Ionization memory of plasma emiters in a solar prominence
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arXiv
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| Main Authors: | , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866910916075847680 |
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| author | Wiehr, E. Balthasar, H. Stellmacher, G. Bianda, M. |
| author_facet | Wiehr, E. Balthasar, H. Stellmacher, G. Bianda, M. |
| contents | Aims. In the low-collisional, partially ionized plasma (PIP) of solar prominences, uncharged emitters might show different signatures of magnetic line broadening than charged emitters. We investigate if the widths of weak metall emissions in prominences exceed the thermal line broadening by a different amount for charged and for uncharged emitters.
Methods. We simultaneously observe five optically thin, weak metall lines in the brightness center of a quiescent prominence and compare their observed widths with the thermal broadening.
Results. The inferred non-thermal broadening of the metall lines does not indicate systematic differences between the uncharged Mg b2 and Na D1 and the charged Fe II emitters, only Sr II is broader.
Conclusions. The additional line broadening of charged emitters is reasonably attributed to magnetic forces. That of uncharged emitters can then come from their temporary state as ion before recombination. Magnetically induced velocities will retain some time after recombination. Modelling partially ionized plasmas then requires consideration of a memory of previous ionization states. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_10456 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Ionization memory of plasma emiters in a solar prominence Wiehr, E. Balthasar, H. Stellmacher, G. Bianda, M. Solar and Stellar Astrophysics Plasma Physics Space Physics Aims. In the low-collisional, partially ionized plasma (PIP) of solar prominences, uncharged emitters might show different signatures of magnetic line broadening than charged emitters. We investigate if the widths of weak metall emissions in prominences exceed the thermal line broadening by a different amount for charged and for uncharged emitters. Methods. We simultaneously observe five optically thin, weak metall lines in the brightness center of a quiescent prominence and compare their observed widths with the thermal broadening. Results. The inferred non-thermal broadening of the metall lines does not indicate systematic differences between the uncharged Mg b2 and Na D1 and the charged Fe II emitters, only Sr II is broader. Conclusions. The additional line broadening of charged emitters is reasonably attributed to magnetic forces. That of uncharged emitters can then come from their temporary state as ion before recombination. Magnetically induced velocities will retain some time after recombination. Modelling partially ionized plasmas then requires consideration of a memory of previous ionization states. |
| title | Ionization memory of plasma emiters in a solar prominence |
| topic | Solar and Stellar Astrophysics Plasma Physics Space Physics |
| url | https://arxiv.org/abs/2503.10456 |