Results 141 to 150 of about 1,410 (184)
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AIP Conference Proceedings, 2016
Turbulence in the solar wind is ubiquitous. To understand the transport of low-frequency turbulence in the sub- and super-Alfvenic solar wind flow, Zank et al. 2012 developed an extensive turbulence transport model that describes the evolution of the energy in forward and backward propagating modes, the total turbulent energy, the cross-helicity, the ...
L. Adhikari +5 more
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Turbulence in the solar wind is ubiquitous. To understand the transport of low-frequency turbulence in the sub- and super-Alfvenic solar wind flow, Zank et al. 2012 developed an extensive turbulence transport model that describes the evolution of the energy in forward and backward propagating modes, the total turbulent energy, the cross-helicity, the ...
L. Adhikari +5 more
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Astrophysics and Space Science, 2001
Launched in October 1990, the ESA-NASA Ulysses mission has conducted the very first survey of the heliosphere within 5 AU of the Sun over the full range of heliolatitudes. With polar passes taking place in 1994 and 1995, the timing of the mission has enabled Ulysses to characterise the global structure of the heliosphere at solar minimum, when the ...
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Launched in October 1990, the ESA-NASA Ulysses mission has conducted the very first survey of the heliosphere within 5 AU of the Sun over the full range of heliolatitudes. With polar passes taking place in 1994 and 1995, the timing of the mission has enabled Ulysses to characterise the global structure of the heliosphere at solar minimum, when the ...
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Space Science Reviews, 1995
A review is given of heliospheric radio emissions. Only radio emissions generated well away from the Sun (beyond a few solar radii) and well away from the magnetized planets are considered. These consist of (1) type III radio bursts, (2) type II radio bursts, and (3) heliospheric 2-3 kHz radio emissions.
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A review is given of heliospheric radio emissions. Only radio emissions generated well away from the Sun (beyond a few solar radii) and well away from the magnetized planets are considered. These consist of (1) type III radio bursts, (2) type II radio bursts, and (3) heliospheric 2-3 kHz radio emissions.
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The STEREO heliospheric imager: how to detect CMEs in the heliosphere
Advances in Space Research, 2005Abstract The STEREO Heliospheric Imager is a wide-angle imaging system that will enable, for the first time, a view of Earth-directed coronal mass ejections (CMEs) in a field of view which also encompasses the Earth. Twin views from widely spaced platforms, combined with the out of Sun–Earth line perspective allow a unique and powerful tool for the ...
R.A. Harrison, C.J. Davis, C.J. Eyles
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1998
In explaining and describing the forces that shape the bubble of solar wind surrounding the Sun, there is a dearth of information. But observations from space are alleviating this situation. Three spacecraft moving away from the Sun-Pioneer 10 and Voyagers 1 and 2-are expected to penetrate the boundaries of the heliosphere within the next few years ...
Axford, W., Suess, S.
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In explaining and describing the forces that shape the bubble of solar wind surrounding the Sun, there is a dearth of information. But observations from space are alleviating this situation. Three spacecraft moving away from the Sun-Pioneer 10 and Voyagers 1 and 2-are expected to penetrate the boundaries of the heliosphere within the next few years ...
Axford, W., Suess, S.
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Space Science Reviews, 2011
The paleo-cosmic ray records are used to study the properties of the heliosphere and solar processes over the past 9300 years. They show that both varied greatly over that time, ranging from ∼26 “Grand Minima” of duration 50–100 yr when the Sun was inactive, to periods similar to the past 50 years of strong solar activity.
Ken McCracken +3 more
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The paleo-cosmic ray records are used to study the properties of the heliosphere and solar processes over the past 9300 years. They show that both varied greatly over that time, ranging from ∼26 “Grand Minima” of duration 50–100 yr when the Sun was inactive, to periods similar to the past 50 years of strong solar activity.
Ken McCracken +3 more
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Is the heliospheric interface submagnetosonic? Consequences for the LISM presence in the heliosphere
Advances in Space Research, 1986Abstract Based on our best knowledge of the physical parameters of the LISM, one comes to the conclusion that for the solar system a submagnetosonic configuration of the plasma interface between the LISM and the expanding solar wind plasma is established extending to some 1000 AU distance upwind from the sun.
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2014
The Sun is our star. It provides the energy that makes life’s existence on Earth possible. The main zones of the observed Sun are the photosphere, chromosphere, and corona. Their composition, structure, and peculiarities are intrinsically related with the interior where nuclear fusion occurs. Solar activity includes an 11-year solar cycle and different
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The Sun is our star. It provides the energy that makes life’s existence on Earth possible. The main zones of the observed Sun are the photosphere, chromosphere, and corona. Their composition, structure, and peculiarities are intrinsically related with the interior where nuclear fusion occurs. Solar activity includes an 11-year solar cycle and different
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Physics Today, 2013
Voyager 1, launched in 1977, has documented its traversal of the abrupt boundary that separates the Sun's domain from interstellar space. Voyager 1, launched in 1977, has documented its traversal of the abrupt boundary that separates the Sun's domain from interstellar space.
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Voyager 1, launched in 1977, has documented its traversal of the abrupt boundary that separates the Sun's domain from interstellar space. Voyager 1, launched in 1977, has documented its traversal of the abrupt boundary that separates the Sun's domain from interstellar space.
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2010
Most of astrophysical shocks are collisionless, where the collective electromagnetic interaction plays the essential role in the dissipation process and results in a large deviation of particle phase-space distribution from the thermal equilibrium. An ideal laboratory for collisionless shocks is the heliosphere, in which shocks are formed ahead of ...
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Most of astrophysical shocks are collisionless, where the collective electromagnetic interaction plays the essential role in the dissipation process and results in a large deviation of particle phase-space distribution from the thermal equilibrium. An ideal laboratory for collisionless shocks is the heliosphere, in which shocks are formed ahead of ...
openaire +1 more source