Titlebook: Solar and Interplanetary Dynamics; M. Dryer,E. Tandberg-Hanssen Book 1980 International Astronomical Union 1980 Variation.astrophysics.cos

limber

Dynamics of Large-Scale Magnetic Field Evolution During Solar Cycle 204. The results include: a unique magnetic pattern coinciding with major coronal holes; variations in the rate of solar rotation through the solar cycle; discovery of convergence and divergence among long-lived magnetic patterns; periodic discontinuities in the organization of large-scale magnetic fi

intrude

A Two-Level Solar Dynamo Based on Solar Activity, Convection, and Differential Rotation both located in the high β regime convection zone. . requires that regime, since its function demands it be driven by mechanical forces. But the function and therefore the operating requirements of . are entirely different, and there seems to be no à . reason, other than historical tradition couple

disrupt

搖擺

Radio Observations of Coronal Holesreas of low brightness, either on the disk or at the limb. At 80 MHz holes on the limb always appear less bright than their surroundings but on the disk they frequently appear brighter..The simplest interpretation is that the coronal temperature in holes near the 80 MHz critical density (8 × 10. cm.

哪有黃油

A Model for the North Coronal Hole Observed at the 1973 Eclipse, Between 1.3 and 3.2 R⊙y-compensated filter. These pictures provide a very good opportunity for studying the large coronal hole at the north polar cap; this hole has been extensively studied during the Skylab period. On the plates of Koutchmy, we could record reliable intensities between 1.3 and 3.2 R . The absolute calib

橫截,橫斷

Solar Observations with a New Earth-Orbiting Coronagraphpproximately 1.25 arc min and a repetition rate of 10 minutes during the one-hour sunlit portion of each 97-minute satellite orbital period. These are the first satellite observations of the outer corona near the peak of a sunspot cycle when coronal transients and high-latitude streamers are common.

Afflict

MAOIS

The Origin of Interplanetary Sectorsoronal magnetic field from the observed photospheric magnetic field shed light on the origin of sectors. Figure 1 from Schatten’s (1971) “Current Sheet Model” is a schematic representation of these similar models. There are three distinct regions in these models where different physical phenomena oc

勤勞

Coronal Structure and Solar Windned through the focussing of solar-ion streams taking account of the local and general solar magnetic fields. This explains the association of coronal holes with weak, diverging open magnetic field lines and envisages the transfer of hydromagnetic wave energy from nearby active centers to account fo

legitimate