Catastrophic cooling instability in optically thin plasmas
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866917870680670208 |
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| author | Waters, Tim Stricklan, Amanda |
| author_facet | Waters, Tim Stricklan, Amanda |
| contents | The solar corona is the prototypical example of a low density environment heated to high temperatures by external sources. The plasma cools radiatively, and because it is optically thin to this radiation, it becomes possible to model the density, velocity, and temperature structure of the system by modifying the MHD equations to include energy source terms that approximate the local heating and cooling rates. The solutions can be highly inhomogeneous and even multiphase because the well known linear instability associated with these source terms, thermal instability, leads to a catastrophic heating and cooling of the plasma in the nonlinear regime. Here we show that there is a separate, much simpler instance of catastrophic heating and cooling accompanying these source terms that can rival thermal instability in dynamical importance. The linear stability criterion is the isochoric one identified by Parker (1953), and we demonstrate that cooling functions derived from collisional ionization equilibrium are highly prone to violating this criterion. If catastrophic cooling instability can act locally in global simulations, then it is an alternative mechanism for forming condensations, and due to its nonequilibrium character, it may be relevant to explaining a host of phenomena associated with the production of cooler gas in hot, low density plasmas. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_15869 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Catastrophic cooling instability in optically thin plasmas Waters, Tim Stricklan, Amanda Solar and Stellar Astrophysics Plasma Physics Space Physics The solar corona is the prototypical example of a low density environment heated to high temperatures by external sources. The plasma cools radiatively, and because it is optically thin to this radiation, it becomes possible to model the density, velocity, and temperature structure of the system by modifying the MHD equations to include energy source terms that approximate the local heating and cooling rates. The solutions can be highly inhomogeneous and even multiphase because the well known linear instability associated with these source terms, thermal instability, leads to a catastrophic heating and cooling of the plasma in the nonlinear regime. Here we show that there is a separate, much simpler instance of catastrophic heating and cooling accompanying these source terms that can rival thermal instability in dynamical importance. The linear stability criterion is the isochoric one identified by Parker (1953), and we demonstrate that cooling functions derived from collisional ionization equilibrium are highly prone to violating this criterion. If catastrophic cooling instability can act locally in global simulations, then it is an alternative mechanism for forming condensations, and due to its nonequilibrium character, it may be relevant to explaining a host of phenomena associated with the production of cooler gas in hot, low density plasmas. |
| title | Catastrophic cooling instability in optically thin plasmas |
| topic | Solar and Stellar Astrophysics Plasma Physics Space Physics |
| url | https://arxiv.org/abs/2408.15869 |