Planetary Nebulae and the Chemical Evolution of Galaxies

1983 ◽  
pp. 463-472
Author(s):  
Alfonso Serrano
Keyword(s):  
Chemical Evolution ◽  
Planetary Nebulae ◽  
Evolution Of Galaxies

scholarly journals What do planetary nebulae and H II regions reveal about the chemical evolution of nearby dwarf galaxies?

2018 ◽  
Vol 14 (S344) ◽  
pp. 161-177 ◽  
Author(s):  
Denise R. Gonçalves
Keyword(s):  
Chemical Evolution ◽  
Local Group ◽  
Planetary Nebulae ◽  
H Ii Regions ◽  
Chemical Abundances ◽  
Local Universe ◽  
Time Line ◽  
Nearby Galaxies ◽  
H Ii Region ◽  
Age Range

AbstractThe Local Group contains a great number of dwarf irregulars and spheroidals, for which the spectroscopy of individual stars can be obtained. Thus, the chemical evolution of these galaxies can be traced, with the only need of finding populations spanning a large age range and such that we can accurately derive the composition. Planetary nebulae (PNe) are old- and intermediate-age star remnants and their chemical abundances can be obtained up to 3-4 Mpc. H ii regions, which are brighter and much easily detected, represent galaxies young content. PNe and H ii regions share similar spectroscopic features and are analysed in the same way. Both are among the best tracers of the chemical evolution allowing to draw the chemical time line of nearby galaxies. The focus in this review are the PN and H ii region populations as constraints to the chemical evolution models and the mass-metallicity relation of the local universe.

scholarly journals Abundance gradients from Planetary Nebulae in the galactic disk

1997 ◽  
Vol 180 ◽  
pp. 397-404 ◽  
Author(s):  
W.J. Maciel
Keyword(s):  
Chemical Evolution ◽  
Spiral Galaxies ◽  
Galactic Disk ◽  
Chemical Elements ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Additional Constraint ◽  
Established Fact ◽  
Metallicity Distribution

Radial abundance gradients in the disks of spiral galaxies are made evident from observations of ionized nebulae (HII regions, planetary nebulae, and SNRs) and stars. They have been observed for several chemical elements, and their presence is an established fact, despite some inconsistencies in the results. Therefore, these gradients can be considered as an additional constraint to the chemical evolution models, as the age-metallicity relation or the metallicity distribution of the G-dwarfs.

scholarly journals ASCA Observations of the Abell 496 Cluster of Galaxies

1998 ◽  
Vol 188 ◽  
pp. 304-305
Author(s):  
I. Hatsukade ◽  
J. Ishizaka ◽  
M. Yamauchi ◽  
K. Takagishi
Keyword(s):  
Mass Flow Rate ◽  
Chemical Evolution ◽  
Mass Flow ◽  
Relative Abundance ◽  
Flow Rate ◽  
Metal Distribution ◽  
Rich Cluster ◽  
Cooling Flow ◽  
Evolution Of Galaxies ◽  
Cluster Of Galaxies

The metal in the intracluster medium (ICM) has been ejected or stripped from galaxies. Thus measurements of the metal distribution and the relative abundance of elements, in particular Si/Fe, are important to study the evolution of galaxies, as well as to study the chemical evolution of the ICM. We present the results from ASCA observations of Abell 496 cluster of galaxies. A496 is a nearby rich cluster with a central cD galaxy. At the redshift z=0.0327 of A496, 1 arcmin is 53kpc, where we assumed H0 = 50kms−1Mpc−1, q0 = 0.5. A496 is known as a cooling flow cluster. Edge and Stewart (1991) obtained the mass flow rate of and the cooling radius of 177 ± 52kpc.

scholarly journals Chemical evolution of the galactic interstellar medium: abundance gradients

1979 ◽  
Vol 84 ◽  
pp. 307-316 ◽  
Author(s):  
Manuel Peimbert
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Planetary Nebulae ◽  
Observational Evidence ◽  
H Ii Regions

Recent abundance determinations of galactic H II regions and planetary nebulae are reviewed. The presence of O/H and N/H abundance gradients is well established; there is observational evidence indicating the presence of N/S, He/H and C/H abundance gradients. Some implications of these results are discussed.

scholarly journals Relations between the galactic evolution and the stellar evolution

1984 ◽  
Vol 105 ◽  
pp. 541-548 ◽  
Author(s):  
Jean Audouze
Keyword(s):  
Chemical Evolution ◽  
Stellar Evolution ◽  
Galactic Evolution ◽  
Evolution Of Galaxies ◽  
The Impact

The question which has been raised in many chapters of this book is about the existence of constraints on stellar evolution coming from related topics like cosmology or in the case of the present chapter the chemical evolution of the galaxies. As it will be seen in this contribution it seems wiser to consider that chemical evolution of galaxies is indeed related to the problem of stellar evolution discussed here but is not going to provide as many constraints on it as one would expect. The purpose of this presentation is therefore to outline the principal relations between these two fields and to discuss the impact of some recent works on them.

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