889 research outputs found

    Novel antibodies against RCD-8 as a tool to study processing bodies

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    Aim. To develop the model system for processing bodies (PBs) state monitoring and accomplish it in the future as a possible read-out of mTOR activity in mammalian cells. Methods. In course of this study we raised polyclonal antibodies against one of the PBs scaffold proteins – RCD-8 and employed cell imaging technique. Results. It has been shown that the obtained antibodies recognize the intracellular structures, namely PBs. The detected protein co-localized with known marker of PBs – DCP1a, and partly with marker of SGs – CPEB. Conclusions. Based on changes of PBs number and size in cells after exposure to known inductors or inhibitors of PB formation we prove the specificity of generated antibodies and possibility of their application for studies on the processing bodies dynamics controlled by mTOR-dependent signalin

    Improved Constraints on the Preferential Heating and Acceleration of Oxygen Ions in the Extended Solar Corona

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    We present a detailed analysis of oxygen ion velocity distributions in the extended solar corona, based on observations made with the Ultraviolet Coronagraph Spectrometer (UVCS) on the SOHO spacecraft. Polar coronal holes at solar minimum are known to exhibit broad line widths and unusual intensity ratios of the O VI 1032, 1037 emission line doublet. The traditional interpretation of these features has been that oxygen ions have a strong temperature anisotropy, with the temperature perpendicular to the magnetic field being much larger than the temperature parallel to the field. However, recent work by Raouafi and Solanki suggested that it may be possible to model the observations using an isotropic velocity distribution. In this paper we analyze an expanded data set to show that the original interpretation of an anisotropic distribution is the only one that is fully consistent with the observations. It is necessary to search the full range of ion plasma parameters to determine the values with the highest probability of agreement with the UVCS data. The derived ion outflow speeds and perpendicular kinetic temperatures are consistent with earlier results, and there continues to be strong evidence for preferential ion heating and acceleration with respect to hydrogen. At heliocentric heights above 2.1 solar radii, every UVCS data point is more consistent with an anisotropic distribution than with an isotropic distribution. At heights above 3 solar radii, the exact probability of isotropy depends on the electron density chosen to simulate the line-of-sight distribution of O VI emissivity. (abridged abstract)Comment: 19 pages (emulateapj style), 13 figures, ApJ, in press (v. 679; May 20, 2008

    Development of a drive that provides torque transmission to the drive shaft performing additional reciprocating motion

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    Synthesis of the tumbling machine spatial mechanism

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    Development of the four-link hinged mechanism of barreling machine drive

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    Development of a drive that provides the torque transmission to the drive shaft of the machine, performing additional reciprocating movement

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    Transition Region Emission and Energy Input to Thermal Plasma During the Impulsive Phase of Solar Flares

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    The energy released in a solar flare is partitioned between thermal and non-thermal particle energy and lost to thermal conduction and radiation over a broad range of wavelengths. It is difficult to determine the conductive losses and the energy radiated at transition region temperatures during the impulsive phases of flares. We use UVCS measurements of O VI photons produced by 5 flares and subsequently scattered by O VI ions in the corona to determine the 5.0 < log T < 6.0 transition region luminosities. We compare them with the rates of increase of thermal energy and the conductive losses deduced from RHESSI and GOES X-ray data using areas from RHESSI images to estimate the loop volumes, cross-sectional areas and scale lengths. The transition region luminosities during the impulsive phase exceed the X-ray luminosities for the first few minutes, but they are smaller than the rates of increase of thermal energy unless the filling factor of the X-ray emitting gas is ~ 0.01. The estimated conductive losses from the hot gas are too large to be balanced by radiative losses or heating of evaporated plasma, and we conclude that the area of the flare magnetic flux tubes is much smaller than the effective area measured by RHESSI during this phase of the flares. For the 2002 July 23 flare, the energy deposited by non-thermal particles exceeds the X-ray and UV energy losses and the rate of increase of the thermal energy.Comment: 20 pages, 3 figures To appear in Ap
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