Exact(8)
The term basic solar motion has been used by some astronomers to define the motion of the Sun relative to stars moving in its neighbourhood in perfectly circular orbits around the galactic centre.
Now, the question is how to define the motion model and the observation likelihood model for the particles.
Based on the principle of making the system as universal as possible, we define the motion model purely based on the historical motion information.
As a result, a 2-D parameter space, in which motion states were visualized and identified, was established by two components of velocity to define the motion states (see Figs. 2K and 3D).
It explains the motion of the charge carrying particles based on the threshold values, also adding the possibility to define the motion of the particles based on the polarity of the input voltage.
Next, if we ignore the higher order terms, divide by Δt, and then take the limit as Δt → 0, we get the Optical flow constraint equation (OFCE): ∂ I ∂ x ⋅ ∂ x ∂ t + ∂ I ∂ y ⋅ ∂ y ∂ t + ∂ I ∂ t = 0. To formulate the motion problem, define the motion velocities u and v using: u x, y, t) = ∂x/∂t and v x, y, t) = ∂y/∂t.
Similar(52)
where p defines the motion search range.
Furthermore, based on the motion degree function we defined, the motion search range of motion estimation can be adaptively adjusted.
And then, based on the motion degree function we defined, the motion search range of ME can be adaptively adjusted.
Therefore, these two probabilities can be written using the probabilities defining the motion language module and the natural language module.
This section first gives a brief introduction of the PF algorithm, and then defines the motion model and observation model in detail.
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Justyna Jupowicz-Kozak
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