THE FORMATION OF SUNSPOTS AND SOLAR MAGNETIC FIELDS. PART I
Arguments are given to show that the magnetic fields of sunspots represent a local intensification of the general solar field. It is suggested that the field of a bipolar spot group (active region) is generated by large- scale convective mass motion in the subphotospheric layers. A system of toroidal fields is formed as each convective element rises and an adjacent region of plasma sinks in the general solar field. The fields arise from inductive currents, and lie in a vertical plane parallel to the solar field and containing the convective element. Upon emerging at the solar surface, the magnetic fields of many convective elements combine to form the field of a bipolar spot group. Their structure agrees with the observations of Stepanov and Bumba, who find that the field of each spot has two polarities. The field strength of the convective elements is estimated. Fields of 10/sup 3/ to 10/sup 4/ gauss can form if the initial field is 50 gauss and the convective cells (10/sup 9/ cm across) ascend at a rate of 10/sup 3/--10/sup 4/ cm/sec for a period of 10/sup 6/-10/sup sec. (auth)
- Research Organization:
- Kiev Univ. Observatory
- NSA Number:
- NSA-18-004391
- OSTI ID:
- 4125558
- Journal Information:
- Soviet Astron.-AJ (English Transl.), Vol. Vol: 7; Other Information: Orig. Receipt Date: 31-DEC-64
- Country of Publication:
- Country unknown/Code not available
- Language:
- English
Similar Records
Relations between the toroidal magnetic field in the solar convection zone and the bipolar magnetic field of sunspots
δ-SUNSPOT FORMATION IN SIMULATION OF ACTIVE-REGION-SCALE FLUX EMERGENCE