Very Long Wavelength Universe: view from the Moon ering Interacting Binaries with Halpha Surveys

Contains fulltext : 35038.pdf (preprint version ) (Open Access)Moon is an inevitable destination in the exploration Space by mankind The use of lunar bases as scientific laboratories is among the most attractive opportunities for the early stages of the exploration of the Moon Environmental conditions on the Moon are beneficial for various types of experimental research Very Long Wavelength radio astronomy is among the most attractive scientific disciplines for the suit of Moon-based laboratories During the last half a century space science has revolutionised astronomy by opening up several hitherto inaccessible windows in the spectrum The opening of each new spectral window has resulted in unexpected major discoveries and made it possible to obtain a comprehensive picture of physical processes in celestial sources by observing their emission in the entire EM-spectrum One of the last remaining unexplored regions of the spectrum is at the lowest radio frequencies Radio emission below 15 MHz wavelengths longer than 20 m is inaccessible from the ground due to ionospheric absorption and scattering Anthropogenic radio interference is also a very serious limiting factor for studying the Universe at wavelengths longer than 20 m The VLW radio region probes unique physical phenomena in the Universe begin itemize item The radiation mechanism that dominates radio astronomy at frequencies above about 50 MHz is synchrotron emission with extragalactic and galactic sources of radiation dominating the radio sky At lower frequencies other mechanisms such as plasma oscillations produce coherent radiation and the A deep (R ~ 19.5) photographic Halpha Survey of the southern Galactic Plane was recently completed using the UK Schmidt Telescope at the AAO. In addition, we have recently started a similar, CCD-based survey of the northern Galactic Plane using the Wide Field Camera on the INT. Both surveys aim to provide information on many types of emission line objects, such as planetary nebulae, luminous blue variables and interacting binaries. Here, we focus specifically on the ability of Halpha emission l