scholarly journals A Monte Carlo based simulation of the Galactic chemical evolution of the Milky Way Galaxy

2018 ◽  
Vol 481 (4) ◽  
pp. 5350-5369 ◽  
Author(s):  
Sandeep Sahijpal ◽  
Tejpreet Kaur
Keyword(s):  
Monte Carlo ◽  
Chemical Evolution ◽  
Milky Way ◽  
Galactic Chemical Evolution ◽  
Milky Way Galaxy

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 Observational constraints on the origin of the elements

2020 ◽  
Vol 635 ◽  
pp. A38 ◽  
Author(s):  
P. Eitner ◽  
M. Bergemann ◽  
C. J. Hansen ◽  
G. Cescutti ◽  
I. R. Seitenzahl ◽  
...  
Keyword(s):  
Chemical Evolution ◽  
Globular Clusters ◽  
Local Thermodynamic Equilibrium ◽  
Galactic Chemical Evolution ◽  
Galactic Disc ◽  
Milky Way Galaxy ◽  
Halo Stars ◽  
Type Ia ◽  
Low Metallicity ◽  
Different Sources

The abundance ratios of manganese to iron in late-type stars across a wide metallicity range place tight constraints on the astrophysical production sites of Fe-group elements. In this work, we investigate the chemical evolution of Mn in the Milky Way galaxy using high-resolution spectroscopic observations of stars in the Galactic disc and halo stars, as well as a sample of globular clusters. Our analysis shows that local thermodynamic equilibrium (LTE) leads to a strong imbalance in the ionisation equilibrium of Mn I and Mn II lines. Mn I produces systematically (up to 0.6 dex) lower abundances compared to the Mn II lines. Non-LTE (NLTE) radiative transfer satisfies the ionisation equilibrium across the entire metallicity range, of −3 ≲ [Fe/H] ≲ −1, leading to consistent abundances from both ionisation stages of the element. We compare the NLTE abundances with Galactic Chemical Evolution models computed using different sources of type Ia and type II supernova (SN Ia and SN II) yields. We find that a good fit to our observations can be obtained by assuming that a significant (∼75%) fraction of SNe Ia stem from a sub-Chandrasekhar (sub-Mch) channel. While this fraction is larger than that found in earlier studies (∼50%), we note that we still require ∼25% near-Mch SNe Ia to obtain solar [Mn/Fe] at [Fe/H] = 0. Our new data also suggest higher SN II Mn yields at low metallicity than typically assumed in the literature.

scholarly journals Chemical Evolution of R-process Elements in the Hierarchical Galaxy Formation

2015 ◽  
Vol 11 (S317) ◽  
pp. 318-319
Author(s):  
Yutaka Komiya ◽  
Toshikazu Shigeyama
Keyword(s):  
Neutron Star ◽  
Chemical Evolution ◽  
Galaxy Formation ◽  
Milky Way ◽  
Galactic Chemical Evolution ◽  
Halo Stars ◽  
R Process ◽  
Process Elements ◽  
Milky Way Halo

AbstractThe main astronomical source of r-process elements has not yet been identified. One plausible site is neutron star mergers (NSMs). From the perspective of Galactic chemical evolution, however, it has been pointed out that the NSM scenario is incompatible with observations. Recently, Tsujimoto & Shigeyama (2014) pointed out that NSM ejecta can spread into much larger volume than ejecta from a supernova. We re-examine the chemical evolution of r-process elements under the NSM scenario considering this difference in propagation of the ejecta. We find that the NSM scenario can be compatible with the observed abundances of the Milky Way halo stars.

scholarly journals Galactic Chemical Evolution

2003 ◽  
Vol 20 (4) ◽  
pp. 401-415 ◽  
Author(s):  
Brad K. Gibson ◽  
Yeshe Fenner ◽  
Agostino Renda ◽  
Daisuke Kawata ◽  
Hyun-chul Lee
Keyword(s):  
Boundary Condition ◽  
Galaxy Evolution ◽  
Chemical Evolution ◽  
Milky Way ◽  
State Of The Art ◽  
Galactic Chemical Evolution ◽  
Current State ◽  
Important Constraint

AbstractThe primary present-day observables upon which theories of galaxy evolution are based are a system’s morphology, dynamics, colour, and chemistry. Individually, each provides an important constraint to any given model; in concert, the four represent a fundamental (intractable) boundary condition for chemodynamical simulations. We review the current state-of-the-art semi-analytical and chemodynamical models for the Milky Way, emphasising the strengths and weaknesses of both approaches.

scholarly journals 1.3. First stellar iron abundance measurements in the Galactic center

1998 ◽  
Vol 184 ◽  
pp. 21-22 ◽  
Author(s):  
K. Sellgren ◽  
J. S. Carr ◽  
S. C. Balachandran
Keyword(s):  
Star Formation ◽  
Gas Phase ◽  
Chemical Evolution ◽  
Milky Way ◽  
Galactic Center ◽  
Star Formation History ◽  
Stellar Abundances ◽  
Milky Way Galaxy ◽  
Formation History ◽  
Iron Abundance

The disk of the Milky Way galaxy shows evidence for gas-phase abundances which increase with decreasing radius (Simpson et al. 1995; Afflerbach et al. 1997). Sustained star formation in the center of the Milky Way Galaxy may be fueled by inflow of inner disk gas (Serabyn & Morris 1996), suggesting that Galactic Center (GC) stars may be metal-rich. Measurements of stellar abundances in the GC allow us to explore the chemical evolution of our Galaxy's nucleus and to infer its star formation history.

scholarly journals The Milky Way Halo and the First Stars: New Frontiers in Galactic Archaeology

2009 ◽  
Vol 5 (H15) ◽  
pp. 184-184
Author(s):  
Timothy C. Beers ◽  
Jason Tumlinson ◽  
Brian O'Shea ◽  
Carolyn Peruta ◽  
Daniela Carollo
Keyword(s):  
Chemical Evolution ◽  
Milky Way ◽  
Galactic Chemical Evolution ◽  
Joint Effort ◽  
First Stars ◽  
Large Samples ◽  
New Models ◽  
First Galaxies ◽  
The Relationship ◽  
Milky Way Halo

AbstractWe discuss plans for a new joint effort between observers and theorists to understand the formation of the Milky Way halo back to the first epochs of chemical evolution. New models based on high-resolution N-body simulations coupled to simple models of Galactic chemical evolution show that surviving stars from the epoch of the first galaxies remain in the Milky Way today and should bear the nucleosynthetic imprint of the first stars. We investigate the key physical influences on the formation of stars in the first galaxies and how they appear today, including the relationship between cosmic reionization and surviving Milky Way stars. These models also provide a physically motivated picture of the formation of the Milky Ways “outer halo,” which has been identified from recent large samples of stars from SDSS. The next steps are to use these models to guide rigorous gas simulations of Milky Way formation, including its disk, and to gradually build up the fully detailed theoretical “Virtual Galaxy” that is demanded by the coming generation of massive Galactic stellar surveys.

scholarly journals Chemical evolution of galaxies: emerging dust and the different gas phases in a new multiphase code

2020 ◽  
Vol 494 (1) ◽  
pp. 146-160
Author(s):  
I Millán-Irigoyen ◽  
M Mollá ◽  
Y Ascasibar
Keyword(s):  
Chemical Evolution ◽  
Milky Way ◽  
Molecular Gas ◽  
Multiphase Model ◽  
Milky Way Galaxy ◽  
Gas Phases ◽  
Conversion Rates ◽  
Low Metallicity ◽  
Consistent Treatment ◽  
Physical Principles

ABSTRACT Dust plays an important role in the evolution of a galaxy, as it is one of the main ingredients for efficient star formation. Dust grains are also a sink/source of metals when they are created/destroyed, and, therefore, a self-consistent treatment is key in order to correctly model chemical evolution. In this work, we discuss the implementation of dust physics in our current multiphase model, which also follows the evolution of atomic, ionized and molecular gas. Our goal is to model the conversion rates among the different phases of the interstellar medium, including the creation, growth and destruction of dust, based, as far as possible, on physical principles rather than on phenomenological recipes. We first present the updated set of differential equations and then discuss the results. We calibrate our model against observations of the Milky Way Galaxy and compare its predictions with extant data. Our results are broadly consistent with the observed data for intermediate and high metallicities, but the models tend to produce more dust than is observed in the low-metallicity regime.

scholarly journals The evolution of the oxygen abundance radial gradient in the Milky Way Galaxy disk

2016 ◽  
Vol 12 (S323) ◽  
pp. 245-253
Author(s):  
Mercedes Mollá ◽  
Oscar Cavichia ◽  
Roberto D. D. Costa ◽  
Walter J. Maciel ◽  
Brad Gibson ◽  
...  
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Milky Way ◽  
Formation Rate ◽  
Milky Way Galaxy ◽  
Oxygen Abundance ◽  
Radial Gradient ◽  
Rate Laws ◽  
Galaxy Disk ◽  
Low Mass

AbstractWe review the state of our chemical evolution models for spiral and low mass galaxies. We analyze the consequences of using different stellar yields, infall rate laws and star formation prescriptions in the time/redshift evolution of the radial distributions of abundances, and other quantities as star formation rate or gas densities, in the Milky Way Galaxy; In particular we will study the evolution of the oxygen abundance radial gradient analyzing its relation with the ratio SFR/infall. We also compare the results with our old chemical evolution models, cosmological simulations and with the existing data, mainly with the planetary nebulae abundances.

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