VLBI from the Moon

Ground Based Vlbi Facilities – the European and Global Vlbi Network

For a comprehensive guide to the various array characteristics, corresponding correlator capabilities, range of diverse observing modes, different proposal submission procedures, user support etc., I refer the reader to the on-line web pages highlighted above. In this paper I have chosen to focus on a sub-set of these facilities, in particular the European VLBI Network (EVN) both in stand-alone...

Thermal Infrared Data from the Moon: Hazards

Introduction: Earth’s relatively clear thermal infrared (TIR) atmospheric windows correspond to the wavelength region of maximum emitted energy for the global average temperature (8-12 μm) as well as the temperature of most volcanoes/fires (3-5 μm). Furthermore, a majority of minerals have diagnostic emissivity spectra in the 8-12 μm region, making it excellent for the study of surface composit...

Zircon from the Moon , Earth and Mars

PSRD: Recent Gas Escape from the Moon

The Moon is generally thought to be geologically inactive, except for being pummeled by meteoroids of various sizes. The youngest returned igneous rocks are about 3 billion years old, although crater counting suggest some lava flows as young as a billion years. However, Peter Schultz (Brown University), Matthew Staid (Planetary Sciences Institute, Tucson), and Carlé Pieters (Brown University) r...

Estimation of EOP from VLBI: Direct Approach

The currently adopted strategy of EOP estimation from VLBI is to estimate six parameters: UT1, UT1 rate, pole positions and nutation o sets for each 24-hour session independently. Then the resulting time series of raw Earth orientation parameters are ltered and a regression analysis is performed in order to obtain nutation coe cients, polhode of the pole and other physical parameters. Thus, the...