Abstract
Proton transfer and condensation reactions followed by dissociative electron recombination and charge transfer processes may yield a significant concentration of PO in interstellar clouds. Relevant terrestrial PO lines in the ultraviolet, infrared and microwave regions are listed in order to aid the detection of PO in interstellar clouds. Within the framework of Klein-Dunham potential, spontaneous emission rates and oscillator strengths of strong (Δv=0 sequence) beta bands of the PO molecule are estimated. For SgrB2 source, under optically thin case, each of the two strongest2π1/2,J=2.5−1.5 rotational transitions (108.998 GHz and 109.206 GHz) of PO would have antenna temperature less than 125 mk for beam efficiency∼0.6 and μ=0.7D (electric dipole moment of PO in thev″=0 level of theX 2 π state). For Orion molecular cloud, PO (4, 4.5, 5-3, 3.5, 4) (e, f) lines are excitable at 196.305 and 196.500 GHz and each line would have antenna temperature less than 110 mK.
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This work was partially supported by Fapesp and CNPq, Brazil, under contract numbers 80/1659-0 and 30.4076/77-FA01, respectively.
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Atalla, R.M., Singh, P.D. PO — Prospects in interstellar medium. Astrophys Space Sci 133, 267–273 (1987). https://doi.org/10.1007/BF00642486
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DOI: https://doi.org/10.1007/BF00642486