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Verfasst von:Pardi, Anabele-Linda [VerfasserIn]   i
 Glover, Simon [VerfasserIn]   i
 Klessen, Ralf S. [VerfasserIn]   i
Titel:The impact of magnetic fields on the chemical evolution of the supernova-driven ISM
Verf.angabe:A. Pardi, P. Girichidis, T. Naab, S. Walch, T. Peters, F. Heitsch, S.C.O. Glover, R S. Klessen, R. Wünsch and A. Gatto
Jahr:2017
Jahr des Originals:2016
Umfang:23 S.
Fussnoten:Published: 29 November 2016 ; Gesehen am 07.06.2018
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2017
Band/Heft Quelle:465(2017), 4, Seite 4611-4633
ISSN Quelle:1365-2966
Abstract:Abstract: We present three-dimensional magneto-hydrodynamical simulations of the self-gravitating interstellar medium (ISM) in a periodic (256 pc)3 box with a mean number density of 0.5 cm−3. At a fixed supernova rate we investigate the multi-phase ISM structure, H2 molecule formation and density-magnetic field scaling for varying initial magnetic field strengths (0, 6 × 10−3, 0.3, 3 μG). All magnetic runs saturate at mass-weighted field strengths of ∼1-3 μG but the ISM structure is notably different. With increasing initial field strengths (from 6 × 10−3 to 3 μG) the simulations develop an ISM with a more homogeneous density and temperature structure, with increasing mass (from 5 to 85 per cent) and volume filling fractions (VFFs; from 4 to 85 per cent) of warm (300 < T < 8000 K) gas, with decreasing VFFs from ∼35 to ∼12 per cent of hot gas (T > 105 K) and with a decreasing H2 mass fraction (from 70 to < 1 per cent). Meanwhile, the mass fraction of gas in which the magnetic pressure dominates over the thermal pressure increases by a factor of 10, from 0.07 for an initial field of 6 × 10−3 μG to 0.7 for a 3 μG initial field. In all but the simulations with the highest initial field strength self-gravity promotes the formation of dense gas and H2, but does not change any other trends. We conclude that magnetic fields have a significant impact on the multi-phase, chemical and thermal structure of the ISM and discuss potential implications and limitations of the model.
DOI:doi:10.1093/mnras/stw3071
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

kostenfrei: Volltext: http://dx.doi.org/10.1093/mnras/stw3071
 kostenfrei: Volltext: https://academic.oup.com/mnras/article/465/4/4611/2608772
 DOI: https://doi.org/10.1093/mnras/stw3071
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1564744396
Verknüpfungen:→ Zeitschrift

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