After the launch and successful beginning of operations of the FERMI satellite, the topics related to high-energy observations of gamma-ray bursts have obtained a considerable attention by the scientific community. Undoubtedly, the diagnostic power of high-energy observations in constraining the emission processes and the physical conditions of

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The neutron star X-ray binary Aql X-1 shows quasi-periodic outbursts about once a year. These active states are relatively well covered in optical/infrared and X-ray domains. In contrast, at radio wavelengths the observations are very scarce (IAUC #5112; ATEL #286; ATEL #491). Following the reports of a new outburst of the object (ATEL #1970; ATEL

Most of our knowledge on young stars comes from snapshot observations: spectra and images taken at a single epoch, or at different epochs at different wavelengths. It is, however, known that many of the systems are variable. Variability at optical and near-infrared wavelength is mostly related to the central star itself. Mid-infrared flux changes

RXTE observations of the intermittent accreting millisecond X-ray pulsar HETE J1900.1-2455 (Kaaret et al. 2006 ApJ 638, 963; Galloway et al. 2007 ApJ 654, L73) showed a Type I X-ray burst on April 2 2009 (08:57 UTC). We detect strong burst oscillations during the peak and initial decay of the burst, drifting upwards from 375.5 Hz to 376.5 Hz

Polarized light provides the most reliable source of information at our disposal for diagnosing the physical properties of astrophysical plasmas, including the magnetic fields of the solar atmosphere. The interaction between radiation and hydrogen plus free electrons through Rayleigh and Thomson scattering gives rise to the polarization of the