Evolution of the Angular Momentum of Molecular Cloud Cores Formed from Filament Fragmentation

Abstract

The angular momentum of molecular cloud cores plays an essential role in the star formation process. However, the time evolution of the angular momentum of molecular cloud cores is still unclear. In this paper, we perform three-dimensional simulations to investigate the time evolution of the angular momentum of molecular cloud cores formed through filament fragmentation. As a result, we find that most of the cores rotate perpendicular to the filament axis. The mean angular momentum of the cores changes by only around 30% during the initial stage of their formation process and then remains almost constant. In addition, we analyze the internal angular momentum structure of the cores. Although the cores gain angular momentum with various directions from the initial turbulent velocity fluctuations of their parent filaments, the angular momentum profile in each core converges to the self-similar solution. We also show that the degree of complexity of the angular momentum structure in a core slightly decreases with time. Moreover, we perform synthetic observations and show that the angular momentum profile measured from the synthetic mean velocity map is compatible with the observations when the filament inclination is taken into account. The present study suggests a theory of core formation from filament fragmentation where the angular momentum structures of the cores are determined by the velocity fluctuation along the filaments and both are compatible with the observations. This theory also provides new insights on the core properties that could be observationally tested.

arXiv comment42 pages, 35 figures, accepted for publication in ApJ

References in corpus (48)

• From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey
• Characterizing interstellar filaments with Herschel in IC5146
• Dense Cores in Dark Clouds. XIV. N2H+(1-0) maps of dense cloud cores
• Herschel view of the Taurus B211/3 filament and striations: Evidence of filamentary growth?
• Reformulation of Smoothed Particle Hydrodynamics with Riemann Solver
• Characterizing the properties of nearby molecular filaments observed with Herschel
• Dense core formation by fragmentation of velocity-coherent filaments in L1517
• Collapse of Rotating Magnetized Molecular Cloud Cores and Mass Outflows
• Herschel-SPIRE observations of the Polaris flare : structure of the diffuse interstellar medium at the sub-parsec scale
• Chains of dense cores in the Taurus L1495/B213 complex
• Formation and evolution of interstellar filaments; Hints from velocity dispersion measurements
• Collapse and Fragmentation of Rotating Magnetized Clouds. II. Binary Formation and Fragmentation of First Cores
• Fragmentation of a Molecular Cloud Core versus Fragmentation of the Massive Protoplanetary Disk in the Main Accretion Phase
• Implementation and performance of FDPS: A Framework Developing Parallel Particle Simulation Codes
• Formation Scenario for Wide and Close Binary Systems
• Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
• TURBULENCE IN MOLECULAR CLOUDS
• The Musca cloud: A 6 pc-long velocity-coherent, sonic filament
• Dust polarized emission observations of NGC 6334; BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network
• Alignment Between Protostellar Outflows and Filamentary Structure
• The Angular Momentum of Magnetized Molecular Cloud Cores: A 2D-3D Comparison
• Evolution of Angular Momentum Distribution during Star Formation
• The central 1000 AU of a pre-stellar core revealed with ALMA. I. 1.3 mm continuum observations
• Angular momentum profiles of Class 0 protostellar envelopes
• Classification of Filament Formation Mechanisms in Magnetized Molecular Clouds
• Molecular filament formation and filament-cloud interaction: Hints from Nobeyama 45m telescope observations
• A possible link between the power spectrum of interstellar filaments and the origin of the prestellar core mass function
• Widespread Molecular Outflows in the Infrared Dark Cloud G28.37+0.07: Indications of Orthogonal Outflow-Filament Alignment
• Angular Momentum of the N2H+ Cores in the Orion A Cloud
• On the typical width of Herschel filaments
• The specific angular momentum radial profile in dense cores: improved initial conditions for disk formation
• Misalignment of Magnetic Fields, Outflows and Discs in Star-forming Clouds
• FAUST II. Discovery of a Secondary Outflow in IRAS 15398-3359: Variability in Outflow Direction during the Earliest Stage of Star Formation?
• Kinematics of dense gas in the L1495 filament
• Geometry, Kinematics, and Magnetization of Simulated Prestellar Cores
• ALMA observations reveal no preferred outflow--filament and outflow--magnetic field orientations
• The Origins of Protostellar Core Angular Momenta
• The core and stellar mass functions in massive collapsing filaments
• The CARMA-NRO Orion Survey: Protostellar Outflows, Energetics, and Filamentary Alignment
• An Origin for the Angular Momentum of Molecular Cloud Cores: a Prediction from Filament Fragmentation
• Protostellar collapse of magneto-turbulent cloud cores: shape during collapse and outflow formation
• Angular Momenta, Magnetization, and Accretion of Protostellar Cores
• Velocity structure of the 50 pc-long NGC 6334 filamentary cloud: Hints of multiple compressions and their impact on the cloud properties?
• Investigating the Complex Velocity Structures within Dense Molecular Cloud Cores with GBT-Argus
• How the power spectrum of dust continuum images may hide the presence of a characteristic filament width
• Evolution of the angular momentum during gravitational fragmentation of molecular clouds
• On estimating angular momenta of infalling protostellar cores from observations
• A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds

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