Abstract
By simple arguments, it is shown how alkaline types of atoms can be seen in dense molecular clouds depending on the average temperature of such regions of the Universe. This paper predicts infrared lines of such atoms that could be seen in molecular clouds. The theory is developed in the first part and the predicted experimental results will follow. It results that the alkaline atoms modelized using the short-range polarization potential are found in quantum states n* > 2.
Highlights
When one considers the polarization potential, it could be detectable in low-temperature parts of the universe that contain atoms, molecules and dust, it is known that these temperatures vary between 50 K ≥ Tclouds ≤ 500 K for molecular clouds of known or estimated densities
This temperature T2 corresponds to an energy in eV E2 = 2.22 eV, considering that H atoms, are part of molecular clouds of temperature Tclouds = 100 K, they can be found in a state of maximum n = 3, while the alkaline atom Lithium has a quantum number:= n* 4.35 > n
The total radiating power is obtained when the oscillator strengths: 2 Ψi d Ψ j of the i → j is calculated, such atomic data are available in [5] and [7] these data take into account atomic structure: NZ number of protons and NE number of electrons for each atomic species Mg, Na, Li, Ca, and atomic data exists for high states of atoms Ψi and Ψ j each element has characteristic quantum numbers for a ∆L =1 transition these are δs and δ p quantum defects, ni=* ni − δs and n f =* ni − δ p are the effective quantum numbers2 (Tables 2-6)
Summary
When one considers the polarization potential, it could be detectable in low-temperature parts of the universe that contain atoms, molecules and dust, it is known that these temperatures vary between 50 K ≥ Tclouds ≤ 500 K for molecular clouds of known or estimated densities (giant interstellar molecular clouds). The prospect of this work is to foresee infrared lines (possibly detectable) emitted by alkaline atoms that exist in molecular clouds, with accepted abundances of these regions of the Universe. For the theoretical part of this work and subsequent calculations the hydrogen ionization energy IH = 13.616 eV is used to measure the effect of the atom core on energy levels αD are the different static dipolar polarizabilities of the atoms, estimates of these quantities exist for elements: Li, Mg, Na, Cs, K, Ca [3] [4]
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