Split the time-evolution operator into factors with , and insert position completeness relations between them. Each factor is evaluated by inserting momentum states normalized by :Multiplying the kernels and integrating the intermediate positions produces the stated time-sliced path integral, including its normalization power. For a free particle this Gaussian short-time kernel is exact, so the convolution identity already holds at finite . Oscillatory integrals are defined with a vanishing convergence regulator, consistently fixing the square-root phase.
The exponent is , whereis the classical action of the piecewise-linear interpolating path. For smooth paths its limit is . The discretization defines the quantum integral; it does not assert that typical quantum paths are differentiable. Weighting histories by their action phase is the central formulation of the original path-integral paper.[ref]
Space-Time Approach to Non-Relativistic Quantum Mechanics by Richard Feynman. 1948, abstract: amplitudes from histories weighted by the exponential of classical action in units of reduced Planck's constant
When action differences on the experimental scales are large compared with , nearby nonstationary phases cancel. stationary phase selects at fixed endpoints, hence . The surviving free classical trajectory is , with action . This is the semiclassical mechanism; it does not mean each individual path becomes a classical path.
The Fresnel convolution of free-particle time slices follows by completing the square:The second term is independent of . The shifted Fresnel integral in the first term givesHere is the positive slice index, not a wave number. The phase is fixed by the same convergence prescription as the short-time kernel.
After integrating , the remaining exponent contains . The square-root factors telescope:Since , the free-particle propagator isFor , the square root has phase . Its short-time limit is the position delta function in the distributional sense, consistent with unitary evolution.
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