Patel, M. R.; Zarnecki, J. C. and Towner, M. C.
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The UV environment on planetary surfaces is of extreme importance in a wide range of scientific disciplines, from meteorological considerations to the viability of biological organisms. Presented here is theoretical modelling for the transmission of ultraviolet radiation (190-400nm) through the martian atmosphere for a variety of possible cases, resulting in surface spectra. Knowledge of the UV transmission gives in-sight into how significant dust presence on Mars interacts with incoming solar radiation, and also yields information on the effect of biologically damaging UV-C on organisms and organic products on the surface. Surface fluxes are calculated using a radiative transfer approximation, for a range of dust loading and ozone abundance. Effects of direct and diffuse illuminance are also highlighted.
In-situ measurements of the UV flux will be possible for the first time onboard the Beagle 2 probe, scheduled to land on Mars in 2003. The instrument will measure the flux at five passbands in the UV, and also measure the total UV dose between 200-400nm throughout the mission lifetime.
|Item Type:||Conference Item|
|Copyright Holders:||2002 Astronomical Society of the Pacific|
|Extra Information:||ISBN: 1-58381-109-5|
|Academic Unit/Department:||Science > Physical Sciences
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|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Patricia Taylor|
|Date Deposited:||15 Feb 2012 10:00|
|Last Modified:||15 Feb 2012 10:00|
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