OBSERVATIONS OF DECAMETER CARBON RADIO RECOMBINATION LINES IN SEVERAL GALACTIC DIRECTIONS Part 2. ANALYSIS OF PHYSICAL CONDITIONS IN DIFFUSE CII REGIONS

Subject and Purpose. In Part 2 of the current paper, we seek to analyze the observational results of decameter carbon radio recombi- nation lines (RRLs) detected near the frequency 26 MHz through the UTR-2 radio telescope towards the S140 emission nebula and the GSH 139-03-69 super shell. These lines have proven themselves as a highly effective tool for cold, rarefied interstellar medium (ISM) diagnostics. The aim is to determine an association of line-forming regions (CII regions) with other ISM components and study physical conditions (electron temperature Te and electron density Ne) in these regions. Methods and Methodology. By iterative comparison of detected and modeled integral intensities of decameter carbon RRLs, we determine physical state ranges where recorded experimental data best fit the model values for various combinations of Te , Ne , and path lengths s. Results. It has been found that the characteristics of the detected decameter carbon RRLs are consistent with the higher-frequency data for both the S140 line of sight and other Galactic plane directions, including the GSH 139-03-69 direction. Ranges of physical con- ditions where recorded data and model values are in the best agreement have been determined, being Te 50 ÷ 100 K, Ne 0.01 cm–3, and s 10 pc — for the S140 nebula direction and its vicinity and, also, Te 50 ÷ 100 K, Ne 0.01 cm–3, and s 5 ÷ 7 pc — for the GSH 139-03-69 super shell direction. Conclusions. The obtained results indicate that the detected decameter carbon RRLs originate from CII regions associated with clouds of diffuse neutral hydrogen HI in the Galactic plane. The lines are seen against a background Galactic radio emission whose brightness temperature increases as frequency decreases.