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Magnetic Fields, Oscillations, and Heating in the Quiet Sun Temperature Minimum Region from Ultraviolet Observations at 1600 Å

Published online by Cambridge University Press:  03 August 2017

J. W. Cook
J. W. Cook*
Affiliation:
E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC 20375, U.S.A.

Abstract

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The High Resolution Telescope and Spectrograph (HRTS) instrument has obtained broadband spectroheliograph images at 1600 Å of the solar temperature minimum region. I discuss HRTS observations of quiet areas and their relation with magnetic fields, five minute oscillations, and heating. The brightness temperature of solar fine structure elements composing the supergranular network is found to be linearly proportional to the local absolute value of magnetic field strength. There is evidence for a 250-s period oscillation occurring in 10-arcsec scale patches, which however is energetically unimportant to the local heating budget. A general nonmagnetic background heating and five minute oscillations occur globally, while the network bright points occur in magnetic regions, heated perhaps from partial dissipation of Alfvén waves (whose energy flux is linearly proportional to B) in individual elemental 1500-G (at the photosphere) flux tubes which expand to form the temperature minimum fine structure bright points.

Keywords

flux tubesinfrared:starsSun: magnetic fieldsSun: UV radiation
Type
Part 3: Infrared Perspectives on Atmospheric Dynamics
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 287 - 294
Copyright
Copyright © Kluwer 1994 

References

Anderson, L.S., and Athay, R.G.: 1990, Astrophys. J. 346, 1010.Google Scholar
Ayres, T.R., and Brault, J.W.: 1990, Astrophys. J. 363, 705.Google Scholar
Cook, J.W.: 1991, in Ulmschneider, P., Priest, E.R., and Rosner, R. (eds.), Mechanisms of Chromospheric and Coronal Heating, Springer, Berlin, p. 83.Google Scholar
Cook, J.W., Brueckner, G.E., and Bartoe, J.-D.F.: 1983, Astrophys. J. (Letters) 270, L89.Google Scholar
Cook, J.W., and Ewing, J.A.: 1990, Astrophys. J. 355, 719.Google Scholar
Cook, J.W., and Ewing, J.A.: 1991, Astrophys. J. 371, 804.CrossRefGoogle Scholar
Cook, J.W., Ewing, J.A., and Sutton, C.S.: 1988, Pub. A.S.P. 100, 402.Google Scholar
Dame, L., Gouttebroze, P., and Malherbe, J.-M.: 1984, Astron. Astrophys. 130, 331.Google Scholar
Lindsey, C.: 1993, these proceedings and private communication.Google Scholar
Lindsey, C., and Roellig, T.: 1987, Astrophys. J. 313, 877.Google Scholar
Noyes, R.W., and Hall, D.N.: 1972, Astrophys. J. (Letters) 176, L89.CrossRefGoogle Scholar
Sheeley, N.R. Jr., Bohlin, J.D., Brueckner, G.E., Purcell, J.D., Scherrer, V., and Tousey, R.: 1975, Solar Phys. 40, 103.CrossRefGoogle Scholar
Title, A., Tarbell, T., Topka, K., Cauffman, D., Balke, C., and Scharmer, G.: 1990, in Russell, C.T., Priest, E.R., and Lee, L.C. (eds.), Physics of Magnetic Flux Ropes, American Geophysical Union, Washington, p. 171.Google Scholar
Title, A.M., Tarbell, T.D., Topka, K.P., Ferguson, S.H., Shine, R.A., and the SOUP Team: 1989, Astrophys. J. 336, 475.CrossRefGoogle Scholar
Vernazza, J.E., Avrett, E.H., and Loeser, R.: 1981, Astrophys. J. Suppl. 45, 635.Google Scholar