Axion emission rates in stars and constraints on its mass

Anthony Pantziris; Kyungsik Kang

doi:10.1103/PhysRevD.33.3509

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Axion emission rates in stars and constraints on its mass

Anthony Pantziris and Kyungsik Kang

Department of Physics, Brown University, Providence, Rhode Island 02912

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Phys. Rev. D 33, 3509 – Published 15 June, 1986

DOI: https://doi.org/10.1103/PhysRevD.33.3509

Abstract

We have calculated in detail the emission rates of the invisible axion of Dine, Fischler, and Srednicki in several representative types of stars and derived upper bounds for its mass. We give, in particular, complete reaction amplitudes and energy rates for axion emission. Our results for the axion mass limits are in qualitative agreement with previous estimates for most of the cases except for the neutron stars which give a stronger bound on the axion mass.

Comments & Replies

Comment on axion emission rates in stars

Georg G. Raffelt

Phys. Rev. D 34, 3927 (1986)

References (23)

R. D. Peccei and H. R. Quinn, Phys. Rev. Lett. 38, 1440 (1977); F. Wilczek, ibid. 40, 279 (1978); S. Weinberg, ibid. 40, 223 (1978); G. 't Hooft, ibid. 37, 8 (1976).
M. Dine, W. Fischler, and M. Srednicki, Phys. Lett. 104, 199 (1981).
M. Fukugita, S. Watamura and M. Yoshimura, Phys. Rev. D 26, 1840 (1982); Phys. Rev. Lett. 48, 1522 (1982).
N. Iwamoto, Phys. Rev. Lett. 53, 1198 (1984).
W. A. Bardeen and S. H. Tye, Phys. Lett. 74, 229 (1978).
V. N. Tsytovich, Zh. Eksp. Teor. Fiz. 13, 1775 (1961) [Sov. Phys. JETP 13, 1249 (1961)]; J. B. Adams, M. A. Ruderman and C.-H. Woo, Phys. Rev. 129, 1383 (1963); see also K. Mikaelian, Phys. Rev. D 18, 3605 (1978).
G. Beaudet, V. Petrosian and E. E. Salpeter, Astrophys. J. 150, 979 (1967).
B. L. Friman and O. V. Maxwell, Astrophys. J. 232, 541 (1979).
Iwamoto of Ref. 4, calculated the spin-summed matrix element, however, based on the nonrelativistic one-pion-exchange potential. In our relativistic treatment the pseudoscalar-axion-nucleon coupling interferes with the pion-nucleon coupling and the matrix element depends on $M_{N}$ ${}^{2}$ | P ${vec}_{1}$ - P ${vec}_{3}$ $|^{2}$ , etc., differently compared to Iwamoto's result; G. Da Prato, Nuovo Cimento 22, 123 (1961).
R. B. Stothers, Phys. Rev. Lett. 24, 538 (1970).
K. Nomoto and S. Tsuruta, Astrophys. J. Lett. 250, L19 (1981).
D. Clayton, Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York, 1968).
J. N. Bahcall and G. Shaviv, Astrophys. J. 153, 11 (1968); ibid. 153, 3 (1968).
See, for example, K. Sato and H. Sato, Prog. Theor. Phys. 54, 1564 (1975); D. A. Dicus, E. W. Kolb, V. L. Teplitz and R. V. Wagoner, Phys. Rev. D 18, 1829 (1978).
D. A. Dicus, Phys. Rev. D 6, 941 (1972); also Ref. 7.
S. C. Vila, Astrophys. J. 146, 437 (1966); ibid. 149, 613 (1967); M. P. Savedoff, H. M. Van Horn and S. C. Vila, ibid. 155, 221 (1969).
H. A. Bethe and M. B. Johnson, Nucl. Phys. 230, 1 (1974).
V. R. Pandharipande and R. A. Smith, Nucl. Phys. 237, 507 (1975); V. R. Pandharipande et al., Astrophys. J. 208, 550 (1976).
N. C. Chao, J. W. Clark, and C. H. Yang, Nucl. Phys. 179, 320 (1972).
G. G. Festa and M. A. Ruderman, Phys. Rev. 180, 1227 (1969); D. A. Dicus, E. W. Kolb, D. N. Schramm and D. L. Tubbs, Astrophys. J. 210, 481 (1976).
M. Soyeur and G. E. Brown, Nucl. Phys. 324, 464 (1979).
T. Takatsuka, Prog. Theor. Phys. 48, 1517 (1972).
D. J. Helfand and R. H. Becker, Nature (London) 307, 215 (1984).

[c1] R. D. Peccei and H. R. Quinn, Phys. Rev. Lett. 38, 1440 (1977); F. Wilczek, ibid. 40, 279 (1978); S. Weinberg, ibid. 40, 223 (1978); G. 't Hooft, ibid. 37, 8 (1976).

[c2] M. Dine, W. Fischler, and M. Srednicki, Phys. Lett. 104, 199 (1981).

[c3] M. Fukugita, S. Watamura and M. Yoshimura, Phys. Rev. D 26, 1840 (1982); Phys. Rev. Lett. 48, 1522 (1982).

[c4] N. Iwamoto, Phys. Rev. Lett. 53, 1198 (1984).

[c5] W. A. Bardeen and S. H. Tye, Phys. Lett. 74, 229 (1978).

[c6] V. N. Tsytovich, Zh. Eksp. Teor. Fiz. 13, 1775 (1961) [Sov. Phys. JETP 13, 1249 (1961)]; J. B. Adams, M. A. Ruderman and C.-H. Woo, Phys. Rev. 129, 1383 (1963); see also K. Mikaelian, Phys. Rev. D 18, 3605 (1978).

[c7] G. Beaudet, V. Petrosian and E. E. Salpeter, Astrophys. J. 150, 979 (1967).

[c8] B. L. Friman and O. V. Maxwell, Astrophys. J. 232, 541 (1979).

[c9] Iwamoto of Ref. 4, calculated the spin-summed matrix element, however, based on the nonrelativistic one-pion-exchange potential. In our relativistic treatment the pseudoscalar-axion-nucleon coupling interferes with the pion-nucleon coupling and the matrix element depends on $M_{N}$ ${}^{2}$ | P ${vec}_{1}$ - P ${vec}_{3}$ $|^{2}$ , etc., differently compared to Iwamoto's result; G. Da Prato, Nuovo Cimento 22, 123 (1961).

[c10] R. B. Stothers, Phys. Rev. Lett. 24, 538 (1970).

[c11] K. Nomoto and S. Tsuruta, Astrophys. J. Lett. 250, L19 (1981).

[c12] D. Clayton, Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York, 1968).

[c13] J. N. Bahcall and G. Shaviv, Astrophys. J. 153, 11 (1968); ibid. 153, 3 (1968).

[c14] See, for example, K. Sato and H. Sato, Prog. Theor. Phys. 54, 1564 (1975); D. A. Dicus, E. W. Kolb, V. L. Teplitz and R. V. Wagoner, Phys. Rev. D 18, 1829 (1978).

[c15] D. A. Dicus, Phys. Rev. D 6, 941 (1972); also Ref. 7.

[c16] S. C. Vila, Astrophys. J. 146, 437 (1966); ibid. 149, 613 (1967); M. P. Savedoff, H. M. Van Horn and S. C. Vila, ibid. 155, 221 (1969).

[c17] H. A. Bethe and M. B. Johnson, Nucl. Phys. 230, 1 (1974).

[c18] V. R. Pandharipande and R. A. Smith, Nucl. Phys. 237, 507 (1975); V. R. Pandharipande et al., Astrophys. J. 208, 550 (1976).

[c19] N. C. Chao, J. W. Clark, and C. H. Yang, Nucl. Phys. 179, 320 (1972).

[c20] G. G. Festa and M. A. Ruderman, Phys. Rev. 180, 1227 (1969); D. A. Dicus, E. W. Kolb, D. N. Schramm and D. L. Tubbs, Astrophys. J. 210, 481 (1976).

[c21] M. Soyeur and G. E. Brown, Nucl. Phys. 324, 464 (1979).

[c22] T. Takatsuka, Prog. Theor. Phys. 48, 1517 (1972).

[c23] D. J. Helfand and R. H. Becker, Nature (London) 307, 215 (1984).

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Axion emission rates in stars and constraints on its mass

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Comment on axion emission rates in stars

References (23)

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