This example demonstrates the inadequacy of spectral lines with widely separate peak temperatures for temperature diagnostic. The electron temperature and density estimated by the helium LIR measurement are about 10 times larger than that of the probe measurement, although the electron. We show that the temperatures derived using the line ratio technique for these two spectral lines can vary by more than 0.8 x 10(exp 6) K due to the contribution from surrounding regions. using daily intensity measurements at 1.15 Rs of the Fe XIV 5303 A and Fe X 6374 A spectral lines carried out at the National Solar Observatory at Sacramento Peak. 11 A number of groups estimate excitation temperature12 from ratio of relative intensity of atomic lines in suggestion that this value is similar to electrons. In this paper we investigate the effect of these surrounding regions on coronal hole temperatures. Even large coronal holes present at the solar poles at solar minimum can be partly or completely obscured by emission from hotter and denser surrounding regions. The corona, however, is far from homogeneous. In a homogeneous plasma the line ratio technique can be used for any two lines if the ratio of the intensities is independent of the density. The specic peaks obtained from the optical emission spectra were selected to accurately calculate the electron temperature. These transitions all produce light in the visible part of the spectra. The obtained optical emission spectra of the plasma jet generated in the system were analyzed to estimate the electron temperature. The Balmer emission lines correspond to transitions from the levels for which n is greater than or equal to 3 down to the level for which n 2. Total Mo and Te are kept in a stoichiometric 2:1 ratio with sufficient MoCl 5 to achieve a Cl density of. The transitions, which are responsible for the emission lines of the Balmer, Lyman, and Paschen series, are also shown in Fig. Since the white-light intensity is proportional to the electron density. The purity of the source materials are Mo 99.9, Te 99.997 and MoCl 5 95 (Sigma Aldrich). The temperatures chosen are close to the peak line formation temperature for these lines, which are 10 6.27, 10 6.1, and 10 6.2 K for 5,303. Room-temperature spectra are compared with laboratory measurements and data. Demonstrating the limitations of line ratio temperature diagnostic using Fe X and Fe XIV spectral line intensity observations The electron temperature in the inner corona can be derived from spectral line intensity measurements by comparing the ratio of the measured intensities of two spectral lines to the ratio calculated from theoretical models. The emission lineintensity ratios give an estimate of the temperature. line intensity ratio gives an electron temperature of 3.4 x 10 6 K.
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