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Multiplicity and parity in Hirota's NN-soliton conditions: the bilinear families L (Dx3+Λ)2n+1L\,(D_x^{3}+Λ)^{2n+1}

Abstract

Hirota's three-soliton condition is the standard test for the integrability of a bilinear equation P(D)f⋅f=0P(D)f\cdot f=0, and the folklore implication ``three-soliton condition ⇒\Rightarrow NN-soliton solutions for all NN'' underlies the classifications of Hietarinta. We study this implication in two directions. The first is the family L (Dx3+Λ)2n+1f⋅f=0L\,(D_x^3+Λ)^{2n+1}f\cdot f=0 with LL, ΛΛ linear forms in the Hirota operators, which for n=0n=0 contains the Korteweg–de Vries, Ito and Boiti–Leon–Manna–Pempinelli equations and for L=DxL=D_x is the family of Gürses and Pekcan. On the principal component of the dispersion variety the NN-soliton condition reduces to a sign sum of two bialternants; counting odd exponents shows that for n=0n=0 the class is Hirota integrable and that for n≥1n\ge1 the three-soliton condition holds for every LL, and an explicit formula for the four-soliton residual proves the Gürses–Pekcan conjecture that the four-soliton condition fails for every n≥1n\ge1. The formula yields sum-of-squares certificates excluding four-soliton solutions at every real configuration for the Gürses–Pekcan and Ito equations, classifies the real members of the class, and determines maximal numbers of nondegenerate solitons: exactly four or five for n=1n=1 according as LL lies in the span of Dx,ΛD_x,Λ or not, five for n=2n=2 and L=DxL=D_x, and finite for every n≥1n\ge1 and every LL. The second direction is a reformulation of the implication for a single non-hyperplane component of multiplicity one, which we prove, with complete classifications, for all graph-type dispersions L(q(D)+Dt)L(q(D)+D_t), for every irreducible even quadric component in any dimension and with an arbitrary cofactor, for parabolic components, for the dispersions F(ℓ)+QF(\ell)+Q containing the Kadomtsev–Petviashvili surface, and, with a prescribed one-parameter phase family, for the cubic graph.

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  • Physics and Astronomy

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