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Crystal Structure of a Putative Histidine-containing Phosphotransfer Protein from Oryza sativa
Euiyoung Bae,Eduard Bitto,Craig A. Bingman,Simon T. Allard,Gary E. Wesenberg,Russell L. Wrobel,Brian G. Fox,George N. Phillips, Jr 한국응용생명화학회 2010 Applied Biological Chemistry (Appl Biol Chem) Vol.53 No.6
Os09g0567400 codes for a hypothetical protein from Oryza sativa that is annotated as the “Histidine-containing phosphotransfer (Hpt) protein”. Hpt domain is a protein module with a histidine residue mediating phosphotransfer reaction in the histidine-aspartate phosphorelay system. We report here the crystal structure and analysis of Os09g0567400.
Crystal Structure of a Putative Histidine-containing Phosphotransfer Protein from Oryza sativa
Bae, Eui-Young,Bitto, Eduard,Bingman, Craig A.,Allard, Simon T.,Wesenberg, Gary E.,Wrobel, Russell L.,Fox, Brian G.,Phillips, George N. Jr. The Korean Society for Applied Biological Chemistr 2010 Applied Biological Chemistry (Appl Biol Chem) Vol.53 No.6
Os09g0567400 codes for a hypothetical protein from Oryza sativa that is annotated as the "Histidine-containing pbospbotransfer (Hpt) protein". Hpt domain is a protein module with a histidine residue mediating phosphotransfer reaction in the bistidine-aspartate phosphorelay system. We report here the crystal structure and analysis of Os09g0567400.
A STUDY OF THE PHOTOMETRIC VARIABILITY OF THE PECULIAR MAGNETIC WHITE DWARF WD 1953-011
Valyavin, G.,Antonyuk, K.,Plachinda, S.,Clark, D. M.,Wade, G. A.,Machado, Lester Fox,Alvarez, M.,Lopez, J. M.,Hiriart, D.,Han, Inwoo,Jeon, Young-Beom,Bagnulo, S.,Zharikov, S. V.,Zurita, C.,Mujica, R. IOP Publishing 2011 The Astrophysical journal Vol.734 No.1
<P>We present and interpret simultaneous new photometric and spectroscopic observations of the peculiar magnetic white dwarf WD 1953-011. The flux in the V-band filter and intensity of the Balmer spectral lines demonstrate variability with the rotation period of about 1.45 days. According to previous studies, this variability can be explained by the presence of a dark spot having a magnetic nature, analogous to a sunspot. Motivated by this idea, we examine possible physical relationships between the suggested dark spot and the strong-field magnetic structure (magnetic 'spot' or 'tube') recently identified on the surface of this star. Comparing the rotationally modulated flux with the variable spectral observables related to the magnetic 'spot,' we establish their correlation and therefore their physical relationship. Modeling the variable photometric flux assuming that it is associated with temperature variations in the stellar photosphere, we argue that the strong-field area and dark, low-temperature spot are comparable in size and located at the same latitudes, essentially overlapping each other with a possible slight longitudinal shift. In this paper, we also present a new, improved value of the star's rotational period and constrain the characteristics of the thermal inhomogeneity over the degenerate's surface.</P>
Suppression of cooling by strong magnetic fields in white dwarf stars
Valyavin, G.,Shulyak, D.,Wade, G. A.,Antonyuk, K.,Zharikov, S. V.,Galazutdinov, G. A.,Plachinda, S.,Bagnulo, S.,Machado, L. Fox,Alvarez, M.,Clark, D. M.,Lopez, J. M.,Hiriart, D.,Han, Inwoo,Jeon, Young Nature Publishing Group, a division of Macmillan P 2014 Nature Vol.515 No.7525
Isolated cool white dwarf stars more often have strong magnetic fields than young, hotter white dwarfs, which has been a puzzle because magnetic fields are expected to decay with time but a cool surface suggests that the star is old. In addition, some white dwarfs with strong fields vary in brightness as they rotate, which has been variously attributed to surface brightness inhomogeneities similar to sunspots, chemical inhomogeneities and other magneto-optical effects. Here we describe optical observations of the brightness and magnetic field of the cool white dwarf WD 1953-011 taken over about eight years, and the results of an analysis of its surface temperature and magnetic field distribution. We find that the magnetic field suppresses atmospheric convection, leading to dark spots in the most magnetized areas. We also find that strong fields are sufficient to suppress convection over the entire surface in cool magnetic white dwarfs, which inhibits their cooling evolution relative to weakly magnetic and non-magnetic white dwarfs, making them appear younger than they truly are. This explains the long-standing mystery of why magnetic fields are more common amongst cool white dwarfs, and implies that the currently accepted ages of strongly magnetic white dwarfs are systematically too young.
Fox, C.J.,Moon, S.Y.,Iaria, G.,Barton, J.J.S. Academic Press 2009 NeuroImage Vol.44 No.2
The recognition of facial identity and expression are distinct tasks, with current models hypothesizing anatomic segregation of processing within a face-processing network. Using fMRI adaptation and a region-of-interest approach, we assessed how the perception of identity and expression changes in morphed stimuli affected the signal within this network, by contrasting (a) changes that crossed categorical boundaries of identity or expression with those that did not, and (b) changes that subjects perceived as causing identity or expression to change, versus changes that they perceived as not affecting the category of identity or expression. The occipital face area (OFA) was sensitive to any structural change in a face, whether it was identity or expression, but its signal did not correlate with whether subjects perceived a change or not. Both the fusiform face area (FFA) and the posterior superior temporal sulcus (pSTS) showed release from adaptation when subjects perceived a change in either identity or expression, although in the pSTS this effect only occurred when subjects were explicitly attending to expression. The middle superior temporal sulcus (mSTS) showed release from adaptation for expression only, and the precuneus for identity only. The data support models where the OFA is involved in the early perception of facial structure. However, evidence for a functional overlap in the FFA and pSTS, with both identity and expression signals in both areas, argues against a complete independence of identity and expression processing in these regions of the core face-processing network.
Molecular Mechanisms of Primary Aldosteronism
Sergei G. Tevosian,Shawna C. Fox,Hans K. Ghayee 대한내분비학회 2019 Endocrinology and metabolism Vol.34 No.4
Primary aldosteronism (PA) results from excess production of mineralocorticoid hormone aldosterone by the adrenal cortex. It isnormally caused either by unilateral aldosterone-producing adenoma (APA) or by bilateral aldosterone excess as a result of bilateraladrenal hyperplasia. PA is the most common cause of secondary hypertension and associated morbidity and mortality. While mostcases of PA are sporadic, an important insight into this debilitating disease has been derived through investigating the familial formsof the disease that affect only a minor fraction of PA patients. The advent of gene expression profiling has shed light on the genes andintracellular signaling pathways that may play a role in the pathogenesis of these tumors. The genetic basis for several forms of familial PA has been uncovered in recent years although the list is likely to expand. Recently, the work from several laboratories provided evidence for the involvement of mammalian target of rapamycin pathway and inflammatory cytokines in APAs; however, theirmechanism of action in tumor development and pathophysiology remains to be understood.