Feedback from an O star formed in a filament

Abstract

We explore a simple semi-analytic model for what happens when an O star (or cluster of O stars) forms in an isolated filamentary cloud. The model is characterised by three configuration parameters: the radius of the filament, R_FIL, the mean density of H_2 in the filament, n_FIL, and the rate at which the O star emits ionising photons, Ndot_LyC. We show that for a wide range of these configuration parameters, ionising radiation from the O star rapidly erodes the filament, and the ionised gas from the filament disperses into the surroundings. Under these circumstances the distance from the O star to the ionisation front (IF) is given approximately by L ~ 5.2 pc [R_FIL/0.2pc]^-1/6 [n_FIL/10^4cm^-3]^-1/3 [Ndot_LyC/10^49s^-1]^1/6 [t/Myr]^2/3, and we derive similar simple power-law expressions for other quantities, for example the rate at which ionised gas boils off the filament, and the mass of the shock-compressed layer (SCL) that is swept up behind the IF. We show that a very small fraction of the ionising radiation is expended locally, and a rather small amount of molecular gas is ionised and dispersed. We discuss some features of more realistic models, and the extent to which they might modify or invalidate the predictions of this idealised model. In particular we show that, for very large R_FIL and/or large n_FIL and/or low Ndot_LyC, continuing accretion onto the filament might trap the ionising radiation from the O star, slowing the erosion of the filament even further.

arXiv comment10 pages, 3 figures, accepted by MNRAS

References in corpus (31)

• From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey
• On the Star Formation Rates in Molecular Clouds
• Global collapse of molecular clouds as a formation mechanism for the most massive stars
• Cluster-formation in the Rosette molecular cloud at the junctions of filaments
• On the Role of Massive Stars in the Support and Destruction of Giant Molecular Clouds
• Massive stars in massive clusters II: Disruption of bound clusters by photoionization
• Nonlinear Instabilities in Shock-Bounded Slabs
• An ALMA study of the Orion Integral Filament: I. Evidence for narrow fibers in a massive cloud
• Dispersal of molecular clouds by ionising radiation
• From Filamentary Networks to Dense Cores in Molecular Clouds: Toward a New Paradigm for Star Formation
• Characterizing the properties of nearby molecular filaments observed with Herschel
• Formation of Structure in Molecular Clouds: A Case Study
• A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey
• Ionisation-induced star formation I: The collect and collapse model
• Radiation driven implosion and triggered star formation
• Ionizing feedback from massive stars in massive clusters: Fake bubbles and untriggered star formation
• Detailed Numerical Simulations on the Formation of Pillars around HII-regions
• Gravity drives the evolution of infrared dark hubs: JVLA observations of SDC13
• Dynamics of cluster-forming hub-filament systems: The case of the high-mass star-forming complex Monoceros R2
• The modelling of feedback in star formation simulations
• On the relation between the column density structures and the magnetic field orientation in the Vela C molecular complex
• The Herschel view of the dense core population in the Ophiuchus molecular cloud
• Clumps and triggered star formation in ionised molecular clouds
• Photoionisation Feedback in a Self-Gravitating, Magnetised, Turbulent Cloud
• 3D simulations of globules and pillars formation around HII regions: turbulence and shock curvature
• Age, size, and position of H ii regions in the Galaxy. Expansion of ionized gas in turbulent molecular clouds
• SILCC-ZOOM: The early impact of ionizing radiation on forming molecular clouds
• Feedback from OB stars on their parent cloud: Gas exhaustion rather than gas ejection
• 3D simulations of pillars formation around HII regions: the importance of shock curvature
• L1495 Revisited: A PPMAP View of a Star-Forming Filament
• Pre-supernova feedback mechanisms drive the destruction of molecular clouds in nearby star-forming disc galaxies

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• Ionized filaments and ongoing physical processes in massive star-forming sites around l = 345.5 degree
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