Physical Processes in Star Formation

Abstract

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 overview of the main processes that are important for the understanding of star formation. We start with an observationally motivated view on star formation from a global perspective and outline the general paradigm of the life-cycle of molecular clouds, in which star formation is the key process to close the cycle. After that we focus on the thermal and chemical aspects in star forming regions, discuss turbulence and magnetic fields as well as gravitational forces. Finally, we review the most important stellar feedback mechanisms.

86 pages, 4 figures. To appear in Space Science Reviews, topical collection Star formation

References in corpus (69)

• Theory of Star Formation
• Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era
• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
• The Statistics of Supersonic Isothermal Turbulence
• A Catalog of Extended Green Objects (EGOs) in the GLIMPSE Survey: A new sample of massive young stellar object outflow candidates
• The Atomic to Molecular Transition in Galaxies. II: HI and H_2 Column Densities
• Momentum Injection by Supernovae in the Interstellar Medium
• Physical properties of molecular clouds for the entire Milky Way disk
• The Vertical Structure of Warm Ionised Gas in the Milky Way
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• The lifecycle of molecular clouds in nearby star-forming disc galaxies
• Simulating the formation of molecular clouds. II. Rapid formation from turbulent initial conditions
• Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
• Observations of the young supernova remnant RX J1713.7-3946 with the Fermi Large Area Telescope
• Magnetic Fields in Dark Cloud Cores: Arecibo OH Zeeman Observations
• HI-to-H2 Transitions and H I Column Densities in Galaxy Star-Forming Regions
• 3D Turbulent Reconnection: Theory, Tests and Astrophysical Implications
• Limiting Accretion onto Massive Stars by Fragmentation-Induced Starvation
• Star formation at very low metallicity. I: Chemistry and cooling at low densities
• Modeling jet and outflow feedback during star cluster formation
• Dependence of Interstellar Turbulent Pressure on Supernova Rate
• Vertical structure of a supernova-driven turbulent magnetized ISM
• Current status of turbulent dynamo theory: From large-scale to small-scale dynamos
• Models of turbulent dissipation regions in the diffuse interstellar medium
• The minimum mass for star formation, and the origin of binary brown dwarfs
• Metal and molecule cooling in simulations of structure formation
• Metal and molecule cooling in simulations of structure formation
• Effective destruction of CO by cosmic rays: implications for tracing H${}_2$ gas in the Universe
• Understanding Spatial and Spectral Morphologies of Ultracompact H II Regions
• Six Myths on the Virial Theorem for Interstellar Clouds
• A Detailed Study of Feedback from a Massive Star
• Early 56Ni decay γ-rays from SN2014J suggest an unusual explosion
• An upper limit to the energy of gamma-ray bursts indicates that GRB/SNe are powered by magnetars
• Is the Scaling of Supersonic Turbulence Universal?
• Turbulence and star formation efficiency in molecular clouds: solenoidal versus compressive motions in Orion B
• Surface chemistry in the Interstellar Medium II. ${\mathrm{H}}_2$ formation on dust with random temperature fluctuations
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• Turbulent small-scale dynamo action in solar surface simulations
• Impact of Protostellar Outflows on Turbulence and Star Formation Efficiency in Magnetized Dense Cores
• Magnetic Fields in the Milky Way
• The role of magnetic fields in the formation of protostellar discs
• Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions
• The Gas-Star Formation Cycle in Nearby Star-Forming Galaxies I. Assessment of Multi-scale Variations
• Scaling Relations of Compressible MHD Turbulence
• The structure and statistics of interstellar turbulence
• The Impact of Feedback During Massive Star Formation by Core Accretion
• Energy transfer in compressible magnetohydrodynamic turbulence
• How Universal is the SFR - H2 Relation?
• MHD Turbulence
• Structure and Stability of Phase Transition Layers in the Interstellar Medium
• Exact law for homogeneous compressible Hall magnetohydrodynamics turbulence
• The Fractional Ionization of the Warm Neutral Interstellar Medium
• Alternative derivation of exact law for compressible and isothermal magnetohydrodynamics turbulence
• Shock-triggered formation of magnetically-dominated clouds
• The volumetric star formation law in the Milky Way
• Collective outflow from a small multiple stellar system
• The impact of X-rays on molecular cloud fragmentation and the IMF
• Flux Correlations in Supersonic Isothermal Turbulence
• An Observational Method to Measure the Relative Fractions of Solenoidal and Compressible Modes in Interstellar Clouds
• The non-thermal superbubble in IC 10: the generation of cosmic ray electrons caught in the act
• Simulating Supersonic Turbulence in Magnetized Molecular Clouds
• Turbulent energy dissipation and intermittency in ambipolar diffusion magnetohydrodynamics
• The Role of Ambipolar Diffusion in the Formation Process of Moderately Magnetized Diffuse Clouds
• Exact relations for energy transfer in self-gravitating isothermal turbulence
• Baropycnal Work: A Mechanism for Energy Transfer Across Scales
• How vortices and shocks provide for a flux loop in two-dimensional compressible turbulence
• The impact of magnetic fields on the chemical evolution of the supernova-driven ISM
• High Resolution Simulations of Supersonic Turbulence in Molecular Clouds

Cited by in corpus (1)

• From diffuse gas to dense molecular cloud cores