Perturbation growth in accreting filaments

• Published in: Monthly notices of the Royal Astronomical Society Vol. 458; no. 1; pp. 319 - 324
• Main Authors: Clarke, S. D., Whitworth, A. P., Hubber, D. A.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 01-05-2016
• Subjects: Accretion; Accretion disks; Astronomy; Estimates; Filaments; Fluid mechanics; Fragmentation; Fragments; Hydrodynamics; Oscillations; Perturbation methods; Simulation; Star & galaxy formation; stars: formation; ISM: clouds; ISM: structure; ISM: kinematics and dynamics
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stw407

We use smoothed particle hydrodynamic simulations to investigate the growth of perturbations in infinitely long filaments as they form and grow by accretion. The growth of these perturbations leads to filament fragmentation and the formation of cores. Most previous work on this subject has been confined to the growth and fragmentation of equilibrium filaments and has found that there exists a preferential fragmentation length-scale which is roughly four times the filament's diameter. Our results show a more complicated dispersion relation with a series of peaks linking perturbation wavelength and growth rate. These are due to gravo-acoustic oscillations along the longitudinal axis during the sub-critical phase of growth. The positions of the peaks in growth rate have a strong dependence on both the mass accretion rate onto the filament and the temperature of the gas. When seeded with a multiwavelength density power spectrum, there exists a clear preferred core separation equal to the largest peak in the dispersion relation. Our results allow one to estimate a minimum age for a filament which is breaking up into regularly spaced fragments, as well as an average accretion rate. We apply the model to observations of filaments in Taurus by Tafalla & Hacar and find accretion rates consistent with those estimated by Palmeirim et al.