Time on Earth

Time Measurement and Earth Rotation

Calculations on space-time curvature within the Earth and Sun

One aspect of the relativistic space-time curvature due to the presence of mass is the breakdown of Euclidean (fiat-space) geometry. For example, the diameter of a spherical mass is greater than the result obtained by dividing the circumference by π. The objective of this article is to determine the amount of discrepancy between ”relativistic” and” non-relativistic” diameters for objects such a...

Time in the Geological past of Earth

1. Geological Time: A Summary 2. Reconstruction and Relative Dating of Earth History 2.1. Early Ideas and Basic Principles 2.2. Uniformitarianism and Catastrophism 2.3. Geological Catastrophes and Events: Particular Historical Geological Phenomena 2.4. Rates of Geological Processes in Terms of Human Timescales 2.4.1. Earth Crust Movements 2.4.2. Plutonic and Volcanic Processes 2.4.3. Weathering...

A numerical time ephemeris of the Earth

We present a time ephemeris of the Earth, TE405, which approximates a relativistic time-dilation integral from 1600 to 2200 using numerical quadrature of quantities supplied by the recent JPL ephemeris, DE405. The integral is required to transform between terrestrial time, TT, and the (solar-system) barycentric time scales Teph or TCB. Teph is a linear transformation of TCB that represents the ...

Approximate earth mover's distance in linear time

Theorem 2 ([3]). f ∈ Lloc(R n), belongs to Cs(Rn) if and only if, in a wavelet decomposition of regularity r ≥ 1 > s there exist constants C0 and C1 such that, Approx. coeffs.: |fk| ≤ C0, k ∈ Z n and Detail coeffs.: |fλ| ≤ C12 −j(n/2+s), λ ∈ Λj, j ≥ 0 (1) Lemma 1. If 0 < s < 1 and (1) holds, then f ∈ Cs(Rn) with CH(f ) < C such that a12(ψ; s)C1 ≤ C ≤ a21(ψ; s)C0 + a22(ψ; s)C1 (2) For discrete d...