Chemical evolution of the Magellanic Clouds: analytical models
نویسندگان
چکیده
منابع مشابه
Planetary Nebulae and the Chemical Evolution of the Magellanic Clouds
The determination of accurate chemical abundances of planetary nebulae (PN) in different galaxies allows us to obtain important constraints of chemical evolution models for these systems. We have a long term program to derive abundances in the galaxies of the Local Group, particularly the Large and Small Magellanic Clouds. In this work, we present our new results on these objects and discuss th...
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We investigate the dynamical and chemical evolution of the Large Magellanic Cloud (LMC) interacting with the Galaxy and the Small Magellanic Cloud (SMC) based on a series of self-consistent chemodynamical simulations. Our numerical models are aimed at explaining the entire properties of the LMC, i.e., the observed structure and kinematics of its stellar halo and disk components as well as the p...
متن کاملChemical composition of nebulosities in the magellanic clouds.
From photoelectric spectrophotometric data secured at Cerro Tololo Interamerican Observatory we have attempted to derive electron densities and temperatures, ionic concentrations, and chemical abundances of He, C, N, O, Ne, S, and Ar in nebulosities in the Magellanic Clouds. Although 10 distinct nebulosities were observed in the Small Cloud and 20 such objects in the Large Cloud, the most detai...
متن کاملChemical Evolution in the Large Magellanic Cloud
We present a new input parameter set of the Pagel model for the LMC (Pagel & Tautvaĭsienė 1998) in order to reproduce the observations, including the star formation rate (SFR) history. It is concluded that high ratio of A (∼ 0.17), which is the probability for 3-8M stars to explode as SNe Ia, is required. As a result, a steep initial mass function (IMF) slope or existence of the outflow is not ...
متن کاملAsymptotic giant branch evolution and its impact on the chemical evolution of the Milky Way and the Magellanic Clouds
The asymptotic giant branch (AGB) phase of stellar evolution is common to most stars of low and intermediate mass. Most of the carbon and nitrogen in the Universe is produced by AGB stars. The final fate of the AGB envelopes are represented by planetary nebulae (PN). By studying PN abundances and compare them with the yields of stellar evolution is possible to quantify carbon and nitrogen produ...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 1998
ISSN: 0035-8711,1365-2966
DOI: 10.1046/j.1365-8711.1998.01792.x