Dynamical accretion flows

Context. Investigating the flow of material along filamentary structures towards the central core can help provide insights into high-mass star formation and evolution. Aims. Our main motivation is to answer the question of what the properties of accretion flows are in star-forming clusters. We used data from the ALMA Evolutionary Study of High Mass Protocluster Formation in the Galaxy (ALMAGAL) survey to study 100 ALMAGAL regions at a ∼1″ resolution, located between ∼2 and 6 kpc. Methods. Making use of the ALMAGAL ∼1.3 mm line and continuum data, we estimated flow rates onto individual cores. We focus specifically on flow rates along filamentary structures associated with these cores. Our primary analysis is centered around position velocity cuts in H 2 CO (3 0, 3 –2 0, 2 ), which allow us to measure the velocity fields surrounding these cores. Combining this work with column density estimates, we were able to derive the flow rates along the extended filamentary structures associated with cores in these regions. Results. We selected a sample of 100 ALMAGAL regions, covering four evolutionary stages from quiescent to protostellar, young stellar objects (YSOs), and H II regions (25 each). Using a dendrogram and line analysis, we identify a final sample of 182 cores in 87 regions. In this paper, we present 728 flow rates for our sample (4 per core), analysed in the context of evolutionary stage, distance from the core, and core mass. On average, for the whole sample, we derived flow rates on the order of ∼10 −4 M ⊙ yr −1 with estimated uncertainties of ±50%. We see increasing differences in the values among evolutionary stages, most notably between the less evolved (quiescent and protostellar) and more evolved (YSO and H II region) sources and we also see an increasing trend as we move further away from the centre of these cores. We also find a clear relationship between the calculated flow rates and core masses ∼ M 2/3 , which is in line with the result expected from the tidal-lobe accretion mechanism. The significance of these relationships is tested with Kolmogorov–Smirnov and Mann-Whitney U tests. Conclusions. Overall, we see an increasing trend in the relationships between the flow rate and the three investigated parameters, namely: evolutionary stage, distance from the core, and core mass.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-08-23
DOI
https://doi.org/10.1051/0004-6361/202449794
Citations
25
Primary Topic
Phase Equilibria and Thermodynamics
Type
article
Field-Weighted Citation Impact
4.61

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article

Dynamical accretion flows

A. Avison, A. Coletta, R.S. Klessen, J. Bally et al.
25 citations
Astronomy and Astrophysics
Phase Equilibria and Thermodynamics
4.61
article

Dynamical accretion flows

A. Avison, A. Coletta, R.S. Klessen, J. Bally, T. Möller, P. Sanhueza, G. A. Fuller, S. Walch, M. Merello, Paul T. P. Ho, C. Gieser, J. Wallace, K. L. J. Rygl, A. J. Rigby, Patrick M. Koch, Y. Maruccia, F. Fontani, H. Beuther, Yongan Tang, T. Liu, C. Mininni, D. C. Lis, Á. Sánchez-Monge, S. Pezzuto, H. Zinnecker, Daniel L. Walker, C. L. Brogan, A. Traficante, M. Scheuck, F. Wyrowski, Chi-Yan Law, Cara Battersby, M. T. Beltrán, J. Syed, M. R. A. Wells, M. Benedettini, B. Jones, P. Schilke, D. Elia, L. Moscadelli, Q. Zhang, S. Molinari, A. Ahmadi, F. van der Tak, R. Kuiper, J. D. Soler, E. Schisano, Shaun D. Clarke, Pamela Klaassen, L. Testi
article en
25 citations

Abstract

Context. Investigating the flow of material along filamentary structures towards the central core can help provide insights into high-mass star formation and evolution. Aims. Our main motivation is to answer the question of what the properties of accretion flows are in star-forming clusters. We used data from the ALMA Evolutionary Study of High Mass Protocluster Formation in the Galaxy (ALMAGAL) survey to study 100 ALMAGAL regions at a ∼1″ resolution, located between ∼2 and 6 kpc. Methods. Making use of the ALMAGAL ∼1.3 mm line and continuum data, we estimated flow rates onto individual cores. We focus specifically on flow rates along filamentary structures associated with these cores. Our primary analysis is centered around position velocity cuts in H 2 CO (3 0, 3 –2 0, 2 ), which allow us to measure the velocity fields surrounding these cores. Combining this work with column density estimates, we were able to derive the flow rates along the extended filamentary structures associated with cores in these regions. Results. We selected a sample of 100 ALMAGAL regions, covering four evolutionary stages from quiescent to protostellar, young stellar objects (YSOs), and H II regions (25 each). Using a dendrogram and line analysis, we identify a final sample of 182 cores in 87 regions. In this paper, we present 728 flow rates for our sample (4 per core), analysed in the context of evolutionary stage, distance from the core, and core mass. On average, for the whole sample, we derived flow rates on the order of ∼10 −4 M ⊙ yr −1 with estimated uncertainties of ±50%. We see increasing differences in the values among evolutionary stages, most notably between the less evolved (quiescent and protostellar) and more evolved (YSO and H II region) sources and we also see an increasing trend as we move further away from the centre of these cores. We also find a clear relationship between the calculated flow rates and core masses ∼ M 2/3 , which is in line with the result expected from the tidal-lobe accretion mechanism. The significance of these relationships is tested with Kolmogorov–Smirnov and Mann-Whitney U tests. Conclusions. Overall, we see an increasing trend in the relationships between the flow rate and the three investigated parameters, namely: evolutionary stage, distance from the core, and core mass.

Astronomy and AstrophysicsVol. 690
Leiden University (NL), Centre National de la Recherche Scientifique (FR), University of Leeds (GB), Institute of Astronomy and Astrophysics, Academia Sinica (TW), European Southern Observatory (DE), Jet Propulsion Laboratory (US), University of Connecticut (US), University of Groningen (NL), University of Cologne (DE), University of Colorado Boulder (US), National Institutes of Natural Sciences (JP), The Graduate University for Advanced Studies, SOKENDAI (JP), Heidelberg University (DE), National Radio Astronomy Observatory (US), Université Paris Sciences et Lettres (FR), Shanghai Astronomical Observatory (CN), Arcetri Astrophysical Observatory (IT), University of Manchester (GB), Universidad Autónoma de Chile (CL), Sorbonne Université (FR), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Institute for Space Astrophysics and Planetology (IT), Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères (FR), Royal Observatory (GB), SKA Observatory (GB), Max Planck Institute for Astronomy (DE), Institute of Space Sciences (ES), Istituto di Radioastronomia di Bologna (IT), East Asian Observatory (US), Forschungsstätte der Evangelischen Studiengemeinschaft (DE), Center for Astrophysics Harvard & Smithsonian (US), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Max Planck Institute for Radio Astronomy (DE), National Astronomical Observatory of Japan (JP), Space Research Organisation Netherlands (NL), UK Astronomy Technology Centre (GB), University of Duisburg-Essen (DE), Chalmers University of Technology (SE), University of Chile (CL), Sapienza University of Rome (IT)
National Science Foundation, National Aeronautics and Space Administration, California Institute of Technology, National Radio Astronomy Observatory, Deutsche Forschungsgemeinschaft, National Natural Science Foundation of China, Chinese Academy of Sciences, Korea Astronomy and Space Science Institute, National Astronomical Observatory of Japan, Jet Propulsion Laboratory, Science and Technology Facilities Council, National Institutes of Natural Sciences
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Phase Equilibria and Thermodynamics
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