Thermal background corrections to the neutrino electromagnetic vertex in models with charged scalar bosons

A. Riotto

doi:10.1103/PhysRevD.50.2139

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Thermal background corrections to the neutrino electromagnetic vertex in models with charged scalar bosons

A. Riotto

International School for Advanced Studies, SISSA-ISAS, Strada Costiera 11, 34014 Miramare, Trieste, Italy
Istituto Nazionale di Fisica Nucleare, Sezione di Padova, 35100 Padova, Italy

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Phys. Rev. D 50, 2139 – Published 1 August, 1994

DOI: https://doi.org/10.1103/PhysRevD.50.2139

Abstract

We calculate the correction to the neutrino electromagnetic vertex due to the background of electrons in a large class of models, as the supersymmetric model with explicit breaking of R parity, where charged scalar bosons couple to leptons and which are able to provide an astrophysically interesting value for the neutrino magnetic (electric) moment: $μ_{ν}$ ∼ $10^{- 12}$ $μ_{B}$ . We show that the medium contribution to the chirality-flipping magnetic (electric) dipole moment is not significant; however, a new chirality-flipping, but helicity-conserving, term arises which does not appear in the standard model with the exchange of W gauge bosons. It signals the presence of CP and CPT asymmetries in the medium and can contribute to the emission or absorption of longitudinal photons. We estimate the contribution of this new term to the rate of the plasmon decay process $γ_{pl}$ →νν in the core of degenerate stars, showing that it can be comparable to the contribution coming from the vacuum magnetic (dipole) moment. We also calculate the correction to the effective potential of a propagating neutrino in the presence of a magnetic field due to a chirality-preserving contribution to the diagonal magnetic moment from the medium. This contribution is identical for particles and antiparticles and so it need not vanish for Majorana neutrinos.

References (14)

See, for instance, G. G. Raffelt, Phys. Rep. 198, 1 (1990), and references therein.
E. Braaten, Phys. Rev. Lett. 66, 1655 (1991); E. Braaten and D. Segel, Phys. Rev. D 48, 1478 (1993); R. F. Sawyer, ibid. 46, 1180 (1992); N. Itoh, H. Mutoh, A. Hikita and Y. Kohyama, Astrophys. J. 395, 622 (1992); M. Haft, G. G. Raffelt, and A. Weiss, ibid. (to be published); T. Altherr, E. Petitgirard and T. del Riogaztelurrutia, Astr. Part. Phys. 1, 289 (1993); T. Altherr, CERN report 1993 (unpublished).
For references and a recent review, see P.B. Pal, Int. J. Mod. Phys. A 7, 5387 (1992).
M. B. Voloshin, M. I. Vysotsky and L. B. Okun, Yad. Fiz. 44, 677 (1986) [Sov. J. Nucl. Phys. 44, 440 (1986)]; Zh. Eksp. Teor. Fiz. 91, 754 (1986) [Sov. Phys. JETP 64, 446 (1986)]; M. B. Voloshin and M. I. Vysotsky, Yad. Fiz. 44, 845 (1986) [Sov. J. Nucl. Phys. 44, 544 (1986)]; L. B. Okun, ibid. 44, 897 (1986) [44, 546 (1986)]; R. Barbieri and G. Fiorentini, Nucl. Phys. B304, 909 (1989).
C. S. Lim and W. J. Marciano, Phys. Rev. D 37, 1368 (1988); E. W. Akhmedov, Phys. Lett. B 213, 64 (1988).
J. Morgan, Phys. Lett. 102B, 247 (1981).
G. Ecker, J. Gasser, A. Pich and E. de Rafael, Nucl. Phys. B321, 311 (1989).
See, for instance, A. Zee, Phys. Lett. 93B, 389 (1980); M. Fukugita and T. B. Yanagida, Phys. Rev. Lett. 58, 1807 (1987); K. S. Babu and V. S. Mathur, ibid. 196, 218 (1987); M. B. Voloshin, Yad. Fiz. 48, 804 (1988) [Sov. J. Nucl. Phys. 48, 512 (1988)]; R. Barbieri and R. N. Mohapatra, Phys. Lett. B 218, 225 (1988); G. Ecker, W. Grimus and H. Neufeld, ibid. 232, 217 (1989); D. Chang, W. Keung and G. Senjanović, Phys. Rev. D 42, 1599 (1990).
R. Barbieri, M. M. Guzzo, A. Masiero and D. Tommasini, Phys. Lett. B 252, 251 (1990); K. S. Babu and R. N. Mohapatra, Phys. Rev. Lett. 64, 1705 (1990).
C. S. Aulakh and R. N. Mohapatra, Phys. Lett. 119B, 136 (1983); L. J. Hall and M. Suzuki, Nucl. Phys. B231, 419 (1984); I. H. Lee, ibid. B246, 120 (1984); J. Ellis et al., Phys. Lett. 150B, 142 (1985); G. G. Ross and J. W. Valle, ibid. 151B, 375 (1985); S. Dawson, Nucl. Phys. B261, 297 (1985); R. N. Mohapatra, Phys. Rev. D 11, 3457 (1986); E. Ma and P. Roy, ibid. 41, 988 (1990); E. Ma and D. Ng, ibid. 41, 1005 (1990); S. Dimopoulos, R. Esmailzadeh, L. J. Hall, J. P. Merlo and G. S. Starkmen, ibid. 41, 2099 (1990); H. Dreiner and R. J. N. Phillips, Nucl. Phys. B367, 591 (1991); L. E. Ibà nez and G. G. Ross, ibid. B368, 3 (1992); K. Enqvist, A. Masiero and A. Riotto, ibid. B373, 95 (1992).
We want to stress that, in the case of light Dirac neutrinos, the strength of the coupling of these new charged scalar bosons to the leptons is constrained by the requirement that the right handed components decouple before the quark hadron phase transition so that their density can be diluted by the subsequent releasing of entropy and give no appreciable contribution to the density of the Universe during at the onset of the primordial nucleosynthesis. If $G_{F}^{R}$ is the strength of the above mentioned coupling, then $G_{F}^{R}$ must be less than sim $10^{- 3}$ : $G_{F}$ [see A. I. Rez and V. B. Semikoz, Phys. Lett. B 249, 125 (1990)]. Again, the induced limit on $μ_{ν}$ is of order of $10^{- 12}$ : $μ_{B}$ .
J. F. Nieves and P. B. Pal, Phys. Rev. D 40, 1963 (1989); J. C. D'Olivo, J. F. Nieves and P. B. Pal, ibid. 40, 3679 (1989); V. N. Oraevsky, V. B. Semikoz and Ya. A. Smorodinsky, Phys. Lett. B 227, 255 (1989); C. Giunti, C. W. Kim and W. P. Lam, Phys. Rev. D 43, 164 (1991); T. Altherr and K. Kainulainen, Phys. Lett. B 262, 79 (1991); S. S. Massod, Phys. Rev. D 48, 3250 (1993); J. F. Nieves and P. B. Pal, Report No. LTP 058 UPR, 1993 (unpublished).
For a review, see for example, H. Nilles, Phys. Rep. 110, 1 (1984) and references therein.
J. F. Nieves, Phys. Rev. D 26, 3152 (1982).

[c1] See, for instance, G. G. Raffelt, Phys. Rep. 198, 1 (1990), and references therein.

[c2] E. Braaten, Phys. Rev. Lett. 66, 1655 (1991); E. Braaten and D. Segel, Phys. Rev. D 48, 1478 (1993); R. F. Sawyer, ibid. 46, 1180 (1992); N. Itoh, H. Mutoh, A. Hikita and Y. Kohyama, Astrophys. J. 395, 622 (1992); M. Haft, G. G. Raffelt, and A. Weiss, ibid. (to be published); T. Altherr, E. Petitgirard and T. del Riogaztelurrutia, Astr. Part. Phys. 1, 289 (1993); T. Altherr, CERN report 1993 (unpublished).

[c3] For references and a recent review, see P.B. Pal, Int. J. Mod. Phys. A 7, 5387 (1992).

[c4] M. B. Voloshin, M. I. Vysotsky and L. B. Okun, Yad. Fiz. 44, 677 (1986) [Sov. J. Nucl. Phys. 44, 440 (1986)]; Zh. Eksp. Teor. Fiz. 91, 754 (1986) [Sov. Phys. JETP 64, 446 (1986)]; M. B. Voloshin and M. I. Vysotsky, Yad. Fiz. 44, 845 (1986) [Sov. J. Nucl. Phys. 44, 544 (1986)]; L. B. Okun, ibid. 44, 897 (1986) [44, 546 (1986)]; R. Barbieri and G. Fiorentini, Nucl. Phys. B304, 909 (1989).

[c5] C. S. Lim and W. J. Marciano, Phys. Rev. D 37, 1368 (1988); E. W. Akhmedov, Phys. Lett. B 213, 64 (1988).

[c6] J. Morgan, Phys. Lett. 102B, 247 (1981).

[c7] G. Ecker, J. Gasser, A. Pich and E. de Rafael, Nucl. Phys. B321, 311 (1989).

[c8] See, for instance, A. Zee, Phys. Lett. 93B, 389 (1980); M. Fukugita and T. B. Yanagida, Phys. Rev. Lett. 58, 1807 (1987); K. S. Babu and V. S. Mathur, ibid. 196, 218 (1987); M. B. Voloshin, Yad. Fiz. 48, 804 (1988) [Sov. J. Nucl. Phys. 48, 512 (1988)]; R. Barbieri and R. N. Mohapatra, Phys. Lett. B 218, 225 (1988); G. Ecker, W. Grimus and H. Neufeld, ibid. 232, 217 (1989); D. Chang, W. Keung and G. Senjanović, Phys. Rev. D 42, 1599 (1990).

[c9] R. Barbieri, M. M. Guzzo, A. Masiero and D. Tommasini, Phys. Lett. B 252, 251 (1990); K. S. Babu and R. N. Mohapatra, Phys. Rev. Lett. 64, 1705 (1990).

[c10] C. S. Aulakh and R. N. Mohapatra, Phys. Lett. 119B, 136 (1983); L. J. Hall and M. Suzuki, Nucl. Phys. B231, 419 (1984); I. H. Lee, ibid. B246, 120 (1984); J. Ellis et al., Phys. Lett. 150B, 142 (1985); G. G. Ross and J. W. Valle, ibid. 151B, 375 (1985); S. Dawson, Nucl. Phys. B261, 297 (1985); R. N. Mohapatra, Phys. Rev. D 11, 3457 (1986); E. Ma and P. Roy, ibid. 41, 988 (1990); E. Ma and D. Ng, ibid. 41, 1005 (1990); S. Dimopoulos, R. Esmailzadeh, L. J. Hall, J. P. Merlo and G. S. Starkmen, ibid. 41, 2099 (1990); H. Dreiner and R. J. N. Phillips, Nucl. Phys. B367, 591 (1991); L. E. Ibà nez and G. G. Ross, ibid. B368, 3 (1992); K. Enqvist, A. Masiero and A. Riotto, ibid. B373, 95 (1992).

[c11] We want to stress that, in the case of light Dirac neutrinos, the strength of the coupling of these new charged scalar bosons to the leptons is constrained by the requirement that the right handed components decouple before the quark hadron phase transition so that their density can be diluted by the subsequent releasing of entropy and give no appreciable contribution to the density of the Universe during at the onset of the primordial nucleosynthesis. If $G_{F}^{R}$ is the strength of the above mentioned coupling, then $G_{F}^{R}$ must be less than sim $10^{- 3}$ : $G_{F}$ [see A. I. Rez and V. B. Semikoz, Phys. Lett. B 249, 125 (1990)]. Again, the induced limit on $μ_{ν}$ is of order of $10^{- 12}$ : $μ_{B}$ .

[c12] J. F. Nieves and P. B. Pal, Phys. Rev. D 40, 1963 (1989); J. C. D'Olivo, J. F. Nieves and P. B. Pal, ibid. 40, 3679 (1989); V. N. Oraevsky, V. B. Semikoz and Ya. A. Smorodinsky, Phys. Lett. B 227, 255 (1989); C. Giunti, C. W. Kim and W. P. Lam, Phys. Rev. D 43, 164 (1991); T. Altherr and K. Kainulainen, Phys. Lett. B 262, 79 (1991); S. S. Massod, Phys. Rev. D 48, 3250 (1993); J. F. Nieves and P. B. Pal, Report No. LTP 058 UPR, 1993 (unpublished).

[c13] For a review, see for example, H. Nilles, Phys. Rep. 110, 1 (1984) and references therein.

[c14] J. F. Nieves, Phys. Rev. D 26, 3152 (1982).

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Thermal background corrections to the neutrino electromagnetic vertex in models with charged scalar bosons

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