They were discovered as pulsating X-ray sourc ...
... sources which undergo repeted bursting of subsecond duration. Sometimes they exhibit luminous superflares lasting some 100 seconds but their repetition has not yet been observed. The other class of high field objects are the Anomalous X-ray Pulsars (AXP).They were discovered as pulsating X-ray sourc ...
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.