Hostname: page-component-5cf477f64f-zrtmk Total loading time: 0 Render date: 2025-04-04T05:35:45.115Z Has data issue: false hasContentIssue false
  • English
  • Français

The X-Ray Corona and the Photospheric Magnetic Field

Published online by Cambridge University Press:  14 August 2015

A. S. Krieger ,
G. S. Vaiana  and
L. P. Van Speybroeck
A. S. Krieger
Affiliation:
American Science and Engineering, Cambridge, Mass., U.S.A.
G. S. Vaiana
Affiliation:
American Science and Engineering, Cambridge, Mass., U.S.A.
L. P. Van Speybroeck
Affiliation:
American Science and Engineering, Cambridge, Mass., U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Soft X-ray (3–60 Å) photographs of the solar corona have been obtained on four flights of a rocket-borne grazing incidence telescope having a resolution of a few arc seconds. The configuration of the X-ray emitting structures in the corona has been compared to the magnetic field distribution measured by photospheric longitudinal magnetograms. The X-ray structures trace the three dimensional configuration of the magnetic field through the lower corona.

Active regions in the corona take the form of tubular structures connecting regions of opposite magnetic polarity within the same or adjacent chromospheric active regions.

Higher, larger structures link widely separated active regions into complexes of activity covering substantial fractions of the disk. The complexes are separated by areas of low average field in the photosphere. Interconnections across the solar equator appear to originate over areas of preceding polarity.

Enhanced X-ray emission is observed, outside the active belt, over areas of enhanced general magnetic field. Bright point-like X-ray features are observed above bipolar areas in the general coronal field.

Two, probably related, classes of X-ray features are associated with points of high field gradient along the longitudinal magnetic, ‘neutral line’. Both in the non-flaring active region and in flares the brightest emission is observed from one or more small line sources (at our present resolution). In flares this can account for a substantial fraction of the total soft X-ray emission of the flare.

Type
Part IV: Observations of Magnetic Fields Associated with Flares and Other Transitory Phenomena
Information
Symposium - International Astronomical Union , Volume 43: Solar Magnetic Fields , 1971 , pp. 397 - 412
Copyright
Copyright © Reidel 1971 

References

Babcock, H. W.: 1961, Astrophys. J. 133, 572.CrossRefGoogle Scholar
Bumba, V. and Howard, R.: 1965, Astrophys. J. 141, 1502.CrossRefGoogle Scholar
Giacconi, R., Reidy, W., Vaiana, G., VanSpeybroeck, L., and Zehnpfennig, T.: 1969, Space Sci. Rev. 9, 3.CrossRefGoogle Scholar
Livingston, W., Harvey, J., and Slaughter, C.: 1970, Nature 226, 1146.CrossRefGoogle Scholar
Newkirk, G. and Lacey, L.: 1970, Nature 226, 1098.CrossRefGoogle Scholar
Solar-Geophysical Data Bulletin : 1970, Environmental Science Services Administration, U.S. Dept. of Commerce, Boulder, Colo., IER-FB-309.Google Scholar
Vaiana, G., Reidy, W., Zehnpfennig, T., VanSpeybroeck, L., and Giacconi, R.: 1968, Science 161, 564.CrossRefGoogle Scholar
Vaiana, G. and Giacconi, R.: 1969, in Plasma Instabilities in Astrophysics , (ed. by Tidman, D. A. and Wentzel, D. G.), Gordon and Breach, N.Y., p. 91.Google Scholar
Van Speybroeck, L. P., Krieger, A. S., and Vaiana, G. S.: 1970, Nature 227, 818.CrossRefGoogle Scholar