TY - JOUR

T1 - Comment on “Constraints on the strength of primordial magnetic fields from big bang nucleosynthesis reexamined

AU - Kernan, Peter J.

AU - Starkman, Glenn D.

AU - Vachaspati, Tanmay

N1 - Copyright:
Copyright 2017 Elsevier B.V., All rights reserved.

PY - 1997

Y1 - 1997

N2 - Recently Cheng, Olinto, Schramm, and Truran reexamined the constraints on the strength of primordial [Formula presented] fields from big bang nucleosynthesis (BBN). Their bottom line agreed with that of an earlier recent paper on the subject by Kernan, Starkman, and Vachaspati, both in its final limit on the [Formula presented] field during BBN and in its conclusion that, for allowed values of the [Formula presented] field, the dominant factor for BBN is the increased expansion rate at a given temperature caused by the energy density of the magnetic field, [Formula presented]. However, their conclusion that weak interaction rates increased with an increasing [Formula presented] field at these low field values contradicted the earlier results of Kernan, Starkman, and Vachaspati. In this Comment we point out that the Taylor series expansion of the weak interaction rate about [Formula presented] used by Cheng et al. is not well defined, while the Euler-McLaurin expansion of Kernan, Starkman, and Vachaspati is well behaved and reliable. Using the Euler-McLaurin expansion we find that the weak interaction rates decrease rather than increase with an increasing [Formula presented] field at small values of the [Formula presented] field.

AB - Recently Cheng, Olinto, Schramm, and Truran reexamined the constraints on the strength of primordial [Formula presented] fields from big bang nucleosynthesis (BBN). Their bottom line agreed with that of an earlier recent paper on the subject by Kernan, Starkman, and Vachaspati, both in its final limit on the [Formula presented] field during BBN and in its conclusion that, for allowed values of the [Formula presented] field, the dominant factor for BBN is the increased expansion rate at a given temperature caused by the energy density of the magnetic field, [Formula presented]. However, their conclusion that weak interaction rates increased with an increasing [Formula presented] field at these low field values contradicted the earlier results of Kernan, Starkman, and Vachaspati. In this Comment we point out that the Taylor series expansion of the weak interaction rate about [Formula presented] used by Cheng et al. is not well defined, while the Euler-McLaurin expansion of Kernan, Starkman, and Vachaspati is well behaved and reliable. Using the Euler-McLaurin expansion we find that the weak interaction rates decrease rather than increase with an increasing [Formula presented] field at small values of the [Formula presented] field.

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U2 - 10.1103/PhysRevD.56.3766

DO - 10.1103/PhysRevD.56.3766

M3 - Article

AN - SCOPUS:18044372920

VL - 56

SP - 3766

EP - 3767

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 6

ER -