Titlebook: Basic Mechanisms of Solar Activity; V. Bumba,J. Kleczek Book 1976 International Astronomical Union 1976 Corona.Main sequence.Photosphere.R

浮夸

Large-Scale Solar Magnetic Fieldserent role or visibilility of structures in both polarities is discussed. The reflection of both main types of the longitudinal distribution of large-scale solar background magnetic fields (the 27-day, the 28–29-day successions, the ‘supergiant’ structures) in the interplanetary magnetic field distribution is also considered.

Suggestions

Velocities Observed in Supergranulesoints. These observations suggest that surface motions do not exhibit the detailed flux redistribution expected in the random-walk diffusion of magnetic fields. It is suggested that the surface motions are only the reflection of magnetic field-convective motion interactions which occur deeper in the convection zone.

Glaci冰

Coronal Bright Pointsntified in X-ray photographs are seen as small (5?10″) emission features in ground-based H. and Ca K spectroheliograms as well as in transition region lines observed in other Skylab instruments. Typical bright point temperatures are 1.5?2×10. K and typical densities are ~ 5×10. cm..

Intuitive

窩轉(zhuǎn)脊椎動(dòng)物

Differential Rotation and Giant Cell Circulation of the Solar Ca+ -Network solar differential rotation and to search for giant cell circulation pattern. Details of the observing method and the results from observations during 1974 have been pub-lished very recently (Schr?ter and W?hl, 1975). Our method consists of measuring the position of 5–15 bright Ca.-mottles with res

愛(ài)國(guó)者

Rotational Characteristics of Coronal Holesonal hole area time series provide synodic rotation periods which indicate an almost rigid rotation by such features for lag lengths as short as one rotation. The rotation periods of coronal holes at high latitudes best compare with inferred interplanetary field rotation periods.

fiction

Large-Scale Solar Magnetic Fieldsore than 15 years of observations are given. The major part of our information concerns the morphology and only some results deal with the kinematics of the field distribution. Results of averaged solar magnetic field fluxes and polarity reversal studies as well as of preliminary investigation of th

打火石

贊美者

Investigation of Coronal Rotation by the Spectroscopic Methodear velocity by 0.4 km s. on the latitude and its relative constancy in the latitude interval 35° < . < 50° are the most typical..In the southern polar region an intensive stream of coronal gas directed oppositely to the solar rotation was detected during the time interval 1969–1972. In the greater