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From giant clumps t...
From giant clumps to clouds - III. The connection between star formation and turbulence in the ISM
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- Ejdetjärn, Timmy (författare)
- Stockholms universitet,Stockholm University,Lund University,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC),Lund Observatory, Sweden
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- Agertz, Oscar (författare)
- Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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- Östlin, Göran (författare)
- Stockholms universitet,Stockholm University,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)
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- Renaud, Florent (författare)
- Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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- Romeo, Alessandro, 1961 (författare)
- Chalmers University of Technology
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(creator_code:org_t)
- 2022-05-24
- 2022
- Engelska.
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Ingår i: Monthly Notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 514:1, s. 480-496
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Abstract
Ämnesord
Stäng
- Supersonic gas turbulence is a ubiquitous property of the interstellar medium. The level of turbulence, quantified by the gas velocity dispersion (sigma(g)), is observed to increase with the star formation rate (SFR) of a galaxy, but it is yet not established whether this trend is driven by stellar feedback or gravitational instabilities. In this work, we carry out hydrodynamical simulations of entire disc galaxies, with different gas fractions, to understand the origins of the SFR-sigma(g) relation. We show that disc galaxies reach the same levels of turbulence regardless of the presence of stellar feedback processes, and argue that this is an outcome of the way disc galaxies regulate their gravitational stability. The simulations match the SFR-sigma(g) relation up to SFRs of the order of tens of M-circle dot yr(-1) and sigma(g) similar to 50 km s(-1) in neutral hydrogen and molecular gas, but fail to reach the very large values (> 100 km s(-1)) reported in the literature for rapidly star-forming galaxies. We demonstrate that such high values of sigma(g) can be explained by ( 1) insufficient beam smearing corrections in observations and (2) stellar feedback being coupled to the ionized gas phase traced by recombination lines. Given that the observed SFR-sigma(g) relation is composed of highly heterogeneous data, with sigma(g) at high SFRs almost exclusively being derived from H alpha observations of high-redshift galaxies with complex morphologies, we caution against analytical models that attempt to explain the SFR-sigma(g) relation without accounting for these effects.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
- NATURVETENSKAP -- Kemi -- Annan kemi (hsv//swe)
- NATURAL SCIENCES -- Chemical Sciences -- Other Chemistry Topics (hsv//eng)
- TEKNIK OCH TEKNOLOGIER -- Maskinteknik -- Strömningsmekanik och akustik (hsv//swe)
- ENGINEERING AND TECHNOLOGY -- Mechanical Engineering -- Fluid Mechanics and Acoustics (hsv//eng)
Nyckelord
- ISM: evolution
- ISM: kinematics and dynamics
- methods: numerical
- galaxies: star formation
- turbulence
- Galaxies: star formation
- ISM: evolution
- ISM: kinematics and dynamics
- Methods: numerical
- Turbulence
Publikations- och innehållstyp
- art (ämneskategori)
- ref (ämneskategori)
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