The Effect of Shock Wave Duration on Star Formation and the Initial Condition of Massive Cluster Formation

Abstract

Stars are born in dense molecular filaments irrespective of their mass. Compression of the ISM by shocks cause filament formation in molecular clouds. Observations show that a massive star cluster formation occurs where the peak of gas column density in a cloud exceeds 10^23 cm^-2. In this study, we investigate the effect of the shock-compressed layer duration on filament/star formation and how the initial conditions of massive star formation are realized by performing three-dimensional (3D) isothermal magnetohydrodynamics (MHD) simulations with {gas inflow duration from the boundaries (i.e., shock wave duration)} as a controlling parameter. Filaments formed behind the shock expand after the duration time for short shock duration models, whereas long duration models lead to star formation by forming massive supercritical filaments. Moreover, when the shock duration is longer than two postshock free-fall times, the peak column density of the compressed layer exceeds 10^23 cm^-2, and {the gravitational collapse of the layer causes that} the number of OB stars expected to be formed in the shock-compressed layer reaches the order of ten (i.e., massive cluster formation).

arXiv comment16 pages, 8 figures

References in corpus (38)

• On the variation of the Initial Mass Function
• From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey
• Interstellar Turbulence I: Observations and Processes
• Comparing the statistics of interstellar turbulence in simulations and observations: Solenoidal versus compressive turbulence forcing
• On the Star Formation Rates in Molecular Clouds
• The Formation of Massive Star Systems by Accretion
• The Universality of Turbulence in Galactic Molecular Clouds
• Massive star formation: Nurture, not nature
• A Super-Alfvenic Model of Dark Clouds
• Interstellar Turbulence II: Implications and Effects
• A Minimum Column Density of 1 g cm^-2 for Massive Star Formation
• Formation of Massive Molecular Cloud Cores by Cloud-cloud Collision
• The "True" Column Density Distribution in Star-Forming Molecular Clouds
• On the universality of interstellar filaments: theory meets simulations and observations
• Radiation-Hydrodynamic Simulations of the Formation of Orion-Like Star Clusters II. The Initial Mass Function from Winds, Turbulence, and Radiation
• On the origin of non self-gravitating filaments in the ISM
• Do cloud-cloud collisions trigger high-mass star formation? I. Small cloud collisions
• Density scaling and anisotropy in supersonic MHD turbulence
• Cloud-cloud collisions and triggered star formation
• Formation of Magnetized Prestellar Cores with Ambipolar Diffusion and Turbulence
• The two molecular clouds in RCW 38; evidence for formation of the youngest super star cluster in the Milky Way triggered by cloud-cloud collision
• Star Formation triggered by cloud-cloud collisions
• Self-gravitational Magnetohydrodynamics with Adaptive Mesh Refinement for Protostellar Collapse
• GMC Collisions as Triggers of Star Formation. III. Density and Magnetically Regulated Star Formation
• Structure and Stability of Phase Transition Layers in the Interstellar Medium
• An ALMA view of molecular filaments in the Large Magellanic Cloud I: The formation of high-mass stars and pillars in the N159E-Papillon Nebula triggered by a cloud-cloud collision
• GMC Collisions as Triggers of Star Formation. II. 3D Turbulent, Magnetized Simulations
• Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds
• Probing fragmentation and velocity sub-structure in the massive NGC 6334 filament with ALMA
• GMC Collisions as Triggers of Star Formation. V. Observational Signatures
• Cloud-cloud collisions in the common foot point of molecular loops 1 and 2 in the Galactic Center
• Shock interactions, turbulence, and the origin of the stellar mass spectrum
• The formation of young massive clusters by colliding flows
• The role of collision speed, cloud density, and turbulence in the formation of young massive clusters via cloud-cloud collisions
• The Responses of Magnetically Sub-Critical Cores to Shocks
• Massive core/star formation triggered by cloud-cloud collision: Effect of magnetic field
• Nature of supersonic turbulence and density distribution function in the multiphase interstellar medium
• Evidence for a Cloud-Cloud Collision in Sh2-233 Triggering the Formation of the High-mass Protostar Object IRAS 05358+3543

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