28242232
The RNA of turnip yellow mosaic virus exhibits icosahedral order.
Difference electron density maps, based on structure factor amplitudes and experimental phases from crystals of wild-type turnip yellow mosaic virus and those of empty capsids prepared by freeze-thawing, show a large portion of the encapsidated RNA to have an icosahedral distribution. Four unique segments of base-paired, double-helical RNA, one to two turns in length, lie between 33-A and 101-A radius and are organized about either 2-fold or 5-fold icosahedral axes. In addition, single-stranded loops of RNA invade the pentameric and hexameric capsomeres where they contact the interior capsid surface. The remaining RNA, not seen in electron density maps, must serve as connecting links between these secondary structural elements and is likely icosahedrally disordered. The distribution of RNA observed crystallographically appears to be in agreement with models based on biochemical data and secondary structural analyses.
38714824
The structure of tomato aspermy virus by X-ray crystallography.
The three-dimensional structure of tomato aspermy virus (TAV) has been solved by X-ray crystallography and refined to an R factor of 0.218 for 3.4-40 A data (effective resolution of 4A). Molecular replacement, using cucumber mosaic virus (Smith et al., 2000), provided phases for the initial maps used for model building. The coat protein of the 280 A diameter virion has the canonical "Swiss roll" beta-barrel topology with a distinctive amino-terminal alpha-helix directed into the interior of the virus where it interacts with encapsidated RNA. The N-terminal helices are joined to the beta-barrels of protein subunits by extended polypeptides of six amino acids, which serve as flexible hinges allowing movement of the helices in response to local RNA distribution. Segments of three nucleotides of partially disordered RNA interact with the capsid, primarily through arginine residues, at interfaces between A and B subunits. Side chains of cys64 and cys106 form the first disulfide observed in a cucumovirus, including a unique cysteine, 106, in a region otherwise conserved. A positive ion, putatively modeled as a Mg(+)ion, lies on the quasi-threefold axis surrounded by three quasi-symmetric glutamate 175 side chains.
26621224
The LISA Optimal Sensitivity
The multiple Doppler readouts available on the Laser Interferometer Space Antenna (LISA) permit simultaneous formation of several interferometric observables. All these observables are independent of laser frequency fluctuations and have different couplings to gravitational waves and to the various LISA instrumental noises. Within the functional space of interferometric combinations LISA will be able to synthesize, we have identified a triplet of interferometric combinations that show optimally combined sensitivity. As an application of the method, we computed the sensitivity improvement for sinusoidal sources in the nominal, equal-arm LISA configuration. In the part of the Fourier band where the period of the wave is longer than the typical light travel-time across LISA, the sensitivity gain over a single Michelson interferometer is equal to $\sqrt{2}$. In the mid-band region, where the LISA Michelson combination has its best sensitivity, the improvement over the Michelson sensitivity is slightly better than $\sqrt{2}$, and the frequency band of best sensitivity is broadened. For frequencies greater than the reciprocal of the light travel-time, the sensitivity improvement is oscillatory and $\sim \sqrt{3}$, but can be greater than $\sqrt{3}$ near frequencies that are integer multiples of the inverse of the one-way light travel-time in the LISA arm.
18125734
Contribution of Compact Mass Transferring Systems to the Galactic Gravitational Wave Background
Compact object binaries, mostly double with dwarfs, are believed to be a potential source of confusion-limited noise for the Laser Interferometer Space Antenna (LISA). In a specific frequency range, this noise may rise above the instrumental noise sources and hence hinder detection of other types of signals, e.g. extreme mass ratio inspirals of stellar mass objects into supermassive black holes. In most previous studies only detached populations of compact object binaries have been considered. Here, we investigate the influence of Galactic populations of compact mass transferring binaries on the shape and strength of the LISA signal and compare our results with the signal for detached binaries only. Our population synthesis includes all binary systems containing two compact remnants. It is found that 99.5% of these systems are double white dwarfs, and therefore we consider only binaries consisting of two white dwarfs when calculating the LISA signal. We find that the mass transferring binaries contributing to the confusion limited noise dominate the population of LISA systems by number (60%), due to their long lifetimes (few Gyrs). However, due to the very specific physical properties of mass transferring systems, it is found that their contribution to the noise is negligible at low frequencies and detached systems will set the magnitude of the confusion-limited signal in this range. However, the mass transferring systems begin to dominate the signal at higher frequencies (f>6 mHz). The transition frequency at which the confusion limited regime becomes important is found at 4 mHz. The addition of mass transferring systems tends to slightly increase the transition frequency (from 3.5 to 4 mHz).