Spectroscopic increase of the flux from the solar temperature minimum region between the minimum-activity epochs 1984-87 and 1995-98. <p> HR: <span class="hr"> 11:25h<br></span> AN: <span class="an"> SH31C-05 INVITED <a href="../absbook/fm03-SH31C.pdf">[PDF]</a><br></span> TI: <span class="ti"> Spectroscopic increase of the flux from the solar temperature minimum region between the minimum-activity epochs 1984-87 and 1995-98. <br></span> AU: <span class="au"> * Livingtson, W C<br></span> EM: <span class="em"> wlivingtson@nso.edu<br></span> AF: <span class="af"> National Solar Observatory, POB 26732, Tucson, AZ 85726 <br></span> AU: <span class="au"> Avrett, E H<br></span> EM: <span class="em"> eavrett@spd.aas.org<br></span> AF: <span class="af"> Harvard-Smithsonian CfA, 60 Garden St, Cambridge, MA 02138 <br></span> AB: <span class="ab"> The photosphere is the visible surface of the Sun, the source of the continuous radiation that constitutes over 99% of the energy measured by spacecraft radiometers such as ACRIM. The temperature decreases with height in the photosphere out to a minimum region and then begins to increase in the chromosphere. The cores of the strong Fraunhofer absorption lines are formed just above the temperature minimum region. They do not have emission cores because of scattering effects. The weaker Fraunhofer lines are formed at and below the temperature minimum region. Since 1980 we have used the 1-meter Fourier Transform Spectrometer (FTS) on Kitt Peak to monitor the solar irradiance spectrum, and in particular, the line-center fluxes of the strong Sodium D and Magnesium b lines and 22 other weaker lines, mostly due to iron. A unique feature of this FTS instrument and its feed optics is that, over this 23 year interval, nothing, to our knowledge, has been changed or modified in any way. The central fluxes of all of the above lines decreased between the 1980 activity maximum and the 1986 minimum, as expected, and then increased as active regions again appeared on the disk. In 1990, however, as solar activity began to diminish, the Fraunhofer line fluxes continued to increase. They did not return to their 1986 minimum values during the 1996 minimum. Instead, the central fluxes of the strong lines increased by 10-15%. We have not found any instrumental effects that might account for this result. Preliminary quiet-Sun model calculations indicate that a temperature rise of a few hundred K in the temperature minimum region could account for such increases. However, the Ca K-index (residual flux in a 1-\AA~passband at the Ca II line center) was the same in 1996 as in 1986, and this places severe constraints on possible increases of quiet-Sun temperatures. Both the Fraunhofer and Ca II line observations represent line-to-continuum ratios, with the various lines and continua formed at different depths. We are investigating whether any combination of temperature variations at different depths might account for these observations. We note that the Willson and Mordvinov composite Total Solar Irradiance (TSI) signal indicated increased output from the Sun in 1995-98 compared to 1984-87. We hope to find an explanation for the Fraunhofer line increases between these two epochs, and, if so, to calculate the corresponding TSI change that would be expected. <br></span> DE: <span class="de"> 1650 Solar variability<br></span> SC: <span class="sc"> SPA - Solar and Heliospheric Physics [SH]<br></span> MN: <span class="mn"> 2003 Fall Meeting<br></span></p></body></html>