Star Formation in Molecular Clouds

Klessen, Ralf S.

doi:10.1051/eas/1151009

Cited by 30 publications

(32 citation statements)

References 247 publications

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“…This scenario is supported by the observations made within the Herschel Gould Belt survey (e.g. André et al 2010;Könyves et al 2010;Men'shchikov et al 2010) and A&A 544, A14 (2012) other Herschel programs (Molinari et al 2010;Schneider et al 2010;Nguyen Luong et al 2011;Hill et al 2011;Schneider et al 2012;Juvela et al 2012) as well as by numerical simulations (Padoan & Nordlund 2011;Vázquez-Semadeni et al 2011;Klessen 2011;Bonnell et al 2011).…”

Section: With Further Contributions Fromsupporting

confidence: 52%

A Corona Australis cloud filament seen in NIR scattered light

Juvela

Pelkonen

White

et al. 2012

A&A

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Context. The dust is an important tracer of dense interstellar clouds but its properties are expected to undergo changes affecting the scattering and emitting properties of the grains. With recent Herschel observations, the northern filament of the Corona Australis cloud has now been mapped in a number of bands from 1.2 μm to 870 μm. The data set provides a good starting point for the study of the cloud over several orders of magnitude in density. Aims. We wish to examine the differences of the column density distributions derived from dust extinction, scattering, and emission, and to determine to what extent the observations are consistent with the standard dust models. Methods. From Herschel data, we calculate the column density distribution that is compared to the corresponding data derived in the near-infrared regime from the reddening of the background stars, and from the surface brightness attributed to light scattering. We construct three-dimensional radiative transfer models to describe the emission and the scattering. Results. The scattered light traces low column densities of A V ∼ 1 m better than the dust emission, remaining useful to A V ∼ 10−15 m . Based on the models, the extinction and the level of dust emission are surprisingly consistent with a sub-millimetre dust emissivity typical of diffuse medium. However, the intensity of the scattered light is very low at the centre of the densest clump and this cannot be explained without a very low grain albedo. Both the scattered light and dust emission indicate an anisotropic radiation field. The modelling of the dust emission suggests that the radiation field intensity is at least three times the value of the normal interstellar radiation field. Conclusions. The inter-comparison between the extinction, light scattering, and dust emission provides very stringent constraints on the cloud structure, the illuminating radiation field, and the grain properties.

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Section: With Further Contributions Fromsupporting

confidence: 52%

A Corona Australis cloud filament seen in NIR scattered light

Juvela

Pelkonen

White

et al. 2012

A&A

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“…Turbulence is driven on large scales comparable to the size L of the cloud and is dissipated on very small scales η K . Adopted from Klessen (2011).…”

Section: Fig 15mentioning

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 connection between star formation processes and molecular clouds is a very fertile research topic encompassing observations (e.g., Bigiel et al 2008), theory (e.g., Krumholz & McKee 2005), and experimental/numerical works (e.g., Klessen 2011). In our approach we revisited a work by Elmegreen & Efremov (1997) chosen for its simplicity.…”

Section: Appendix B: Star Formation Efficiency and Disruption Time Rementioning

confidence: 99%

Dissipative phenomena in extended-body interactions

Pasetto

Bertelli

Grebel

et al. 2012

A&A

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Aims. Dissipative phenomena occurring during the orbital evolution of a dwarf satellite galaxy around a host galaxy may leave signatures in the star formation activity and signatures in the colour-magnitude diagram of the galaxy stellar content. Our goal is to reach a simple and qualitative description of these complicated phenomena. Methods. We develop an analytical and numerical technique able to study the ram pressure, Kelvin-Helmholtz instability, RayleighTaylor, and tidal forces acting on the star formation processes in molecular clouds. We consider it with synthetic colour-magnitude diagram techniques. Results. We developed a method of investigating the connections between gas consumption processes and star formation processes in the context of the two extended-body interactions, paying special attention to the dwarf galaxies dynamical regime.

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Star Formation in Molecular Clouds

Cited by 30 publications

References 247 publications

A Corona Australis cloud filament seen in NIR scattered light

A Corona Australis cloud filament seen in NIR scattered light

Physical Processes in the Interstellar Medium

Dissipative phenomena in extended-body interactions

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