FP11: DRAKE et al. - Astronomical Institute WWW Homepage
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
... rotational phases of HD 3980 were calculated using the ephemeris from Maitzen et al. (1980). Two “Li spots” are observed on the surface of the star. The Li I line originated in spot 1 appears at the phase φ = – 0.146 = 0.832 and moves to the red up to the phase φ = 0.146. The second Li-rich spot (sp ...
science - St Edward`s Oxford
... operation. At that point, mission managers will have to start turning off these instruments one by one to conserve power, with the last one turning off around….. The two Voyager spacecraft were launched in 1977 and, between them, had visited Jupiter, Saturn, Uranus and Neptune by 1989. Voyager 1's p ...
... operation. At that point, mission managers will have to start turning off these instruments one by one to conserve power, with the last one turning off around….. The two Voyager spacecraft were launched in 1977 and, between them, had visited Jupiter, Saturn, Uranus and Neptune by 1989. Voyager 1's p ...
Evolution of filamentary molecular clouds in the presence of
... molecular clouds that make a different angle with the axis in the outer region of the filament. Fiege & Pudritz (2000) showed that the toroidal component of the magnetic field in the outer region of the filament dominates the other components when the models consist of poloidal and toroidal magnetic ...
... molecular clouds that make a different angle with the axis in the outer region of the filament. Fiege & Pudritz (2000) showed that the toroidal component of the magnetic field in the outer region of the filament dominates the other components when the models consist of poloidal and toroidal magnetic ...
Geomagnetism and Aeronomy, 2016, Vol. 56, № 7, pp. 1
... heliospheric physics remain unsolved yet. In particular, we do not yet understand in details mechanisms of the solar dynamo and solar cycle, heating of the solar corona and formation of the solar wind, acceleration of charged particles to high (relativistic) energies and their transport in the helio ...
... heliospheric physics remain unsolved yet. In particular, we do not yet understand in details mechanisms of the solar dynamo and solar cycle, heating of the solar corona and formation of the solar wind, acceleration of charged particles to high (relativistic) energies and their transport in the helio ...
Solar-like oscillations in intermediate red giants
... Helioseismology is currently the best method for verifying stellar evolution modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
... Helioseismology is currently the best method for verifying stellar evolution modelling theories and for understanding the structure and interior processes within the sun. It was able to rule out the possibility that the solar neutrino problem was due to incorrect models. ...
Electromagnetic waves have unique traits.
... Because they do not need a medium, EM waves can pass through outer space, which is a near vacuum. Also, because they do not give up energy in traveling, EM waves can cross the great distances that separate stars and planets. For example, rays from the Sun travel about 150 million kilometers (93 mill ...
... Because they do not need a medium, EM waves can pass through outer space, which is a near vacuum. Also, because they do not give up energy in traveling, EM waves can cross the great distances that separate stars and planets. For example, rays from the Sun travel about 150 million kilometers (93 mill ...
Solar Changes and the Climate
... of half the sunspot activity may disappear by about 2015 (Penn and Livingston, 2006). These studies only suggest that the Sun may have left the 20th century grand maximum and not that it is entering another grand minimum…However, much more evidence is needed and at present there is very low confiden ...
... of half the sunspot activity may disappear by about 2015 (Penn and Livingston, 2006). These studies only suggest that the Sun may have left the 20th century grand maximum and not that it is entering another grand minimum…However, much more evidence is needed and at present there is very low confiden ...
Neutron Stars – Thermal Emitters
... indeed be detected, which added impetus to theoretical work as well as to modeling of expected NS observational properties. The crucial point, attracting a lot of interest in the astrophysical community, was that the study of NS cooling could constrain the physical properties of superdense matter in ...
... indeed be detected, which added impetus to theoretical work as well as to modeling of expected NS observational properties. The crucial point, attracting a lot of interest in the astrophysical community, was that the study of NS cooling could constrain the physical properties of superdense matter in ...
scholer-shocks
... ahead of it, and the wave steepens. The wave steepens until the flow becomes nonadiabatic. Viscous effects become important and a shock wave forms where steepening is balanced by viscous dissiplation. ...
... ahead of it, and the wave steepens. The wave steepens until the flow becomes nonadiabatic. Viscous effects become important and a shock wave forms where steepening is balanced by viscous dissiplation. ...
A FUSE Survey of Coronal Forbidden Lines in Late
... additional DR 0:4 1:3 R above the stellar photosphere, or represent the turbulent broadening caused by flows along magnetic loop structures. For the stars in which Fe xviii is detected, there is an excellent correlation between the observed Röntgensatellit (ROSAT) 0.2–2.0 keV soft X-ray flux and t ...
... additional DR 0:4 1:3 R above the stellar photosphere, or represent the turbulent broadening caused by flows along magnetic loop structures. For the stars in which Fe xviii is detected, there is an excellent correlation between the observed Röntgensatellit (ROSAT) 0.2–2.0 keV soft X-ray flux and t ...
Assessing the massive young Sun hypothesis to solve the warm
... CO2 atmosphere is that models predict that the CO2 will begin to condense out as a cloud layer at the required atmospheric pressures, thereby increasing the global albedo and off-setting the warming greenhouse effect (Kasting 1991). Pierrehumbert & Erlick (1998) proposed a model of the early martian ...
... CO2 atmosphere is that models predict that the CO2 will begin to condense out as a cloud layer at the required atmospheric pressures, thereby increasing the global albedo and off-setting the warming greenhouse effect (Kasting 1991). Pierrehumbert & Erlick (1998) proposed a model of the early martian ...
SAGE_prop
... until the mid 20th century that Bierman (1951) established the concept that `radiation' from the Sun was responsible, building on earlier work involving the interaction of atomic physics and astronomy that finally proved that the solar corona was hot (Grotian 1939, Edlen 1942). Despite major advance ...
... until the mid 20th century that Bierman (1951) established the concept that `radiation' from the Sun was responsible, building on earlier work involving the interaction of atomic physics and astronomy that finally proved that the solar corona was hot (Grotian 1939, Edlen 1942). Despite major advance ...
Low-energy charged particle measurement by MAP-PACE onboard SELENE
... from the lunar surface are mainly composed of neutrals, which are ionized by solar photons and electrons. Both ionized particles and sputtered/desorped ions are accelerated and transported by the solar wind in cycloidal motion. These ions will be observed by the in-situ low-energy ion measurement by ...
... from the lunar surface are mainly composed of neutrals, which are ionized by solar photons and electrons. Both ionized particles and sputtered/desorped ions are accelerated and transported by the solar wind in cycloidal motion. These ions will be observed by the in-situ low-energy ion measurement by ...
The Scale of the Cosmos
... • The darkness lasts only a few minutes. • This is because the umbra is never more than 270 km in diameter on Earth’s surface and sweeps across the landscape at over 1600 km/hr. • The period of totality lasts on average only 2 or 3 minutes and never more than 7.5 minutes. ...
... • The darkness lasts only a few minutes. • This is because the umbra is never more than 270 km in diameter on Earth’s surface and sweeps across the landscape at over 1600 km/hr. • The period of totality lasts on average only 2 or 3 minutes and never more than 7.5 minutes. ...
- Mastering Physics Answers
... unusual property that they do not interact with light, and therefore they do not respond to the electromagnetic forces that affect protons and electrons. Neutrinos can therefore stream outward from the center of the Sun nearly uninterrupted by collisions. We can detect them (by looking for their ver ...
... unusual property that they do not interact with light, and therefore they do not respond to the electromagnetic forces that affect protons and electrons. Neutrinos can therefore stream outward from the center of the Sun nearly uninterrupted by collisions. We can detect them (by looking for their ver ...
Opacities and spectra of hydrogen atmospheres of moderately
... fields B ∼ 1011 G. Meanwhile, available models of partially ionized hydrogen atmospheres of neutron stars with strong magnetic fields are restricted to B 1012 G. Extension of the applicability range of the photosphere models to lower field strengths is complicated by a stronger asymmetry of decent ...
... fields B ∼ 1011 G. Meanwhile, available models of partially ionized hydrogen atmospheres of neutron stars with strong magnetic fields are restricted to B 1012 G. Extension of the applicability range of the photosphere models to lower field strengths is complicated by a stronger asymmetry of decent ...
Possible new astrophysics-relevant experiments with high
... 5) Experimental comparison of two potent instabilities affecting a variety of collisionless processes in astrophysics: electromagnetic filamentation instability and (mostly) electrostatic beam-plasma instability. References: 1) D.D. Ryutov. “Destabilizing effect of thermal conductivity on the Raylei ...
... 5) Experimental comparison of two potent instabilities affecting a variety of collisionless processes in astrophysics: electromagnetic filamentation instability and (mostly) electrostatic beam-plasma instability. References: 1) D.D. Ryutov. “Destabilizing effect of thermal conductivity on the Raylei ...
Требования к файлу доклада для публикации
... An artist’s concept of the principal structures found in the central region shows the dipole magnetic field as dotted yellow curves anchored to the central MECO object. The luminous sharp ring at the inner edge of the accretion disc is the structure that becomes microlensed. The ultraviolet outer ou ...
... An artist’s concept of the principal structures found in the central region shows the dipole magnetic field as dotted yellow curves anchored to the central MECO object. The luminous sharp ring at the inner edge of the accretion disc is the structure that becomes microlensed. The ultraviolet outer ou ...
Lecture 30 Solar System Formation and Early Evolution
... The compositions of chondrites and other meteorites place important bounds on the formation of the solar system, although some are not mutually consistent. This indicates our incomplete understanding of the process. ~ Temporal constraints ~ J An absolute upper limit on the time of collapse of the so ...
... The compositions of chondrites and other meteorites place important bounds on the formation of the solar system, although some are not mutually consistent. This indicates our incomplete understanding of the process. ~ Temporal constraints ~ J An absolute upper limit on the time of collapse of the so ...
A magnetic communication scenario for hot Jupiters
... The input parameters of our model are the stellar and planetary parameters listed above, of which only T and B are varied in order to fit the observations. The only output is the stellar wind solution, i.e. density, magnetic field and velocity as a function of the distance from the stellar surfac ...
... The input parameters of our model are the stellar and planetary parameters listed above, of which only T and B are varied in order to fit the observations. The only output is the stellar wind solution, i.e. density, magnetic field and velocity as a function of the distance from the stellar surfac ...
SIMULATION OF QUIET-SUN WAVES IN THE Ca ii INFRARED TRIPLET
... Doppler shift analysis and obscures the true oscillatory signal. The magnetic flux in the quiet Sun is very small (3 Mx cm2 in the internetwork; Lites 2002), so useful observations need a high signal-to-noise ratio (S/ N 103 ), which, when combined with the high time cadence required to resolve ...
... Doppler shift analysis and obscures the true oscillatory signal. The magnetic flux in the quiet Sun is very small (3 Mx cm2 in the internetwork; Lites 2002), so useful observations need a high signal-to-noise ratio (S/ N 103 ), which, when combined with the high time cadence required to resolve ...
Hubble Does Double-Duty Science: Finding Planets and
... solar flare behavior. Based on the star’s brightness, we saw modest flares in the brighter stars (flares increase of 10% or less in the star’s brightness) and larger flares in the fainter stars. A surprising fraction (85%) of flaring stars showed underlying variations, despite being a small componen ...
... solar flare behavior. Based on the star’s brightness, we saw modest flares in the brighter stars (flares increase of 10% or less in the star’s brightness) and larger flares in the fainter stars. A surprising fraction (85%) of flaring stars showed underlying variations, despite being a small componen ...
Synergistic effect of sterilization by microwave-excited atmospheric-pressure plasma jet using photo-catalyst TiO2 with H2O2 and distilled water
... Unlike UV-based sterilization methods, a significant synergy on the bactericidal effect is observed when the plasma is combined with TiO2 and H2O2 at a time. All the bacteria samples used in ~4´107 CFU/ml of concentration are destructed within 30 seconds. A kinetic simulation shows plenty of electro ...
... Unlike UV-based sterilization methods, a significant synergy on the bactericidal effect is observed when the plasma is combined with TiO2 and H2O2 at a time. All the bacteria samples used in ~4´107 CFU/ml of concentration are destructed within 30 seconds. A kinetic simulation shows plenty of electro ...
Presentazione di PowerPoint
... • Multiwavelength studies to understand non-radiative heating of stellar atmospheres in late-type stars; • Partecipation to the ESA cornerstone mission GAIA; • Partecipation to the future ESA mission PLATO. ...
... • Multiwavelength studies to understand non-radiative heating of stellar atmospheres in late-type stars; • Partecipation to the ESA cornerstone mission GAIA; • Partecipation to the future ESA mission PLATO. ...
Magnetic fields in galaxies
... electrons in a range of energies: * widely assumed power law distribution of electrons combined with the equipartition of energy density between magnetic field ...
... electrons in a range of energies: * widely assumed power law distribution of electrons combined with the equipartition of energy density between magnetic field ...
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.