Towards a Complete Library of Stellar Spectra for Evolutionary Synthesis

1996 ◽  
pp. 355-355 ◽  
Author(s):  
F. Cuisinier ◽  
Th. Lejeune ◽  
R. Buser
Keyword(s):  
Evolutionary Synthesis ◽  
Stellar Spectra

scholarly journals New Models for Massive Star Populations in Young Starbursts: Summary of the Models and Applications

1999 ◽  
Vol 186 ◽  
pp. 285-285
Author(s):  
Daniel Schaerer ◽  
William D. Vacca
Keyword(s):  
Emission Line ◽  
Stellar Evolution ◽  
Massive Star ◽  
Optical Emission ◽  
Emission Lines ◽  
Evolutionary Synthesis ◽  
Stellar Spectra ◽  
New Models ◽  
Helium Emission ◽  
Line Strengths

Using the latest stellar evolution models, theoretical stellar spectra, and a compilation of observed emission line strengths from Wolf-Rayet (WR) stars, we have constructed evolutionary synthesis models for young starbursts (Schaerer & Vacca 1997; see also Schaerer 1996). We provide detailed predictions of UV and optical emission line strengths for both the WR stellar lines and the major nebular hydrogen and helium emission lines, as a function of several input parameters related to the starburst episode.

scholarly journals Towards a Complete Library of Stellar Spectra for Evolutionary Synthesis

1996 ◽  
Vol 171 ◽  
pp. 355-355 ◽  
Author(s):  
F. Cuisinier ◽  
Th. Lejeune ◽  
R. Buser
Keyword(s):  
Chemical Evolution ◽  
Evolutionary Synthesis ◽  
Good Knowledge ◽  
Stellar Spectra ◽  
Synthetic Spectra ◽  
Cool Stars ◽  
Uneven Sampling ◽  
High Metallicity

The population and evolutionary synthesis of the integrated light of clusters and galaxies requires a good knowledge of the underlying stellar spectra. Libraries of observed stellar spectra can be used, but they have several disadvantages, e.g. uneven sampling — which causes problems in the integration phase. Furthermore, no comprehensive library of low– or high–metallicity stars does exist, which would be required to model chemical evolution. Libraries of synthetic spectra could — and should — solve these problems. Using Kurucz and more recent libraries dedicated to cool stars, we constituted a library covering the whole range of Teff: 50 000 – 2500 K.

Some problems of objective-prism spectra classification

1966 ◽  
Vol 24 ◽  
pp. 51-52
Author(s):  
E. K. Kharadze ◽  
R. A. Bartaya
Keyword(s):  
Short Wave ◽  
High Quality ◽  
Stellar Spectra ◽  
Objective Prism

The unique 70-cm meniscus-type telescope of the Abastumani Astrophysical Observatory supplied with two objective prisms and the seeing conditions characteristic at Mount Kanobili (Abastumani) permit us to obtain stellar spectra of a high quality. No additional design to improve the “climate” immediately around the telescope itself is being applied. The dispersions and photographic magnitude limits are 160 and 660Å/mm, and 12–13, respectively. The short-wave end of spectra reaches 3500–3400Å.

QUICK INTERPRETATION OF UNRESOLVED HYPERFINE AND/OR ZEEMAN STRUCTURES IN STELLAR SPECTRA

1988 ◽  
Vol 49 (C1) ◽  
pp. C1-263-C1-265 ◽  
Author(s):  
J. BAUCHE ◽  
J. OREG
Keyword(s):  
Stellar Spectra

Revising Plants, man and life: Edgar Anderson reshapes a classic book

2003 ◽  
Vol 30 (1) ◽  
pp. 85-96 ◽  
Author(s):  
Kim Kleinman
Keyword(s):  
Twentieth Century ◽  
Evolutionary Theory ◽  
Evolutionary Synthesis ◽  
Ernst Mayr ◽  
Active Participant ◽  
Evolutionary Mechanism ◽  
Popular Work ◽  
Scientific Attention ◽  
Key Events ◽  
Jesup Lectures

On at least four occasions, Edgar Anderson (1897–1969) began revising his book Plants, man and life (1952). Given both its place in Anderson's career and his place in the development of evolutionary theory in the mid-twentieth century, the emendations are noteworthy. Though a popular work, Plants, man and life served as the distillation of Anderson's ideas on hybridization as an evolutionary mechanism, the need for more scientific attention on domesticated and semi-domesticated plants, and the opportunities such plants provided for the study of evolution. Anderson was an active participant in several key events in what historians have come to call the Evolutionary Synthesis. For example, he and Ernst Mayr shared the 1941 Jesup Lectures on “Systematics and the origin of species”. Anderson's proposed revisions to his book reflect both an attempt to soften certain acerbic comments as well as an attempt to recast the book as a whole.

Introduction: Challenging the Modern Synthesis

2017 ◽  
Author(s):  
Denis M. Walsh ◽  
Philippe Huneman
Keyword(s):  
20Th Century ◽  
Cell Biology ◽  
Population Change ◽  
Modern Synthesis ◽  
Evolutionary Synthesis ◽  
Comparative Biology ◽  
Darwinian Theory ◽  
Modern Evolutionary Synthesis

The modern evolutionary synthesis arose out of the conjunction of the Mendelian theory of inheritance and the neo-Darwinian theory of population change early in the 20th century.1 In the nearly 100 years since its inception, the modern evolutionary synthesis has grown to encompass practically all fields of comparative biology—ecology, ethology, paleontology, systematics, cell biology, physiology, genetics, development. Theodosius Dobzhansky’s dictum—“nothing in biology makes sense except in the light of evolution” (...

Toward a Nonidealist Evolutionary Synthesis

2017 ◽  
Author(s):  
Stuart A. Newman
Keyword(s):  
Evolutionary Theory ◽  
Raw Material ◽  
Evolutionary Synthesis ◽  
Living Systems ◽  
Evolution Of Development ◽  
Search Process ◽  
Physical Processes ◽  
Explanatory Framework ◽  
Material Systems ◽  
Modern Physics

The received model of evolution sees all inherited features resulting from deterministic networks of interacting genes, implying that living systems are reducible to information in genetic programs. The model requires these programs and their associated phenotypes to have evolved by an isotropic search process occurring in gradual steps with no preferred morphological outcomes. The alternative is to recognize that clusters and aggregates of cells, the raw material of evolution, constitute middle-scale material systems. This implies the necessity of bringing the modern physics of mesoscale matter into the explanatory framework for the evolution of development. The relevant, often nonlinear, physical processes were mobilized at the inception of the phyla when their signature morphological outcomes first appeared and remain as efficient causes, albeit transformed, in present-day embryos. This physicogenetic perspective reengages with concepts of saltation, orthogenesis, and environment-induced plasticity long excluded from evolutionary theory.

Why Would We Call for a New Evolutionary Synthesis?

2017 ◽  
Author(s):  
Philippe Huneman
Keyword(s):  
Genotypic Variation ◽  
Modern Synthesis ◽  
Evolutionary Synthesis ◽  
Alternative Scheme ◽  
Random Nature

Considering challenges to the modern synthesis (MS), this chapter reconstructs an explanatory scheme proper to the MS. It contrasts it with the explanatory scheme proper to some alternatives to the MS. It considers which empirical facts should compel us to adopt the alternative scheme, or stand with the MS, or consider a weakly attenuated form of its explanatory scheme. Hence the last section focuses on the form of variation: Given that many findings are accumulating concerning the not purely random nature of variation, it asks which specific patterns of variation would be likely to support an alternative explanatory scheme. It argues that neither biased variation nor random genotypic variation is likely to vindicate a specific explanatory scheme.

Recovering the star formation history of galaxies through spectral fitting: Current challenges

2019 ◽  
Vol 15 (S359) ◽  
pp. 386-390
Author(s):  
Lucimara P. Martins
Keyword(s):  
Star Formation ◽  
Mass Function ◽  
Initial Mass Function ◽  
Star Formation History ◽  
Stellar Spectra ◽  
Spectral Fitting ◽  
Formation History ◽  
History Of ◽  
Nearby Galaxies ◽  
Extract Information

AbstractWith the exception of some nearby galaxies, we cannot resolve stars individually. To recover the galaxies star formation history (SFH), the challenge is to extract information from their integrated spectrum. A widely used tool is the full spectral fitting technique. This consists of combining simple stellar populations (SSPs) of different ages and metallicities to match the integrated spectrum. This technique works well for optical spectra, for metallicities near solar and chemical histories not much different from our Galaxy. For everything else there is room for improvement. With telescopes being able to explore further and further away, and beyond the optical, the improvement of this type of tool is crucial. SSPs use as ingredients isochrones, an initial mass function, and a library of stellar spectra. My focus are the stellar libraries, key ingredient for SSPs. Here I talk about the latest developments of stellar libraries, how they influence the SSPs and how to improve them.

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