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11: 24.19 Methods of Computation
Equations (24.5.3) and (24.5.4) enable B n and E n to be computed by recurrence. …For example, the tangent numbers T n can be generated by simple recurrence relations obtained from (24.15.3), then (24.15.4) is applied. … For number-theoretic applications it is important to compute B 2 n ( mod p ) for 2 n p 3 ; in particular to find the irregular pairs ( 2 n , p ) for which B 2 n 0 ( mod p ) . …
  • Buhler et al. (1992) uses the expansion

    24.19.3 t 2 cosh t 1 = 2 n = 0 ( 2 n 1 ) B 2 n t 2 n ( 2 n ) ! ,

    and computes inverses modulo p of the left-hand side. Multisectioning techniques are applied in implementations. See also Crandall (1996, pp. 116–120).

  • A method related to “Stickelberger codes” is applied in Buhler et al. (2001); in particular, it allows for an efficient search for the irregular pairs ( 2 n , p ) . Discrete Fourier transforms are used in the computations. See also Crandall (1996, pp. 120–124).

  • 12: 15.9 Relations to Other Functions
    §15.9 Relations to Other Functions
    §15.9(i) Orthogonal Polynomials
    Jacobi
    Legendre
    Meixner
    13: 13.6 Relations to Other Functions
    §13.6 Relations to Other Functions
    §13.6(iv) Parabolic Cylinder Functions
    §13.6(v) Orthogonal Polynomials
    Laguerre Polynomials
    §13.6(vi) Generalized Hypergeometric Functions
    14: 10.9 Integral Representations
    Poisson’s and Related Integrals
    Schläfli’s and Related Integrals
    Mehler–Sonine and Related Integrals
    See Paris and Kaminski (2001, p. 116) for related results. …
    15: 6.5 Further Interrelations
    §6.5 Further Interrelations
    6.5.1 E 1 ( x ± i 0 ) = Ei ( x ) i π ,
    6.5.3 1 2 ( Ei ( x ) + E 1 ( x ) ) = Shi ( x ) = i Si ( i x ) ,
    6.5.4 1 2 ( Ei ( x ) E 1 ( x ) ) = Chi ( x ) = Ci ( i x ) 1 2 π i .
    6.5.5 Si ( z ) = 1 2 i ( E 1 ( i z ) E 1 ( i z ) ) + 1 2 π ,
    16: 19.6 Special Cases
    17: 19.21 Connection Formulas
    Legendre’s relation (19.7.1) can be written … Let y , z , and p be positive and distinct, and permute y and z to ensure that y does not lie between z and p . …If 0 < p < z and y = z + 1 , then as p 0 (19.21.6) reduces to Legendre’s relation (19.21.1). … Change-of-parameter relations can be used to shift the parameter p of R J from either circular region to the other, or from either hyperbolic region to the other (§19.20(iii)). … In (19.21.12), if x is the largest (smallest) of x , y , and z , then p and q lie in the same region if it is circular (hyperbolic); otherwise p and q lie in different regions, both circular or both hyperbolic. …
    18: 13.8 Asymptotic Approximations for Large Parameters
    For the parabolic cylinder function U see §12.2, and for an extension to an asymptotic expansion see Temme (1978). … where w = arccosh ( 1 + ( 2 a ) 1 x ) , and β = ( w + sinh w ) / 2 . … For an extension to an asymptotic expansion complete with error bounds see Temme (1990b), and for related results see §13.21(i). … uniformly with respect to bounded positive values of x in each case. … For generalizations in which z is also allowed to be large see Temme and Veling (2022).
    19: 28.20 Definitions and Basic Properties
    §28.20(ii) Solutions Ce ν , Se ν , Me ν , Fe n , Ge n
    §28.20(iv) Radial Mathieu Functions Mc n ( j ) , Ms n ( j )
    §28.20(vi) Wronskians
    §28.20(vii) Shift of Variable
    And for the corresponding identities for the radial functions use (28.20.15) and (28.20.16).
    20: 36.7 Zeros
    Close to the y -axis the approximate location of these zeros is given by … Outside the bifurcation set (36.4.10), each rib is flanked by a series of zero lines in the form of curly “antelope horns” related to the “outside” zeros (36.7.2) of the cusp canonical integral. There are also three sets of zero lines in the plane z = 0 related by 2 π / 3 rotation; these are zeros of (36.2.20), whose asymptotic form in polar coordinates ( x = r cos θ , y = r sin θ ) is given by …
    §36.7(iv) Swallowtail and Hyperbolic Umbilic Canonical Integrals
    The zeros of these functions are curves in 𝐱 = ( x , y , z ) space; see Nye (2007) for Φ 3 and Nye (2006) for Φ ( H ) .