Abstract
FROM observations of magnetic disturbances on the Earth, Bartels1 suggested the existence of M-regions on the Sun. Attempts have been made to associate these M-regions with other solar phenomena. Allen2 tried to show that coronal streams and M-regions are identical; he also concluded that M-regions avoid spot groups or are even destroyed by them. This conclusion was implicitly modified by the results of Denisse3 and Becker4. Identification of M-regions with regions of unusually weak corona emission was recently suggested by Bell and Glazer5. Kiepenheuer6 arrived at the conclusion that filaments are the possible source of M-disturbances. As a result of measurements of the solar magnetic field, Babcock and Babcock7 believed that the observed unipolar magnetic regions are M-regions. With these measurements M-regions may have ceased to be hypothetical in character. Whether or not this is so, it is still of interest to continue the study of M-regions relative to other solar phenomena.
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References
Bartels, J., Terr. Mag. Atm. Elect., 37, 48 (1932).
Allen, C. W., Mon. Not. Roy. Astro. Soc., 104, 13 (1944).
Denisse, J. F., C.R. Acad. Sci., Paris, 236, 1856 (1953).
Becker, U., J. Atm. Terr. Phys., 4, 70 (1954).
Bell, B., and Glazer, H., J. Geophys. Res., 61, 179 (1956).
Kiepenheuer, K. O., Astrophys. J., 105, 408 (1947).
Babcock, H. W., and Babcock, H. D., Astrophys. J., 121, 349 (1955).
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TOMAN, K. Identification of M-Regions on the Sun. Nature 181, 641–642 (1958). https://doi.org/10.1038/181641a0
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DOI: https://doi.org/10.1038/181641a0
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