Bursty star formation feedback and cooling outflows
<p>We study how outflows of gas launched from a central galaxy undergoing repeated starbursts propagate through the circumgalactic medium (CGM), using the simulation code RAMSES. We assume that the outflow from the disk can be modelled as a rapidly moving bubble of hot gas at ~ 1 kpc above dis...
| Main Authors: | , , , , |
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| Format: | Journal article |
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Oxford University Press
2016
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| _version_ | 1826264263993327616 |
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| author | Suarez, T Pontzen, A Peiris, H Slyz, A Devriendt, J |
| author_facet | Suarez, T Pontzen, A Peiris, H Slyz, A Devriendt, J |
| author_sort | Suarez, T |
| collection | OXFORD |
| description | <p>We study how outflows of gas launched from a central galaxy undergoing repeated starbursts propagate through the circumgalactic medium (CGM), using the simulation code RAMSES. We assume that the outflow from the disk can be modelled as a rapidly moving bubble of hot gas at ~ 1 kpc above disk, then ask what happens as it moves out further into the halo around the galaxy on ~ 100 kpc scales. To do this we run 60 two-dimensional simulations scanning over parameters of the outflow. Each of these is repeated with and without radiative cooling, assuming a primordial gas composition to give a lower bound on the importance of cooling. In a large fraction of radiative-cooling cases we are able to form rapidly outflowing cool gas from in situ cooling of the flow. We show that the amount of cool gas formed depends strongly on the ‘burstiness’ of energy injection; sharper, stronger bursts typically lead to a larger fraction of cool gas forming in the outflow. The abundance ratio of ions in the CGM may therefore change in response to the detailed historical pattern of star formation. For instance, outflows generated by star formation with short, intense bursts contain up to 60 per cent of their gas mass at temperatures < 5 X 10^4 K; for near-continuous star formation the figure is ≲ 5 per cent. Further study of cosmological simulations, and of idealised simulations with e.g., metal-cooling, magnetic fields and/or thermal conduction, will help to understand the precise signature of bursty outflows on observed ion abundances.</p> |
| first_indexed | 2024-03-06T20:04:57Z |
| format | Journal article |
| id | oxford-uuid:2899d410-3c22-467c-8040-6fe58c456f50 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T20:04:57Z |
| publishDate | 2016 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:2899d410-3c22-467c-8040-6fe58c456f502022-03-26T12:13:51ZBursty star formation feedback and cooling outflowsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:2899d410-3c22-467c-8040-6fe58c456f50Symplectic Elements at OxfordOxford University Press2016Suarez, TPontzen, APeiris, HSlyz, ADevriendt, J<p>We study how outflows of gas launched from a central galaxy undergoing repeated starbursts propagate through the circumgalactic medium (CGM), using the simulation code RAMSES. We assume that the outflow from the disk can be modelled as a rapidly moving bubble of hot gas at ~ 1 kpc above disk, then ask what happens as it moves out further into the halo around the galaxy on ~ 100 kpc scales. To do this we run 60 two-dimensional simulations scanning over parameters of the outflow. Each of these is repeated with and without radiative cooling, assuming a primordial gas composition to give a lower bound on the importance of cooling. In a large fraction of radiative-cooling cases we are able to form rapidly outflowing cool gas from in situ cooling of the flow. We show that the amount of cool gas formed depends strongly on the ‘burstiness’ of energy injection; sharper, stronger bursts typically lead to a larger fraction of cool gas forming in the outflow. The abundance ratio of ions in the CGM may therefore change in response to the detailed historical pattern of star formation. For instance, outflows generated by star formation with short, intense bursts contain up to 60 per cent of their gas mass at temperatures < 5 X 10^4 K; for near-continuous star formation the figure is ≲ 5 per cent. Further study of cosmological simulations, and of idealised simulations with e.g., metal-cooling, magnetic fields and/or thermal conduction, will help to understand the precise signature of bursty outflows on observed ion abundances.</p> |
| spellingShingle | Suarez, T Pontzen, A Peiris, H Slyz, A Devriendt, J Bursty star formation feedback and cooling outflows |
| title | Bursty star formation feedback and cooling outflows |
| title_full | Bursty star formation feedback and cooling outflows |
| title_fullStr | Bursty star formation feedback and cooling outflows |
| title_full_unstemmed | Bursty star formation feedback and cooling outflows |
| title_short | Bursty star formation feedback and cooling outflows |
| title_sort | bursty star formation feedback and cooling outflows |
| work_keys_str_mv | AT suarezt burstystarformationfeedbackandcoolingoutflows AT pontzena burstystarformationfeedbackandcoolingoutflows AT peirish burstystarformationfeedbackandcoolingoutflows AT slyza burstystarformationfeedbackandcoolingoutflows AT devriendtj burstystarformationfeedbackandcoolingoutflows |