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A0535+26 is a slowly rotating pulsar accreting from the wind of a massive Be starand exhibits two cyclotron absorption lines in its X-ray spectrum, at about 45 and 100 keV, respectively. Unlike similar sources, no significant variations of the energy of its cyclotron lines with flux have beenobserved to date. The bright outburst of 2011 February thus offers a unique occasion to probe this peculiar behavior at flux levels not yet observed with presentday instruments. Here we report on the spectral and timing analysis of the data from the spectrometer SPI onboard INTEGRAL collected during the outburst. At the peak of the outburst the estimated luminosity is ∼4.9 × 10 37 erg s −1 . The fundamental cyclotron feature is detected at all flux levels, and its centroid energy is positively correlated with the flux of the source, confirming that A0535+26 is accreting at a sub-critical regime. The correlation seems to fall off at ∼10 37 erg s −1 , suggesting a transition from a Coulomb-stopping regime to a gasmediated shock regime. From the timing analysis we found that the pulsar was spinning up during most of the outburstand that the spin-up rate correlates with the flux of the source, althoughthe correlation is steeper than the one expected from the standard disk accretion theory. Finally, we show that the pulse profile of the source changes dramatically as the flux increases. At high luminosity the profile is highly asymmetric, implying an asymmetry in the geometry of the accretion flow.

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In this paper, we discuss the possibility of making geophysical measurements using the large-scale laser interferometrical gravitational wave antenna. An interferometer with suspended mirrors can be used as a gradiometer measuring variations of an angle between gravity force vectors acting on the spatially separated suspensions. We analyse the restrictions imposed by the atmospheric noises on the feasibility of such measurements. Two models of the atmosphere are invoked: a quiet atmosphere with a hydrostatic coupling of pressure and density and a dynamic model of moving region of the density anomaly (cyclone). Both models lead to similar conclusions up to numerical factors. Besides the hydrostatic approximation, we use a model of turbulent atmosphere with the pressure fluctuation spectrum ∼f −7/3 to explore the Newtonian noise in a higher frequency domain (up to 10 Hz) predicting the gravitational noise background for modern gravitational wave detectors. Our estimates show that this could pose a serious problem for realization of such projects. Finally, angular fluctuations of spatially separated pendula are investigated via computer simulation for some realistic atmospheric data giving the level estimate ∼10 −11 rad Hz −1/2 at frequency ∼10 −4 Hz. This looks promising for the possibility of the measurement of weak gravity effects such as Earth inner core oscillations.