Hostname: page-component-669899f699-vbsjw Total loading time: 0 Render date: 2025-04-25T11:24:28.421Z Has data issue: false hasContentIssue false
  • English
  • Français

Properties of Faculae from Observations Near the Opacity Minimum

Published online by Cambridge University Press:  03 August 2017

P Foukal  and
T Moran
P Foukal
Affiliation:
CRI, Inc., 21 Erie Street, Cambridge, MA 02139, U.S.A.
T Moran
Affiliation:
NASA/Goddard Space Flight Center, Greenbelt, MD 20771, 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.

Imaging of active regions in continuum around 1.6 μm shows that many facular regions are less bright than the photosphere when observed nearer to disk center than μ = cos θ ~ 0.75. The contrast of these dark faculae increases with magnetic flux above a threshold of approximately 2 × 1018 Mx. This explains why not all faculae are dark at 1.6 μm, since the magnetic flux density in many regions of bright Ca K plage emission falls below this threshold. After correction for blurring, the typical contrast value is about 4-5%, so the brightness temperature deficit is about 130 K. Faculae are brighter than the photosphere at 1.63 μm nearer to the limb than μ ~ 0.5. The negative contrast of dark faculae may arise from cooling of the surrounding photosphere, or from increased visibility of cool layers of the facular flux tube itself. Quantitative comparison of these IR data with MHD models awaits calculation of flux tube contrasts at realistic angular resolution.

Keywords

infrared: starsMHDSun: faculae, plagesSun: photosphere
Type
Part 1: Infrared Diagnostics of the Solar Atmosphere and Solar Activity
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 23 - 27
Copyright
Copyright © Kluwer 1994 

References

Ayres, T.: 1989, Solar Phys. 124, 15.Google Scholar
Chapman, G.: 1984, Astrophys. J. 232, 923.Google Scholar
Deinzer, W., Hensler, G., Schüssler, M., and Weisshaar, E.: 1984, Astron. Astrophys. 139, 435.Google Scholar
Elste, G.: 1985, in Theoretical Problems in High Resolution Solar Physics, ed. Schmidt, H., MPA Report 212, p. 185.Google Scholar
Foukal, P., and Duvall, T.: 1985, Astrophys. J. 296, 739.Google Scholar
Foukal, P., Little, R., Graves, J., Rabin, D., and Lynch, D.: 1990, Astrophys. J. 353, 712.Google Scholar
Foukal, P., Little, R., and Mooney, J.: 1989, Astrophys. J. (Letters) 336, 33.Google Scholar
Knölker, M., and Schüssler, M.: 1988, Astron. Astrophys. 202, 275.Google Scholar
Lawrence, J., Chapman, G., and Herzog, A.: 1988, Astrophys. J. 324, 1184.Google Scholar
Moran, T., Foukal, P., and Rabin, D.: 1992, Solar Phys. 142, 35.Google Scholar
Müller, R.: 1975, Solar Phys. 45, 105.Google Scholar
Spruit, H.: 1976, Solar Phys. 50, 269.Google Scholar
Vernazza, J., Avrett, E., and Loeser, R.: 1976, Astrophys. J. Suppl. 30, 1.Google Scholar
Walton, S.: 1987, Astrophys. J. 312, 909.Google Scholar
Wang, H., and Zirin, H.: 1987, Solar Phys. 110, 281.Google Scholar
Worden, P.: 1975, Solar Phys. 45, 521.Google Scholar
Zirin, M., and Wang, M.: 1992, Astrophys. J. (Letters) 385, 27.Google Scholar