Observations of solar magnetoconvection from a lunar base

Details Observations of solar magnetoconvection from a lunar base Observations of solar magnetoconvection from a lunar base

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aipc..207..111s&link_type=abstract

IN: Astrophysics from the moon; Proceedings of the Workshop, Annapolis, MD, Feb. 5-7, 1990 (A91-56576 24-89). New York, American

Astronomy and Astrophysics

Astrophysics

2

Convective Flow, Lunar Bases, Lunar Observatories, Solar Atmosphere, Solar Flares, Solar Magnetic Field, Photosphere, Plasma Dynamics, Solar Observatories, Spatial Resolution

Scientific paper

Extremely-high-resolution observations are required in order to make significant progress 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/sec. Spatial resolution must be better than 0.05 arcsec. Finally, spectral resolution of at least 10 exp 5 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 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.

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