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- W173671898 abstract "M33(NGC 598),as one of the spirals in Local Group,is an excellent target for testing galactic chemical evolution theory.Owing to its proper distance and angular size,detailed observations of present gas distribution,star formation rate(SFR),and abundance properties are available. In this paper,the authors have established a chemical evolution model for M33 disk.They adopt two infall formulas,representing the collapse model and the accretion model respectively, to describe the growth of the disk with the advantage of ignoring complicated processes required in a Lambda CDM cosmology,and the influence of timescaleτhas been discussed.Apart from adopting a simple assumption of the constant infall timescaleτ,they also examine the outflow which is assumed to be proportional to the star formation rate.Since M33 is less massive compared with the Milky Way,the lower potential well would very probably result in a significant outflow during the evolution of disk by supernova explosions or other perturbations.Their motivation for the present model is to discuss the different roles of infall and outflow in building the M33 galaxy disk.They would like to know in what way the model could best reproduce the observed global properties. The main conclusions of this work are as follows:1) Short infall timescale will lead to low gas fraction,low SFR and high abundance in ISM.Because most of gas will fall onto the disk at early time,and fuel the star formation.When stars are dying,they eject the newly produced elements and enrich the ISM quickly.No matter the collapse model or the accretion model, the results are all consistent with the observations except for the abundance gradient if a longer infall time-scale(15 Gyr) is adopted.These means M33 should form through the slow accreting process.2) Outflow has significant influence on ISM enrichment,especially for the inner disk, but no obvious change in other model predictions.Due to the high SFR in the inner disk,more metals are carried out by outflowing gas and hence flatten the abundance gradient.The model results are consistent with observations when the outflow rate is comparable with SFR(b = 0.8). Outflow can not be neglected owing to the low abundance in M33 disk.3) The revised K-S SFR law which is similar to MW's can reproduce most of the observations by adopting long infall time-scale and considering outflow in our model.TheobservedSFR law doesn't work." @default.
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- W173671898 date "2009-01-01" @default.
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- W173671898 title "Chemical evolution of M33." @default.
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