| Revision as of 12:03, 6 January 2005 editWorldtraveller (talk | contribs)8,569 editsNo edit summary | Revision as of 16:52, 6 January 2005 edit undoPaul August (talk | contribs)Autopatrolled, Administrators205,113 edits indicate that the ionization is caused by the stripping of electrons from the atoms; simplify next sentence.Next edit → | ||
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| '''Collisional excitation''' is a process which gives rise to ]s in the ] of ]s such as ]e and ]s. | '''Collisional excitation''' is a process which gives rise to ]s in the ] of ]s such as ]e and ]s. | ||
| In these objects, most ]s are ] by ]s from hot ]s embedded within the nebular ] |
In these objects, most ]s are ] by ]s from hot ]s embedded within the nebular ], stripping away ]. The emitted electrons, (called ]s), may collide with atoms or ions within the gas, and ] them. When these excited atoms or ions revert to their ], they will emit a photon. The spectral lines formed by these photons are called ''collisionally excited lines'' (often abbreviated to CELs). | ||
| CELs are only seen in gases at very low densities (typically less than a few thousand particles per cm³). At higher densities, the reverse process of '''collisional de-excitation''' suppresses the lines. Even the hardest ] produced on earth is still too dense for CELs to be observed. For this reason, when CELs were first observed by ] in the spectrum of the ], he did not know what they were, and attributed them to a hypothetical new element called ''Nebulium''. However, the lines he observed were later found to be emitted by extremely rarefied ]. | CELs are only seen in gases at very low densities (typically less than a few thousand particles per cm³). At higher densities, the reverse process of '''collisional de-excitation''' suppresses the lines. Even the hardest ] produced on earth is still too dense for CELs to be observed. For this reason, when CELs were first observed by ] in the spectrum of the ], he did not know what they were, and attributed them to a hypothetical new element called ''Nebulium''. However, the lines he observed were later found to be emitted by extremely rarefied ]. | ||
Revision as of 16:52, 6 January 2005
Collisional excitation is a process which gives rise to spectral lines in the spectra of astronomical objects such as planetary nebulae and H II regions.
In these objects, most atoms are ionised by photons from hot stars embedded within the nebular gas, stripping away electrons. The emitted electrons, (called photoelectrons), may collide with atoms or ions within the gas, and excite them. When these excited atoms or ions revert to their ground state, they will emit a photon. The spectral lines formed by these photons are called collisionally excited lines (often abbreviated to CELs).
CELs are only seen in gases at very low densities (typically less than a few thousand particles per cm³). At higher densities, the reverse process of collisional de-excitation suppresses the lines. Even the hardest vacuum produced on earth is still too dense for CELs to be observed. For this reason, when CELs were first observed by William Huggins in the spectrum of the Cat's Eye Nebula, he did not know what they were, and attributed them to a hypothetical new element called Nebulium. However, the lines he observed were later found to be emitted by extremely rarefied oxygen.
CELs are very important in the study of gaseous nebulae, because they can be used to determine the density and temperature of the gas.