⢠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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STARK-B• http://stark-b.obspm.fr/• This is a database of calculated widths and shifts of isolated <strong>l<strong>in</strong>e</strong>s ofatoms and ions due to electron and ion collisions.iThis database is devoted to modellisation and spectroscopicdiagnostics of stellar atmospheres and envelopes. In addition, it isalso devoted to laboratory <strong>plasmas</strong>, laser equipments andtechnological <strong>plasmas</strong>. So, the doma<strong>in</strong> of temperatures anddensities covered by the tables is wide and depends on theionization degree of the considered ion. The temperature can varyfrom several thousands for neutral atoms to several hundredthousands of Kelv<strong>in</strong> for highly charged ions. The electron or iondensity can vary from 10 12 (case of stellar atmospheres) to several10 19 cm -3 (some white dwarfs and some laboratory <strong>plasmas</strong>).
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