Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-12T09:37:29.925Z Has data issue: false hasContentIssue false
  • English
  • Français

Statistical Features of the Quiet Sun in EUV

Published online by Cambridge University Press:  13 May 2016

A. Pauluhn ,
S. K. Solanki ,
I. Rüedi ,
E. Landi  and
U. Schühle
A. Pauluhn
Affiliation:
INTEC HTA Bern and Inst. of Astronomy, ETH Zürich, Switzerland
S. K. Solanki
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany
I. Rüedi
Affiliation:
Physikalisch Meteorologisches Observatorium, World Radiation Center Davos, Switzerland
E. Landi
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany
U. Schühle
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany

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.

Frequency distributions of the intensities of EUV emission lines in the quiet Sun have in the past usually been modelled using two Gaussians. Here we test this and other distribution functions against observed distributions with exceptional statistics. The data were obtained in a number of spectral lines observed with CDS and SUMER. We show that the frequency distribution of the radiance is best modelled by a lognormal distribution. The fact that the radiance distribution of the quiet Sun including the network and the intranetwork is better reproduced by a single lognormal distribution function than by two Gaussians suggests that the same heating processes are acting in both types of features.

Type
Session IV: Structure and Dynamics of the Transiton Region and Corona
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 416 - 418
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Bocchialini, K., Vial, J.-C., & Einaudi, G., 1997, 5 th SOHO Worksh., Oslo, ESA SP-404, 211.Google Scholar
Dammasch, I.E., Hassler, D.M., Curdt, W., & Wilhelm, K., 1999, Space Sci. Rev. 87, 161.CrossRefGoogle Scholar
Gallagher, P.T., Phillips, K.J.H., Harra-Murnion, L.K., & Keenan, F.P., 1998, A&A 335, 733.Google Scholar
Griffiths, N.W., Fisher, G.H., Woods, D.T., & Siegmund, O.H.W., 1999, ApJ 512, 992.CrossRefGoogle Scholar
Huber, M.C.E., Foukal, P., Noyes, R.W. et al., 1974, ApJ 194, L115.CrossRefGoogle Scholar
Lemaire, P., Wilhelm, K., Curdt, W. et al., 1997, Sol. Phys. 170/1, 105.CrossRefGoogle Scholar
Pauluhn, A., Rüedi, I., Solanki, S.K. et al., 1999, Appl. Optics 38, No. 34, 7035.CrossRefGoogle Scholar
Pauluhn, A., Solanki, S.K., Rüedi, I., et al., 2000, to appear in A&A.Google Scholar
Reeves, E.M., Vernazza, J.E, Withbroe, G.L., 1976, Phil. Trans. R. Soc. London, Ser. A 281, 319.Google Scholar