Solar and Space Physics Space Science in the Twenty-First Century -- Imperatives for the Decades 1995 to 2015 (1988) / Chapter Skim
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2. Scientific Objectives
2. Scientific Objectives
Pages 7-16
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From page 7... ...
This discovery has made ~helioseismology" possible, by which the depth of the convective zone and the rotation below the photosphere have been inferred. In addition, by ruling out the classical model of coronal heating by acoustic waves, observations from the ground and from OSO-8 raised anew the question of what maintains the corona's high temperature.
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From page 8... ...
Skylab observations unambiguously identified magnetic arches as the basic structure of coronal flares. This perception altered our theoretical picture of solar flares and clarified the need for a coordinated multiinstrument attack, which was initiated with the Solar Maximum Mission.
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From page 9... ...
~ ~q:_ ~ How Does Solar Plasma / Interact with Strong Magnetic Fields7 How Is Solar Flare Energy Released ? C SOLAR PHYSICS—R ECU I R ED MEASU R EMENTS How Is Solar Wind Generated?
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From page 10... ...
Currents flowing along the Earth's magnetic field and connecting the polar ionosphere to the magnetosphere were found to create strong localized electric fields at high altitudes. These fields may accelerate the electrons responsible for intense terrestrial radio bursts and
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From page 11... ...
A collisionless bow shock stands upstream of the magnetopause, the boundary separating shocked solar wind from the magnetosphere proper. The Moon is 60 earth radii from the Earth; the Earth's magnetic tail is thought to extend some thousand earth radii downstream.
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From page 12... ...
The catalytic reactions of odd hydrogen, nitrogen, and chlorine compounds destroy ozone, thereby altering the absorb tion of solar ultraviolet radiation. Results from three Atmospheric Explorers, which largely quantified the photochemistry of the thermosphere and ionosphere, also illustrate the strength of the electrodynam~c coupling of the thermosphere to the magnetosphere.
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From page 13... ...
Solar ultraviolet photons deposit their energy largely in the stratosphere and above. The magnetosphere interacts with the upper atmosphere both through energetic plasma deposition and through electric fields, which are generated by magnetospheric motions.
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From page 14... ...
~ Provide, to the extent possible, simultaneous measurements on many links in the chain of interactions coupling solar perturbations to their terrestrial response. Create and test increasingly comprehensive quantitative Whereas 10 years ago it was generally believed that significant effects of solar variability penetrate only as far as the upper atmosphere, some scientists now believe that they also reach the lower atmosphere and so affect weather and climate in ways not yet completely understood.
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From page 15... ...
COMPARATIVE PLANETARY STUDIES Comparative studies of the interaction of the solar wind with planets and comets highlight the physics pertinent to each and put solar-terrestrial interactions in a broader scientific context. The solar system has a variety of magnetospheres sufficient to make their comparative study fruitful.
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From page 16... ...
16 ~ Secrete our underst~dlog of rapidly rotating magneto spheres Evolving strong stmospberic ~d sateDite interactions. ~ Determine the role of at~spberes in substor~ Id other magnetospber~ processes by orbits studies ~ ~e~ury-tbe only known m~ne~zed planet without ~ dyn~caDy d~c~t Tam sphere.
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