Observations of Solar Magnetoconvection from a Lunar Base. (Reannouncement withNew Availability Information)

摘要

Extremely-high resolution observations are required in order to make significantprogress in solving some of the major problems in solar magnetoconvection. Temporal resolution demands a data stream that is uninterrupted for a minimum of thirty days, collected at very high rates of at least 100 megabits per second. Spatial resolution must be better than 35 km (0.05 arcsec). Finally, spectral resolution of at least 100,000 is needed. Since the magnetic structures of interest are very much three-dimensional, extending from below the solar surface up into the corona, observations from the IR, visible, EUV, XUV, and X-ray portions of the spectrum are essential. The above requirements preclude the use of Earth-based observatories, which are handicapped by turbulence (seeing) in the Earth's atmosphere, absorption of EUV and X-ray radiation, and the 24 hour day-night cycle. Thus the relevant facilities must operate from space. Whether they should be free-flyers or lunar-based depends partly on specific experiment requirements, and also on factors of cost, logistics, and timing. The results of an informal poll of some two dozen solar physicists regarding the advantages of solar observations from the moon are discussed.