![A single picture for solar coronal outflows and radio noise storms](http://s1.studyres.com/store/data/017454582_1-8e31761e55702d11e6798b6cf13ff511-300x300.png)
A single picture for solar coronal outflows and radio noise storms
... that the blue-shifts were associated with regions where the extrapolated coronal field lines appeared open. Similar suggestions were made by Harra et al. (2008) and Doschek et al. (2008). Baker et al. (2009) presented Hinode/EIS observations of NOAA 10942 and supplemented them with detailed magnetic ...
... that the blue-shifts were associated with regions where the extrapolated coronal field lines appeared open. Similar suggestions were made by Harra et al. (2008) and Doschek et al. (2008). Baker et al. (2009) presented Hinode/EIS observations of NOAA 10942 and supplemented them with detailed magnetic ...
Pickup ions near Mars associated with escaping oxygen atoms
... in channel 1 were 1000 cm2 s1 sr1 near the inbound shock crossing and 3000 cm2 s1 sr1 near the outbound shock. The statistical uncertainty associated with these fluxes is less than one percent. [10] The solar wind conditions appropriate for the test particle simulation for Circular Orbit 42 ...
... in channel 1 were 1000 cm2 s1 sr1 near the inbound shock crossing and 3000 cm2 s1 sr1 near the outbound shock. The statistical uncertainty associated with these fluxes is less than one percent. [10] The solar wind conditions appropriate for the test particle simulation for Circular Orbit 42 ...
The middle atmospheric circulation of a tidally locked Earth
... We investigate the influence of the sea surface temperature (SST) changes on the middle atmosphere of a tidally locked Earth-like planet orbiting a G star using the coupled 3D chemistry-climate model CESM1(WACCM). We perform three 90 day simulations. The first simulation is a present-day Earth (PDE) ...
... We investigate the influence of the sea surface temperature (SST) changes on the middle atmosphere of a tidally locked Earth-like planet orbiting a G star using the coupled 3D chemistry-climate model CESM1(WACCM). We perform three 90 day simulations. The first simulation is a present-day Earth (PDE) ...
Spectral properties, magnetic fields, and dust transport at lunar swirls
... homogeneous area of the lunar surface will nominally display a linear trend in this plot. For mare regions, higher maturity pixels are found in upper left, and immature pixels are found in the lower right, herein called the ‘‘maturity trend.’’ This trend is illustrated as Trend 2 in Fig. 3a, for the ...
... homogeneous area of the lunar surface will nominally display a linear trend in this plot. For mare regions, higher maturity pixels are found in upper left, and immature pixels are found in the lower right, herein called the ‘‘maturity trend.’’ This trend is illustrated as Trend 2 in Fig. 3a, for the ...
S.V. Berdyugina, I.G. Usoskin, Preferred Longitudes in Sunspot
... the two different filtering techniques, we find that the methods produce similar results (see Fig. 2). Therefore, we conclude that our results are method independent. For further analysis, we transform the Carrington longitudes, λ, into phases of the Carrington period: ϕ = λ/360 ◦. Note that the phas ...
... the two different filtering techniques, we find that the methods produce similar results (see Fig. 2). Therefore, we conclude that our results are method independent. For further analysis, we transform the Carrington longitudes, λ, into phases of the Carrington period: ϕ = λ/360 ◦. Note that the phas ...
Solar Rotation - Stanford Solar Physics
... The Sun rotates differentially, i.e. the solar rotation rate varies with both latitude and radius. The differential rotation is particularly prominent in the convection zone where equatorial zones rotate almost 30% faster than near-polar regions. There are also strong variations of the rotation rate ...
... The Sun rotates differentially, i.e. the solar rotation rate varies with both latitude and radius. The differential rotation is particularly prominent in the convection zone where equatorial zones rotate almost 30% faster than near-polar regions. There are also strong variations of the rotation rate ...
A novel mechanism for electron-cyclotron maser
... Another important instability driven by a fast electron beam is the Langmuir wave (LW) instability, which usually has a much faster growth rate than that of the AW instability. However, this does not imply that the LW instability is more important than the AW instability. The propagation of the LW c ...
... Another important instability driven by a fast electron beam is the Langmuir wave (LW) instability, which usually has a much faster growth rate than that of the AW instability. However, this does not imply that the LW instability is more important than the AW instability. The propagation of the LW c ...
Winds from clusters with non-uniform stellar distribution
... in which the distribution of stars (i.e., the number of stars per unit volume) within the cluster is spherically symmetric, has a power-law radial dependence, and drops discontinuously to zero at the outer radius of the cluster. We carry out comparisons between an analytic model (in which the stars ...
... in which the distribution of stars (i.e., the number of stars per unit volume) within the cluster is spherically symmetric, has a power-law radial dependence, and drops discontinuously to zero at the outer radius of the cluster. We carry out comparisons between an analytic model (in which the stars ...
The Present Status of Chinese Study of Solar Eclipses
... harmonious in constellation Fang, the blind beat drums, junior officers galloped, people ran around…” Most people thought that it relates to a solar eclipse. Wu Shouxian (1998, 2000) carried out a thorough analysis of these earlier investigations. Fourteen different conclusions contained in them wer ...
... harmonious in constellation Fang, the blind beat drums, junior officers galloped, people ran around…” Most people thought that it relates to a solar eclipse. Wu Shouxian (1998, 2000) carried out a thorough analysis of these earlier investigations. Fourteen different conclusions contained in them wer ...
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 ( ...
Neutral Density and Crosswind Determination from
... The aerodynamic force coefficient vector Ca is a function of the satellite shape, its orientation with respect to the flow, and the nature of the aerodynamic interaction with the atmospheric particles. These aspects will be discussed further in the next paragraphs. The area Aref is a fixed reference va ...
... The aerodynamic force coefficient vector Ca is a function of the satellite shape, its orientation with respect to the flow, and the nature of the aerodynamic interaction with the atmospheric particles. These aspects will be discussed further in the next paragraphs. The area Aref is a fixed reference va ...
Electric Currents – The Key to Magnetic Fields
... Regardless of the direction of the main driving current coming into the Sun, the elevenyear reversal of the magnetic loops can be explained by transformer action as shown above. If the main magnetic field that induces the surface currents is growing in strength, the surface current will point in one ...
... Regardless of the direction of the main driving current coming into the Sun, the elevenyear reversal of the magnetic loops can be explained by transformer action as shown above. If the main magnetic field that induces the surface currents is growing in strength, the surface current will point in one ...
STELLAR ABLATION OF PLANETARY ATMOSPHERES
... atmospheric evolution to which solar photon or solar wind ablation or erosion must have contributed. Mercury barely has an exosphere [Hunten et al., 1988]. Venus’ atmosphere has been desiccated of water [Kasting, 1988]. Mars has lost most of an atmosphere that increasingly appears to have contained ...
... atmospheric evolution to which solar photon or solar wind ablation or erosion must have contributed. Mercury barely has an exosphere [Hunten et al., 1988]. Venus’ atmosphere has been desiccated of water [Kasting, 1988]. Mars has lost most of an atmosphere that increasingly appears to have contained ...
extrasolar planets
... The End of Planet Formation • Rocks, metals & ices go into solid bodies (planets, asteroids & comets). • H & He gas amount to 98% of the mass of the nebula. – Some gas locked up in the Jovian planets. – The rest is blown away by the young solar wind or evaporated by Sunʼs radiation. ...
... The End of Planet Formation • Rocks, metals & ices go into solid bodies (planets, asteroids & comets). • H & He gas amount to 98% of the mass of the nebula. – Some gas locked up in the Jovian planets. – The rest is blown away by the young solar wind or evaporated by Sunʼs radiation. ...
Magnetic Reconnection Project
... • Can plasmoids produce fast MHD reconnection in the corona? Daughton et al ‘09 Bhattacharjee et al. (2009) Cassak et al. (2009) Uzdensky et al. (2010) Shepherd and Cassak (2010) Huang et al (2011) ...
... • Can plasmoids produce fast MHD reconnection in the corona? Daughton et al ‘09 Bhattacharjee et al. (2009) Cassak et al. (2009) Uzdensky et al. (2010) Shepherd and Cassak (2010) Huang et al (2011) ...
Real Properties of Electromagnetic Fields and
... zero valued (B is “solenoidal”), some recent statements are equivocal on this point. “Magnetic field lines can exist in two types: closed and open. A closed magnetic field line is anchored at two points in the photosphere and extends into the corona as a loop or arch. This explains the shape of sola ...
... zero valued (B is “solenoidal”), some recent statements are equivocal on this point. “Magnetic field lines can exist in two types: closed and open. A closed magnetic field line is anchored at two points in the photosphere and extends into the corona as a loop or arch. This explains the shape of sola ...
Orbital effects of Sun`s mass loss and the Earth`s fate
... I deal with the topic of determining the classical orbital effects induced by an isotropic variation Ṁ /M of the mass of a central body on the motion of a test particle; my analysis is also valid for a change Ġ/G of the Newtonian constant of gravitation. This problem, although interesting in itsel ...
... I deal with the topic of determining the classical orbital effects induced by an isotropic variation Ṁ /M of the mass of a central body on the motion of a test particle; my analysis is also valid for a change Ġ/G of the Newtonian constant of gravitation. This problem, although interesting in itsel ...
Investigation of mass flows in the transition region and corona in a
... active region, spatially scaled down by a factor of five, and another one from a quiet Sun area. Thus, the resulting magnetic map represents the quiet Sun with some activity added by a pore and is supposed to be typical for the magnetic field underlying the transition region of the Sun outside activ ...
... active region, spatially scaled down by a factor of five, and another one from a quiet Sun area. Thus, the resulting magnetic map represents the quiet Sun with some activity added by a pore and is supposed to be typical for the magnetic field underlying the transition region of the Sun outside activ ...
Solar Weather Event Modelling and Prediction
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
... indicating that the results obtained from ANN are in good agreement with the actual values. To date, such an approach seems to be the most promising and is widely used in prediction systems e.g. for sunspots and flares, as reported in Sects. 4.1.3 and 4.2.2. The chaotic nature of the Sun as a comple ...
Potential for Life on the Terrestrial Planets
... fluxes result in higher exospheric temperatures and more expanded thermosphereexosphere environments and, hence, suffer stronger atmospheric erosion, which may result in the total loss of several hundred bars even if an exoplanet is protected by a “magnetic shield” with its boundary located at one E ...
... fluxes result in higher exospheric temperatures and more expanded thermosphereexosphere environments and, hence, suffer stronger atmospheric erosion, which may result in the total loss of several hundred bars even if an exoplanet is protected by a “magnetic shield” with its boundary located at one E ...
Experimental_Neutrino_Physics
... implies accessible minimum mass (∝ Δm213) within reach of next generation ...
... implies accessible minimum mass (∝ Δm213) within reach of next generation ...
ICP-MS and Planetary Geosciences
... region of interstellar space where the Sun formed. For example, the variability of the amount of 60 Fe and 26 Al (both are short-lived, now extinct, isotopes) might conceivably mean that 60 Fe was added to our Solar System a million years after it formed, but when the solar nebula was still present. ...
... region of interstellar space where the Sun formed. For example, the variability of the amount of 60 Fe and 26 Al (both are short-lived, now extinct, isotopes) might conceivably mean that 60 Fe was added to our Solar System a million years after it formed, but when the solar nebula was still present. ...
Wind-Blown Bubbles around Evolved Stars
... In these simulations, the stellar wind is injected in the form of a thermal energy and mass source in a small volume around the star, and for this reason temperatures in the unshocked stellar wind region are high but do not affect the dynamics since the flow is highly supersonic in this region. ...
... In these simulations, the stellar wind is injected in the form of a thermal energy and mass source in a small volume around the star, and for this reason temperatures in the unshocked stellar wind region are high but do not affect the dynamics since the flow is highly supersonic in this region. ...
ASTRONOMY AND ASTROPHYSICS Properties of solar pores
... visible lines of different formation heights, Thim (1993) finds 3.3 G km;1; the empirical model of Sütterlin (1991) predicts a gradient of 2-3 G km ;1. Theoretical models as well as observations show that the diameter of a pore increases with height in the atmosphere (Simon & Weiss 1970; Zirin & Wan ...
... visible lines of different formation heights, Thim (1993) finds 3.3 G km;1; the empirical model of Sütterlin (1991) predicts a gradient of 2-3 G km ;1. Theoretical models as well as observations show that the diameter of a pore increases with height in the atmosphere (Simon & Weiss 1970; Zirin & Wan ...
Skywave Excitement - Lake Area Radio Klub
... A possible benefit to radio communications resulting from periods of high geomagnetic activity is that the aurora that can reflect VHF signals. (G3A16) ...
... A possible benefit to radio communications resulting from periods of high geomagnetic activity is that the aurora that can reflect VHF signals. (G3A16) ...
Solar wind
![](https://commons.wikimedia.org/wiki/Special:FilePath/Solar_wind_Speed_interplanetary_magnetic_field.jpg?width=300)
The solar wind is a stream of charged particles released from the upper atmosphere of the Sun. This plasma consists of mostly electrons, protons and alpha particles with energies usually between 1.5 and 10 keV; embedded in the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar longitude. Its particles can escape the Sun's gravity because of their high energy, from the high temperature of the corona and magnetic, electrical and electromagnetic phenomena in it.The solar wind flows outward supersonically to great distances, filling a region known as the heliosphere, an enormous bubble-like volume surrounded by the interstellar medium. Other related phenomena include the aurora (northern and southern lights), the plasma tails of comets that always point away from the Sun, and geomagnetic storms that can change the direction of magnetic field lines and create strong currents in power grids on Earth.