⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
⢠Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
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INTERSTELLAR MOLECULARCLOUDS• In <strong>in</strong>terstellar t molecular l clouds, typical electrontemperatures are around 30 K or smaller, andtypical electron densities are 2-15 cm¯³. Insuchconditions, free electrons may be captured(recomb<strong>in</strong>ation) by an ion <strong>in</strong> very distant orbitwith pr<strong>in</strong>cipal quantum number (n) values ofseveral hundreds and deexcite <strong>in</strong> cascade toenergy levels n-1, n-2,... radiat<strong>in</strong>g <strong>in</strong> radiodoma<strong>in</strong>. Such distant electrons are weaklybounded with the core and may be <strong>in</strong>fluenced byvery weak electric microfield. Consequently,Stark <strong>broaden<strong>in</strong>g</strong> may be significant.
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