Morphology of the Quiet Solar Upper Atmosphere in the 4x10^4<T_e<1.4x10^6 K Temperature Regime

Details Morphology of the Quiet Solar Upper Atmosphere in the 4x10^4<T_e<1.4x10^6 K Temperature Regime Morphology of the Quiet Solar Upper Atmosphere in the 4x10^4<T_e<1.4x10^6 K Temperature Regime

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...522.1133f&link_type=abstract

The Astrophysical Journal, Volume 522, Issue 2, pp. 1133-1147.

Astronomy and Astrophysics

Astronomy

73

Sun: Abundances, Sun: Atmosphere, Sun: Transition Region

Scientific paper

Studies on the morphology of the solar upper atmosphere began over three decades ago. Early models assumed that the temperature structure of the solar upper atmosphere was continuous with a thin transition region connecting the chromosphere with the corona. Over the years it became apparent that the original depiction of the solar upper atmosphere was too simplistic. In this paper we present a morphological study of the solar upper atmosphere over a wide range of temperatures (4x10^4<=T_e<=1.4x10^6 K) using high-resolution images (1^''-2^'') taken by TRACE, the SUMER spectrometer on SOHO, and the NRL spectroheliograph on Skylab. The images clearly show that the 4x10^4<=T_e<=1.4x10^6 K temperature domain of the solar upper atmosphere consists of a hierarchy of isothermal loop structures. While at the T_e<8x10^5 K temperature regime the looplike structures are more abundant along the chromospheric network, at higher temperatures (T_e>9x10^5 K) no association between them and the chromospheric network is apparent. The hottest (T_e~1.4x10^6 K), which are also the longest among the quiet-Sun loop structures, form a canopy over the lower temperature loop structures. We discuss in the paper possible relationships between the morphology of the solar upper atmosphere, its elemental abundance, and ideas regarding the origin of the slow-speed solar wind.

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