Chemical evolution during gas-rich galaxy interactions

We perform and analyse a set of galaxy interactions performed by using a self-consistent chemo-hydrodynamical model which includes star formation, supernova (SN) feedback and chemical evolution. In agreement with previous works, we find that tidally induced low-metallicity gas inflows dilute the cen...

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Publicado:	2011
Materias:	Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p580_Perez http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p580_Perez
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00358711_v417_n1_p580_Perez
record_format	dspace
spelling	paper:paper_00358711_v417_n1_p580_Perez2023-06-08T15:01:32Z Chemical evolution during gas-rich galaxy interactions Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions We perform and analyse a set of galaxy interactions performed by using a self-consistent chemo-hydrodynamical model which includes star formation, supernova (SN) feedback and chemical evolution. In agreement with previous works, we find that tidally induced low-metallicity gas inflows dilute the central oxygen abundance and contribute to the flattening of the metallicity gradients. The tidally induced inflows trigger starbursts which increase the impact of Type II supernova (SN II) feedback injecting new chemical elements and driving galactic winds which modulate the metallicity distribution. Although α-enhancement in the central regions is detected as a result of the induced starbursts in agreement with previous works, our simulations suggest that this parameter can only provide a timing of the first pericentre mainly for non-retrograde encounters. In order to reproduce wet major mergers at low and high redshifts, we have run simulations with respectively 20 and 50 per cent of the disc in the form of gas. We find that the more gas-rich encounters behave similarly to the less rich ones, between the first and second pericentre, where low-metallicity gas inflows are triggered. However, the higher strength of the inflows triggered in the more gas-rich interactions produces larger metal dilution factors, which are modulated afterwards by the new chemical production by SN. We find that the more gas-rich interaction develops violent and clumpy star formation triggered by local instabilities all over the disc before the first pericentre, so that if these galaxies were observed at these early stages where no important tidally induced inflows have been able to be developed yet, they would tend to show an excess of oxygen. We find a global mean correlation of both the central abundances and the gradients with the strength of the star formation activity. However, the correlations are affected by orbital parameters, gas inflows and outflows, suggesting that it might be difficult to determine it from observations. Overall, our findings show that a consistent description of the gas dynamics and stellar evolution along the interactions is necessary to assess their effects on the chemical properties of the interstellar medium. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p580_Perez http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p580_Perez
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions
spellingShingle	Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions Chemical evolution during gas-rich galaxy interactions
topic_facet	Galaxies: abundances Galaxies: evolution Galaxies: formation Galaxies: interactions
description	We perform and analyse a set of galaxy interactions performed by using a self-consistent chemo-hydrodynamical model which includes star formation, supernova (SN) feedback and chemical evolution. In agreement with previous works, we find that tidally induced low-metallicity gas inflows dilute the central oxygen abundance and contribute to the flattening of the metallicity gradients. The tidally induced inflows trigger starbursts which increase the impact of Type II supernova (SN II) feedback injecting new chemical elements and driving galactic winds which modulate the metallicity distribution. Although α-enhancement in the central regions is detected as a result of the induced starbursts in agreement with previous works, our simulations suggest that this parameter can only provide a timing of the first pericentre mainly for non-retrograde encounters. In order to reproduce wet major mergers at low and high redshifts, we have run simulations with respectively 20 and 50 per cent of the disc in the form of gas. We find that the more gas-rich encounters behave similarly to the less rich ones, between the first and second pericentre, where low-metallicity gas inflows are triggered. However, the higher strength of the inflows triggered in the more gas-rich interactions produces larger metal dilution factors, which are modulated afterwards by the new chemical production by SN. We find that the more gas-rich interaction develops violent and clumpy star formation triggered by local instabilities all over the disc before the first pericentre, so that if these galaxies were observed at these early stages where no important tidally induced inflows have been able to be developed yet, they would tend to show an excess of oxygen. We find a global mean correlation of both the central abundances and the gradients with the strength of the star formation activity. However, the correlations are affected by orbital parameters, gas inflows and outflows, suggesting that it might be difficult to determine it from observations. Overall, our findings show that a consistent description of the gas dynamics and stellar evolution along the interactions is necessary to assess their effects on the chemical properties of the interstellar medium. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
title	Chemical evolution during gas-rich galaxy interactions
title_short	Chemical evolution during gas-rich galaxy interactions
title_full	Chemical evolution during gas-rich galaxy interactions
title_fullStr	Chemical evolution during gas-rich galaxy interactions
title_full_unstemmed	Chemical evolution during gas-rich galaxy interactions
title_sort	chemical evolution during gas-rich galaxy interactions
publishDate	2011
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v417_n1_p580_Perez http://hdl.handle.net/20.500.12110/paper_00358711_v417_n1_p580_Perez
_version_	1768545364749582336

Chemical evolution during gas-rich galaxy interactions

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