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Earth exhibits remarkably few craters despite a similar cratering rate to the Moon, primarily due to geological processes such as erosion. Erosion constantly reshapes landscapes with varying rates across different regions. For example, the Himalayas see rates of 2-3 km/Ma, while areas like the Atacama Desert experience much lower rates at 0.5 m/Ma. Continuous uplift in mountain ranges counteracts erosion, indicating that the Earth is a dynamic planet. This interplay between erosion and uplift is vital in understanding the persistence of mountain topography.
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Question: If cratering rate on Earth is same as our Moon, why are their so few craters preserved? Answer: Erosion
Estimating natural erosion rates Accumulation of sediment versus time in alluvial fans. Ratio of cosmogenic isotopic creation rate/unit area to concentration/unit volume of sediments. Closure age of exposed minerals at surface plus increase of temperature with depth.
mm/y = m/Ka = Km/Ma Erosion Rate for Cascades ~ 0.05 – .25 Km/Ma
Summary of Erosion rates • Himalaya: 2-3 m/Ky = 2-3 km/Ma • Eastern edge of Bolivian Altiplano: 3 km/Ma • Cascades: 300 m/Ma • Massif Central (France): 50 m/Ma • Atacama Desert (Chile/Peru): 0.5 m/Ma • Central Australia: 0.5 m/Ma
Question If erosion can flatten mountain topography in only a few million years, why are there mountains at all?
Question: If erosion can flatten mountain topography in only a few million years, why are there mountains at all? Answer: Uplift is continuous Implication: Earth is a dynamic planet
L = cA½ Channel length and drainage area
Streamflow and drainage area… or River basins in Kentucky, USA, from Solyom and Tucker, 2004 Q = 0.0171*A0.9932 R2 = 0.9977
Channel Width: Data from the Clearwater River, Washington State, from Tomkin et al., 2003. Q = 0.1335 * A0.9 W=4.2*A0.42
W = b(AP)½ Should actually be discharge = Area x precipitation
Precip Distance Spatially Variable Precipitation, Ellis, Densmore & Anderson, 1999