Results 111 to 120 of about 4,101 (147)

Complete Data Analysis Workflow for Quantitative DIA Mass Spectrometry Using Nextflow. [PDF]

J Proteome Res
Perk M, Pietilä S, Välikangas T, Balint B, Suomi T, Elo LL.   +5 more
europepmc   +1 more source

Shifts in the Rhizosphere Bacterial Community and Improved Essential Oil Yield and Quality in Chamomilla recutita L. Plant Through Cyanobacterial Inoculation. [PDF]

Microb Ecol
Ibrahim D, Ali AH, Refaat A, Abdallah RZ, AbouZid S, Elsayed T, El Mokadem M, Berg G, Nour E.   +8 more
europepmc   +1 more source

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Abundances in Galaxies

Astrophysics and Space Science, 2001
To start things going, the following topics were suggested:* 1. Reliability of abundances Stars vs H ii regions H ii classical diagnostics Effects of shocks and inhomogeneities on H ii-region diagnostics H n new diagnostics Can reliable H ii-region diagnostics be developed for high metallicity?
B. E. J. Pagel, M. G. Edmunds
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Abundances in dwarf galaxies

AIP Conference Proceedings, 1989
In an attempt to discover regions of very low heavy element abundance, we have observed H II regions in 7 nearby, very low luminosity dwarf irregular galaxies. All yield oxygen abundances of less than one‐tenth of the solar value, and three are within a factor of two of the lowest oxygen abundance ever detected in an H II region.
Evan D. Skillman, R. C. Kennicutt
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Molecular Abundances in Galaxies

AIP Conference Proceedings, 2006
Two topics are discussed here. The first is an observational study on molecular abundance in nearby (< 10 Mpc) gas‐rich galaxies based on our ammonia survey and on data in literature. As a result, a systematically peculiar molecular abundance was found in a famous starburst galaxy M 82 regarding the formation mechanisms of molecules.
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The evolution of abundances in the galaxy

AIP Conference Proceedings, 1989
This very brief review of the evolution of the abundances in our Galaxy first recalls the main observational facts regarding such abundances which have to be taken into account by any model of chemical evolution of our Galaxy. After having defined what are the crucial parameters which define such models, the emphasis is made on two approaches: the ...
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Nebulae and abundances in galaxies

Publications of the Astronomical Society of the Pacific, 1986
Some current problems related to abundances in H II regions are briefly reviewed. For H II regions with measured electron temperatures, the discrepancy in O/H between the sun and the Orion Nebula is stressed. Studies of abundance and temperature variations within H II regions in NGC 604 are summarized.
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Lithium abundance at the formation of the Galaxy

Nature, 1982
The observed abundance of lithium in population I stars (young stars)1 seems to have been stable during the past 5 × 109 yr (ref. 2). This stability has been used previously1,3 to estimate the abundance of lithium at the time of formation of the Galaxy and at pre-galactic times1,3. But because the basis for this estimate was not completely satisfactory,
M. Spite, F. Spite
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Chemical Abundances in Galaxies

1988
This article is intended as a brief overview of chemical abundances in galaxies other than our own. Attention is concentrated on global properties of ellipticals and spirals, and the methods by which abundances are estimated. References are predominantly to work which has appeared since the review of Pagel and Edmunds (1981).
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