Isotropic Gaussian Random Fields on the Sphere: Regularity, Fast Simulation and Stochastic Partial Differential Equations IV: Heat-Equation Spectral Truncation Error ≤ κ^{−β} a.s. for β < α/2Research Paper
Motivation
Stochastic partial differential equations on the sphere model quantities that live on the surface of the Earth or of the sky and are perturbed by spatially correlated noise: temperature anomalies, geophysical fields, fluctuations of the cosmic microwave background. The simplest such model is the stochastic heat equation on the unit sphere with additive isotropic noise. Because the noise is isotropic and the Laplace–Beltrami operator is diagonal in the spherical harmonics, the equation decouples into one scalar Ornstein–Uhlenbeck equation per harmonic, and the solution can be simulated exactly in law by truncating its spherical-harmonic expansion at a degree . The practical question is how fast this spectral truncation converges, in mean square and along a single simulated path.
A. Lang and Ch. Schwab answer this in §7 of Isotropic Gaussian random fields on the sphere: regularity, fast simulation and stochastic partial differential equations (arXiv:1305.1170v3, Ann. Appl. Probab. 25(6), 2015). Their rates are expressed through the decay of the angular power spectrum of the noise, the same quantity that governs the sample regularity and the Karhunen–Loève truncation of isotropic Gaussian random fields in the earlier sections of the paper.
Setting
Let be the unit sphere with surface measure (total mass ) and the real square-integrable functions with norm . The spherical harmonics , , , are built from the Legendre polynomials ; the functions , , () form a real orthonormal basis of the degree- harmonics, on which the Laplace–Beltrami operator acts as multiplication by , .
On a probability space let (, , ) be independent real Brownian motions, and let , , be an angular power spectrum. The isotropic -Wiener process is
The stochastic heat equation is
Its solution is with
and the spectral approximation is . The norm measures random fields. The standing assumption of §7 is the decay condition
Formalization targets
Goal: Corollary 7.3 (p. 43)
For every and every , almost surely
The goal fixes no constant; only the exponent enters, so it survives any improvement of the constants below.
Milestones
- Display (3), p. 36. For , .
- Lemma 7.1, pp. 39–40, as proved. If the coefficients of are independent of the noise, then for and
- Lemma 7.2, pp. 41–43, as proved. For each there is with, for and ,
Significance
Corollary 7.3 is the pathwise convergence rate of the spectral method for the stochastic heat equation on the sphere: a single simulated path of the truncated series is within of the true path in for all large , for any . Combined with the exact-in-law recursion on a time grid (pp. 36–38), it says that the only source of error in simulating this SPDE is the spectral truncation, and that the rate is governed by the decay exponent of the noise spectrum alone, with sufficing (no trace-class condition is needed, thanks to the smoothing of the heat semigroup). The mean-square and estimates of Lemmas 7.1 and 7.2 are the quantitative inputs; the bound for all is what makes a Borel–Cantelli argument possible.
The results are proved in the paper; none of them, nor the stochastic heat equation on the sphere, nor spherical harmonics, has a machine-checked formalization on the platform or in Mathlib. The work here is to formalize the known proof. Two printed statements need correction (see Formalization scope); the milestones state the bounds that the paper's proofs establish.
Difficulty
The obvious argument writes as the tail of the series, splits it into the damped initial condition and the noise, and bounds each. The noise part is a Gaussian random field whose angular power spectrum decays like , so its truncation error is controlled by the corresponding estimates for isotropic Gaussian random fields (Proposition 5.2 and Theorem 5.3 of the paper), which must be re-derived here. Several steps have no current library support: the Wiener integral of a deterministic integrand and its Gaussian law, orthonormality and completeness of the spherical harmonics in , moment equivalence for Gaussian vectors in a Hilbert space (to pass from to all ), and the passage between the pointwise series and its limit. The initial-condition tail decays like but not uniformly as , which is exactly why the printed "uniformly in time" bounds fail and why every statement takes fixed.
Formalization scope
- is
Metric.sphere (0 : EuclideanSpace ℝ (Fin 3)) 1with coordinates indexed (the paper's ); is the measuretoSphereof Lebesgue measure, of mass . Spherical harmonics are written in Cartesian form, , which is the paper's function also at the poles. For real the projection is written in the real orthonormal basis. - Brownian motions are Mathlib's
IsBrownianRealprocesses on , independent as a family of path-valued random variables. The stochastic convolution is defined pathwise as , which equals the Wiener integral almost surely (integration by parts; a.s.). This is the one place where a stochastic integral is replaced by a pathwise expression. - The Laplace–Beltrami operator is not defined: the paper's spectral solution formula of p. 36 is taken as the definition of , as a pointwise limit of partial sums in ; where they diverge (a -null set for ) the value is irrelevant to every norm. All statements take ; the paper's time partition with forces this, and since is defined from the solution itself the independence of the time discretization is automatic and the partition is not an argument.
- Norms are lower Lebesgue integrals in , so no integrability side condition hides in a default value; is jointly measurable with ; ; .
- Corrections. Lemmas 7.1 and 7.2 claim bounds uniform in time with constants depending only on , , (and ). Their proofs bound the initial-condition tail by (resp. ) and absorb it into with a -dependent constant; for nonzero the printed uniform bounds are false (as the error tends to the tail of ). The milestones state the proofs' bounds with the explicit exponential term; for Lemma 7.1 is the printed statement, uniformly in . Lemma 7.1 additionally assumes that the coefficients of are independent of the noise, which its proof uses to drop a cross term. In Lemma 7.2 the constant depends on only and is quantified before everything else. Corollary 7.3 is stated for each fixed : "uniformly in time" is not formalized. The constant on p. 42, , should read ; it is existential in Lemma 7.2 and has no effect.
- A trivializing reading is ruled out: the error is measured against the solution defined by the explicit series, not against an arbitrary process satisfying a hypothesis, and no hypothesis pins the conclusion.
- Reusable infrastructure: real spherical harmonics and their orthonormality on , the Wiener integral of deterministic functions and the Ornstein–Uhlenbeck law, and moment equivalence for Gaussian fields. Contributions of any of these, or of the truncation estimates of §5 for the shifted spectrum, are welcome.
Selected references
- A. Lang, Ch. Schwab, Isotropic Gaussian random fields on the sphere: regularity, fast simulation and stochastic partial differential equations, Ann. Appl. Probab. 25(6), 2015. arXiv:1305.1170
- A. Jentzen, P. E. Kloeden, Overcoming the order barrier in the numerical approximation of stochastic partial differential equations with additive space–time noise, Proc. R. Soc. A 465, 2009. doi:10.1098/rspa.2008.0325
- G. Da Prato, J. Zabczyk, Stochastic Equations in Infinite Dimensions, Cambridge University Press, 1992. doi:10.1017/CBO9780511666223
- D. Marinucci, G. Peccati, Random Fields on the Sphere, Cambridge University Press, 2011. doi:10.1017/CBO9780511751677