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- W2560381807 abstract "A unique combination of photographic and K-coronameter data were used to study the structure and evolution of two known coronal streamers. In addition, two other K-coronameter enhancements were studied as representing ideal second examples of the known streamers. As a general rule the observations indicate that these features were direct coronal manifestations of photospheric bipolar magnetic regions (BMR) and were of two basic types: active region, by which is meant a coronal streamer which develops radially over a low-latitude active region; and helmet which denotes a streamer whose structure and development appear to be a consequence of a long-lived complex of activity, composed of both trailing magnetic fields and a parent center of disk activity. The similarity of growth rates during the first solar rotation of life led to derivation of a total streamer density of 4-5 l0 s cm -3 at r= 1.125 R| This density may represent a characteristic maximum density at the base of streamers. The intensity gradient of the inner (r ~< 1.5 R| corona was used to establish a qualitative evolutionary model of streamers which synthesizes the observations. Briefly, streamers initially develop over active regions; the streamer growth rate may be as rapid as the disk activity, or at worst lags flare activity by ~ �89 solar rotation. The streamer can be the cause of inter- planetary and geomagnetic effects at 1 AU within a solar rotation after birth. Thereafter the streamer follows an evolution dictated by the underlying solar magnetic fields. In any case the lowest level of the coronal enhancement has a lifetime not exceeding that of the solar disk activity." @default.
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- W2560381807 date "1970-01-01" @default.
- W2560381807 modified "2023-09-26" @default.
- W2560381807 title "II: Evolution of Discrete Features from the Sun to 1 AU" @default.
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