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   <subfield code="a">Evolution of the Alfvénic correlation in the solar wind</subfield>
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   <subfield code="c">[R. Bruno, B. Bavassano]</subfield>
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   <subfield code="a">Summary: The radial evolution of Alfvénic correlation is such that its value decreases with increasing heliocentric distance. So far this behaviour has been interpreted as an increase in the local production of &lt;&lt;inward&gt;&gt; modes interacting destructively with the &lt;&lt;outward&gt;&gt; modes. This work, which deals with largescale turbulence, shows that local generation phenomena are not commonly found in the solar wind and that the Alfvénic character of the fluctuations mainly depend on the &lt;&lt;outward&gt;&gt; modes alone. The interaction of these modes with density and/or magnetic-field structures convected by the wind causes their destruction and a consequent depletion of the Alfvénic correlation. The same effect would be obtained if &lt;&lt;inward&gt;&gt; modes were really present. Our conclusions are that large-scale &lt;&lt;inward&gt;&gt; modes are the spectral counterpart of non-propagating field and plasma structures convected by the solar wind and identified as both compression regions and pressure balance structures.</subfield>
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   <subfield code="a">Società Italiana di Fisica, 1992</subfield>
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   <subfield code="u">Istituto di Fisica dello Spazio Interplanetario, CNR C.P. 27, 00044, Frascati, Roma, Italia</subfield>
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   <subfield code="t">Il Nuovo Cimento C</subfield>
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   <subfield code="g">15/5(1992-09-01), 599-605</subfield>
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