Globular base

Fi-ATPase has three a and three (I subunits arranged in alternation around the y subunit, which has a globular base and an extended coiled-coil domain (Fig. 1.10). All of the a and (1 subunits bind nucleotides, but only the three (1 subunits are catalytically active. The crystal structures of F1-ATPase provide views of distinct conformational states of the catalytic 3 subunits [30,35,36]. The centrally located and asymmetric y subunit forms a shaft, and it has been proposed that its orientation determines the conformations of the P subunits. The original crystal structure [30] of Fi-ATPase from bovine heart mitochondria led to the identification of three conformations of the P subunits Pg (empty), Prpp (ATP analog bound), and P p (ADP bound). In a more recent high-resolution crystal structure [35], the Prpp and Pqp subunits contain an ATP analog (ADP plus AIFJ) and the third catalytic... 

M J1990. Calculation of Conformational Ensembles from Potentials of Mean Force. An Approach o the Knowledge-Based Prediction of Local Structures in Globular Proteins. Journal of Molecular Siology 213 859-883. 

MI Sippl. Calculation of conformational ensembles from potentials of mean force. An approach to the knowledge-based prediction of local structures m globular proteins. I Mol Biol 213 859-883, 1990. 

Figure 28 A dendrimer-based approach for the design of globular protein mimic using glutamic (Glu) and aspartic (Asp) acids as the building blocks and adamantyl as the core [151].

Abstract. A review is presented on abundance determinations in stars of the Galactic bulge, both in the field and in globular clusters. Previous low-resolution spectroscopy results are revised. Recent high resolution and high S/N spectroscopy results based on Keck-Hires, Gemini-Phoenix and VLT-UVES data are presented. Finally, recent analyses of FLAMES data are discussed. 

Globular clusters are quite distant and their turnoff (TO) stars are intrinsically relatively faint. Following the advent of state-of-the-art instrumentation in 4m class telescopes, the first Li observations were carried on in GC stars, while with the advent of 8m class telescopes a quality jump occurred high quality spectra can now be obtained for the TO stars of the closest clusters, comparable to that available for field stars. In spite of this advancement, only a handful of published refereed papers have been devoted to the study of Li in globular cluster stars, and only one to beryllium. Based upon the wealth of information made available as a result of this data, I will present new findings concerning stellar mixing, primordial Li production and GC formation. 

Abstract. We present a new calibration of the Call triplet as metallicity indicator based in 4 globular and 11 open clusters which cover a range of metallicity -2<[Fe/H]<+0.1 and age 13<(Age/Gyr)<0.25. We use it to derive the metallicity distribution in two fields situated at 5 and 8 degrees from the center of the LMC. We show that the mean [Fe/H] of the LMC field decreases as we move away from the bar. 

It is the sequence and types of amino acids and the way that they are folded that provides protein molecules with specific structure, activity, and function. Ionic charge, hydrogen bonding capability, and hydrophobicity are the major determinants for the resultant three-dimensional structure of protein molecules. The a-chain is twisted, folded, and formed into globular structures, a-helicies, and P-sheets based upon the side-chain amino acid sequence and weak intramolecular interactions such as hydrogen bonding between different parts of the peptide... 

The Hamaker constant for interaction across water is about 6.5x10 21J for globular proteins (Nir 1977) and 2-5xl0 2oJ for such oxides as silica and metal oxides (Lyklema 1991c). Based on these values and applying (6) and (4) to a spherical protein molecule having a radius of 3 nm at a distance of 0.1 nm from the surface of a soil particle, AadsGdisp at... 

Identifying stars in globular and open clusters as either old stars from the primordial explosion or new stars formed after a supernova event is based on the atomic composition of the stars. The primary way of identifying the elements in any excited state is to study the atomic spectroscopy of the stellar spectrum, such as in Figure 4.2 and identify the atoms by assigning the spectra. This becomes a complicated process for the heavier elements but is very informative even for the simple H-atom spectra. 

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