THE DIAGNOSTIC O VI ABSORPTION LINE IN DIFFUSE PLASMAS: COMPARISON OF NON-EQUILIBRIUM IONIZATION STRUCTURE SIMULATIONS TO
                    <i>FUSE</i>
                    DATA

Avillez, Miguel A. de; Breitschwerdt, D.

doi:10.1088/2041-8205/761/2/l19

Cited by 16 publications

(6 citation statements)

References 44 publications

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“…There are many efforts to account for non-equilibrium effects, either by explicitly solving for the non-equilibrium ionization state (see e.g. Cen and Fang, 2006;de Avillez and Breitschwerdt, 2012;Oppenheimer and Schaye, 2013;Richings et al, 2014) or with an ionization state dominated by photoionization rather than collisional ionization (e.g. Wiersma et al, 2009;Gnedin and Hollon, 2012).…”

Section: Cooling By Permitted Transitionsmentioning

confidence: 99%

Physical Processes in Star Formation

Girichidis¹,

Offner²,

Kritsuk³

et al. 2020

Space Sci Rev

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Star formation is a complex multi-scale phenomenon that is of significant importance for astrophysics in general. Stars and star formation are key pillars in observational astronomy from local star forming regions in the Milky Way up to high-redshift galaxies. From a theoretical perspective, star formation and feedback processes (radiation, winds, and supernovae) play a pivotal role in advancing our understanding of the physical processes at work, both individually and of their interactions. In this review we will give an

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Section: Cooling By Permitted Transitionsmentioning

confidence: 99%

Physical Processes in Star Formation

Girichidis¹,

Offner²,

Kritsuk³

et al. 2020

Space Sci Rev

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show abstract

“…Cen & Fang, 2006;de Avillez & Breitschwerdt, 2012;Oppenheimer & Schaye, 2013;Richings et al, 2014), or by pre-computing and tabulating rates appropriate for gas cooling at constant pressure or constant density (Gnat & Sternberg, 2007), or with an ionization state dominated by photoionization rather than collisional ionization (e.g. Wiersma et al, 2009;Gnedin & Hollon, 2012).…”

Section: Permitted Transitionsmentioning

confidence: 99%

Physical Processes in the Interstellar Medium

Klessen

Glover

2015

Saas-Fee Advanced Course

170

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Interstellar space is filled with a dilute mixture of charged particles, atoms, molecules and dust grains, called the interstellar medium (ISM). Understanding its physical properties and dynamical behavior is of pivotal importance to many areas of astronomy and astrophysics. Galaxy formation and evolution, the formation of stars, cosmic nucleosynthesis, the origin of large complex, prebiotic molecules and the abundance, structure and growth of dust grains which constitute the fundamental building blocks of planets, all these processes are intimately coupled to the physics of the interstellar medium. However, despite its importance, its structure and evolution is still not fully understood. Observations reveal that the interstellar medium is highly turbulent, consists of different chemical phases, and is characterized by complex structure on all resolvable spatial and temporal scales. Our current numerical and theoretical models describe it as a strongly coupled system that is far from equilibrium and where the different components are intricately linked together by complex feedback loops. Describing the interstellar medium is truly a multi-scale and multi-physics problem. In these lecture notes we introduce the microphysics necessary to better understand the interstellar medium. We review the relations between large-scale and small-scale dynamics, we consider turbulence as one of the key drivers of galactic evolution, and we review the physical processes that lead to the formation of dense molecular clouds and that govern stellar birth in their interior.

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“…The ionization structure, cooling and emission spectra of H, He, C, N, O, Ne, Mg, Si, S, and Fe ions (with solar abundances; Asplund et al 2009) are traced on the spot at each time step assuming an equal Maxwellian temperature for electrons and ions (see details and references in Avillez & Breitschwerdt 2012).…”

Section: Thermal and Dynamical Evolution Of The Ismmentioning

confidence: 99%

ISM simulations: an overview of models

Avillez

Breitschwerdt

Asgekar³

et al. 2012

Proc. IAU

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Abstract. Until recently the dynamical evolution of the interstellar medium (ISM) was simulated using collisional ionization equilibrium (CIE) conditions. However, the ISM is a dynamical system, in which the plasma is naturally driven out of equilibrium due to atomic and dynamic processes operating on different timescales. A step forward in the field comprises a multi-fluid approach taking into account the joint thermal and dynamical evolutions of the ISM gas.

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THE DIAGNOSTIC O VI ABSORPTION LINE IN DIFFUSE PLASMAS: COMPARISON OF NON-EQUILIBRIUM IONIZATION STRUCTURE SIMULATIONS TO FUSE DATA

Cited by 16 publications

References 44 publications

Physical Processes in Star Formation

Physical Processes in Star Formation

Physical Processes in the Interstellar Medium

ISM simulations: an overview of models

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