A unified construction of stellar evolution and chemical evolution models for the multiple populations in globular clusters

2019 ◽  
Vol 14 (S351) ◽  
pp. 302-304
Author(s):  
Sohee Jang ◽  
Jenny J. Kim ◽  
Young-Wook Lee
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Globular Clusters ◽  
Evolution Model ◽  
Star Formation History ◽  
Multiple Populations ◽  
Rr Lyrae ◽  
Formation History ◽  
Type Ab ◽  
Chemical Evolution Model

AbstractRecent investigations of multiple stellar populations in globular clusters (GCs) suggest that the horizontal-branch (HB) morphology and mean period of type ab RR Lyrae variables are mostly sensitive to helium abundance, while the star formation timescale has the greatest effect on our chemical evolution model constructed to reproduce the Na-O anti-correlation of GCs. Therefore, by combining the results from synthetic HB model with those from chemical evolution model, we could put better constraints on star formation history and chemical evolution in GCs with multiple populations. From such efforts made for four GCs, M4, M5, M15, and M80, we find that consistent results can be obtained from these two independent models.

Stellar population synthesis of galaxies with chemical evolution model

2019 ◽  
Vol 15 (S341) ◽  
pp. 147-151
Author(s):  
Shiyin Shen ◽  
Jun Yin
Keyword(s):  
Chemical Evolution ◽  
Stellar Population ◽  
Local Group ◽  
Evolution Model ◽  
Star Formation History ◽  
Population Synthesis ◽  
Formation History ◽  
Fitting Algorithm ◽  
Stellar Population Synthesis ◽  
Chemical Evolution Model

AbstractThe derivation of accurate stellar populations of galaxies is a non-trivial task because of the well-known age-metallicity degeneracy. We aim to break this degeneracy by invoking a chemical evolution model (CEM) for isolated disk galaxy, where its metallicity enrichment history (MEH) is modelled to be tightly linked to its star formation history (SFH). Our CEM has been successfully tested on several local group dwarf galaxies whose SFHs and MEHs have been both independently measured from deep colour-magnitude diagrams of individual stars. By introducing the CEM into the stellar population fitting algorithm as a prior, we expect that the SFH of galaxies could be better constrained.

scholarly journals Dynamical and Chemical Evolution of IZw18

2004 ◽  
Vol 21 (2) ◽  
pp. 157-160
Author(s):  
Simone Recchi
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Dwarf Galaxy ◽  
Star Formation History ◽  
Intermediate Mass ◽  
Intermediate Mass Stars ◽  
Formation History ◽  
Type Ia ◽  
Ia Supernovae ◽  
Detailed Chemical

AbstractWe study the effect of different star formation regimes on the dynamical and chemical evolution of IZw18, the most metal-poor dwarf galaxy locally known. To do that we adopt a two-dimensional hydrocode coupled with detailed chemical yields originating from Type II and Type Ia supernovae and from intermediate-mass stars. Particular emphasis is devoted to the problem of mixing of metals. We conclude that, under particular conditions, cooling of metals occurs with a timescale of the order of 10 Myr, thus confirming the hypothesis of instantaneous mixing adopted in chemical evolution models. We try to draw conclusions about the star formation history and the age of the last burst in IZw18.

scholarly journals STAR FORMATION HISTORY AND CHEMICAL EVOLUTION OF THE SEXTANS DWARF SPHEROIDAL GALAXY

2009 ◽  
Vol 703 (1) ◽  
pp. 692-701 ◽  
Author(s):  
Myung Gyoon Lee ◽  
In-Soo Yuk ◽  
Hong Soo Park ◽  
Jason Harris ◽  
Dennis Zaritsky
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Star Formation History ◽  
Formation History

scholarly journals The LMC Centre Unfolding

1999 ◽  
Vol 190 ◽  
pp. 357-358 ◽  
Author(s):  
A. Ardeberg ◽  
P. Linde ◽  
B. Gustafsson
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Star Formation History ◽  
Formation History

We study star formation history and chemical evolution in the LMC Bar centre. With the HST PC and WFC plus uvby photometry, we find 30% of the stars younger than 200 My and evidence for reduced star formation 3 to 0.2 Gy ago. The overall [Fe/H] is −0.5. Many stars older than 4 Gy contradict a very young Bar.

scholarly journals A Comparison of Chemical Evolution between the Milky Way and M31 Galaxy

2006 ◽  
Vol 2 (S235) ◽  
pp. 313-313
Author(s):  
J. Yin ◽  
J.L. Hou ◽  
R.X. Chang ◽  
S. Boissier ◽  
N. Prantzos
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Milky Way ◽  
Local Group ◽  
Spiral Galaxies ◽  
Star Formation History ◽  
Milky Way Galaxy ◽  
Andromeda Galaxy ◽  
Formation History ◽  
Formation And Evolution

Andromeda galaxy (M31,NGC224) is the biggest spiral in the Local Group. By studying the star formation history(SFH) and chemical evolution of M31, and comparing with the Milky Way Galaxy, we are able to understand more about the formation and evolution of spiral galaxies.

scholarly journals SMART for the Next Decade

2009 ◽  
Vol 5 (S262) ◽  
pp. 291-294
Author(s):  
Myung Gyoon Lee ◽  
In-Soo Yuk ◽  
Sungsoon Lim
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Star Formation History ◽  
Formation History

AbstractSMART is a model to derive both star formation history and chemical evolution simultaneously from color-magnitude diagrams of resolved stars in a galaxy. We present current progress and discuss the prospects of SMART for the next decade.

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