LOGIN TO YOUR ACCOUNT

Username
Password
Remember Me
Or use your Academic/Social account:

CREATE AN ACCOUNT

Or use your Academic/Social account:

Congratulations!

You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.

Important!

Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message

CREATE AN ACCOUNT

Name:
Username:
Password:
Verify Password:
E-mail:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Law, Sandy S. C.; McDonald, Kristian L. (2013)
Languages: English
Types: Preprint
Subjects: High Energy Physics - Phenomenology

Classified by OpenAIRE into

arxiv: High Energy Physics::Phenomenology
We present a class of models with radiative neutrino mass and stable dark-matter candidates. Neutrino mass is generated by a one-loop diagram with the same topography as Ma's 2006 proposal (which used an inert scalar-doublet and singlet fermion). We generalize this approach and determine all variants with new fields no larger than the adjoint representation. When the neutrino mass diagram contains a Majorana mass insertion there are two possibilities, both of which are known. If the mass insertion is of the Dirac type there are seven additional models, two of which are excluded by direct-detection experiments. The other five models are also constrained, such that only scalar dark-matter is viable. There are cases with an inert singlet, an inert doublet, and an inert triplet, providing a natural setting for inert N-tuplet models of dark matter, with the additional feature of achieving radiative neutrino mass. We show that some of the models admit a simple explanation for the (requisite) discrete symmetry, and briefly discuss cases with representations larger than the adjoint, which can admit a connection to the astrophysical gamma-ray signal.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • [1] M. C. Gonzalez-Garcia, M. Maltoni, J. Salvado and T. Schwetz, JHEP 1212, 123 (2012) [arXiv:1209.3023 [hep-ph]].
    • [2] A. H. G. Peter, arXiv:1201.3942 [astro-ph.CO].
    • [3] E. Ma, Phys. Rev. D 73, 077301 (2006) [hep-ph/0601225].
    • [4] E. Ma and D. Suematsu, Mod. Phys. Lett. A 24, 583 (2009) [arXiv:0809.0942 [hep-ph]].
    • [5] J. Kopp, E. T. Neil, R. Primulando and J. Zupan, Phys. Dark. Univ. 2 (2013) 22 [arXiv:1301.1683 [hep-ph]].
    • [6] C. Weniger, JCAP 1208, 007 (2012) [arXiv:1204.2797 [hep-ph]].
    • [7] L. M. Krauss, S. Nasri and M. Trodden, Phys. Rev. D 67, 085002 (2003) [hepph/0210389].
    • [8] C. Boehm, Y. Farzan, T. Hambye, S. Palomares-Ruiz and S. Pascoli, Phys. Rev. D 77, 043516 (2008) [hep-ph/0612228]; M. Lindner, D. Schmidt and T. Schwetz, Phys. Lett. B 705, 324 (2011) [arXiv:1105.4626 [hep-ph]]; F. -X. Josse-Michaux and E. Molinaro, Phys. Rev. D 84, 125021 (2011) [arXiv:1108.0482 [hep-ph]]; S. Kanemura, T. Nabeshima and H. Sugiyama, Phys. Rev. D 85, 033004 (2012) [arXiv:1111.0599 [hepph]]; M. Gustafsson, J. M. No and M. A. Rivera, arXiv:1212.4806 [hep-ph]; M. Aoki, J. Kubo and H. Takano, arXiv:1302.3936 [hep-ph]; Y. Kajiyama, H. Okada and T. Toma, arXiv:1303.7356 [hep-ph].
    • [9] V. Silveira and A. Zee, Phys. Lett. B 161, 136 (1985); J. McDonald, Phys. Rev. D 50 (1994) 3637 [hep-ph/0702143 [HEP-PH]]; C. P. Burgess, M. Pospelov and T. ter Veldhuis, Nucl. Phys. B 619 (2001) 709 [hep-ph/0011335].
    • [10] R. Barbieri, L. J. Hall and V. S. Rychkov, Phys. Rev. D 74 (2006) 015007 [hepph/0603188]; L. Lopez Honorez, E. Nezri, J. F. Oliver and M. H. G. Tytgat, JCAP 0702 (2007) 028 [hep-ph/0612275]. Q. -H. Cao, E. Ma and G. Rajasekaran, Phys. Rev. D 76 (2007) 095011 [arXiv:0708.2939 [hep-ph]]; S. Andreas, M. H. G. Tytgat and Q. Swillens, JCAP 0904 (2009) 004 [arXiv:0901.1750 [hep-ph]]; L. Lopez Honorez and C. E. Yaguna, JCAP 1101 (2011) 002 [arXiv:1011.1411 [hep-ph]]; M. Gustafsson, S. Rydbeck, L. Lopez-Honorez and E. Lundstrom, Phys. Rev. D 86 (2012) 075019 [arXiv:1206.6316 [hep-ph]]; S. Kashiwase and D. Suematsu, Phys. Rev. D 86 (2012) 053001 [arXiv:1207.2594 [hep-ph]].
    • [11] M. Cirelli, N. Fornengo and A. Strumia, Nucl. Phys. B 753, 178 (2006) [hepph/0512090]; M. Cirelli, A. Strumia and M. Tamburini, Nucl. Phys. B 787, 152 (2007) [arXiv:0706.4071 [hep-ph]].
    • [12] E. Ma, Phys. Rev. Lett. 81 (1998) 1171 [hep-ph/9805219].
    • [13] F. Bonnet, M. Hirsch, T. Ota and W. Winter, JHEP 1207, 153 (2012) [arXiv:1204.5862 [hep-ph]].
    • [14] M. Fabbrichesi and S. Petcov, arXiv:1304.4001 [hep-ph].
    • [15] K. L. McDonald, arXiv:1303.4573 [hep-ph].
    • [16] K. Hally, H. E. Logan and T. Pilkington, Phys. Rev. D 85, 095017 (2012) [arXiv:1202.5073 [hep-ph]].
    • [17] R. Foot, H. Lew, X. G. He and G. C. Joshi, Z. Phys. C 44, 441 (1989).
    • [18] S. -Y. Ho and J. Tandean, arXiv:1303.5700 [hep-ph].
    • [19] C. -K. Chua and S. S. C. Law, Phys. Rev. D 83, 055010 (2011) [arXiv:1011.4730 [hepph]]; A. Delgado, C. Garcia Cely, T. Han and Z. Wang, Phys. Rev. D 84, 073007 (2011) [arXiv:1105.5417 [hep-ph]]; S. S. C. Law and K. L. McDonald, Phys. Lett. B 713, 490 (2012) [arXiv:1204.2529 [hep-ph]]; I. Baldes, N. F. Bell, K. Petraki and R. R. Volkas, arXiv:1304.6162 [hep-ph]; G. Bambhaniya, J. Chakrabortty, S. Goswami and P. Konar, arXiv:1305.2795 [hep-ph].
    • [20] E. Del Nobile, R. Franceschini, D. Pappadopulo and A. Strumia, Nucl. Phys. B 826, 217 (2010) [arXiv:0908.1567 [hep-ph]].
    • [21] A. Joglekar, P. Schwaller and C. E. M. Wagner, JHEP 1212 (2012) 064 [arXiv:1207.4235 [hep-ph]].
    • [22] C. Arina, R. N. Mohapatra and N. Sahu, Phys. Lett. B 720 (2013) 130 [arXiv:1211.0435 [hep-ph]].
    • [23] S. S. C. Law, JHEP 1202 (2012) 127 [arXiv:1106.0375 [hep-ph]].
    • [24] M. Aoki, S. Kanemura and K. Yagyu, Phys. Lett. B 702, 355 (2011) [Erratum-ibid. B 706, 495 (2012)] [arXiv:1105.2075 [hep-ph]].
    • [25] W. Konetschny and W. Kummer, Phys. Lett. B 70, 433 (1977); T. P. Cheng and L. F. Li, Phys. Rev. D 22, 2860 (1980); M. Magg and C. Wetterich, Phys. Lett. B 94, 61 (1980); J. Schechter and J. W. F. Valle, Phys. Rev. D 22, 2227 (1980); G. Lazarides, Q. Shafi and C. Wetterich, Nucl. Phys. B 181, 287 (1981); C. Wetterich, Nucl. Phys. B 187, 343 (1981); R. N. Mohapatra and G. Senjanovic, Phys. Rev. D 23, 165 (1981).
    • [26] S. S. C. Law and K. L. McDonald, arXiv:1303.6384 [hep-ph].
    • [27] X. -G. He, Eur. Phys. J. C 34, 371 (2004) [hep-ph/0307172].
    • [28] K. S. Babu, S. Nandi and Z. Tavartkiladze, Phys. Rev. D 80, 071702 (2009) [arXiv:0905.2710 [hep-ph]].
    • [29] E. Aprile et al. [XENON100 Collaboration], Phys. Rev. Lett. 107 (2011) 131302 [arXiv:1104.2549 [astro-ph.CO]]; Phys. Rev. Lett. 109, 181301 (2012) [arXiv:1207.5988 [astro-ph.CO]].
    • [30] E. M. Dolle and S. Su, Phys. Rev. D 80 (2009) 055012 [arXiv:0906.1609 [hep-ph]].
    • [31] E. Komatsu et al. [WMAP Collaboration], Astrophys. J. Suppl. 192 (2011) 18 [arXiv:1001.4538 [astro-ph.CO]].
    • [32] A. Goudelis, B. Herrmann and O. Stl, arXiv:1303.3010 [hep-ph].
    • [33] M. Klasen, C. E. Yaguna and J. D. Ruiz-Alvarez, arXiv:1302.1657 [hep-ph]; M. Klasen, C. E. Yaguna, J. D. Ruiz-Alvarez, D. Restrepo and O. Zapata, arXiv:1302.5298 [hep-ph].
    • [34] P. Fileviez Perez, H. H. Patel, M. J. Ramsey-Musolf and K. Wang, Phys. Rev. D 79, 055024 (2009) [arXiv:0811.3957 [hep-ph]];
    • [35] T. Hambye, F. -S. Ling, L. Lopez Honorez and J. Rocher, JHEP 0907 (2009) 090 [Erratum-ibid. 1005 (2010) 066] [arXiv:0903.4010 [hep-ph]].
    • [36] T. Araki, C. Q. Geng and K. I. Nagao, Phys. Rev. D 83 (2011) 075014 [arXiv:1102.4906 [hep-ph]]; T. Araki, C. Q. Geng and K. I. Nagao, Int. J. Mod. Phys. D 20 (2011) 1433 [arXiv:1108.2753 [hep-ph]].
    • [37] R. Foot, A. Kobakhidze, K. L. McDonald and R. R. Volkas, Phys. Rev. D 76 (2007) 075014 [arXiv:0706.1829 [hep-ph]]; R. Foot, A. Kobakhidze, K. L. McDonald and R. R. Volkas, Phys. Rev. D 77, 035006 (2008) [arXiv:0709.2750 [hep-ph]].
    • [38] Y. Kajiyama, H. Okada and K. Yagyu, arXiv:1303.3463 [hep-ph].
    • [39] S. Kanemura and H. Sugiyama, Phys. Rev. D 86 (2012) 073006 [arXiv:1202.5231 [hepph]].
    • [40] A. Djouadi, O. Lebedev, Y. Mambrini and J. Quevillon, Phys. Lett. B 709, 65 (2012) [arXiv:1112.3299 [hep-ph]].
    • [41] K. Kumericki, I. Picek and B. Radovcic, Phys. Rev. D 86, 013006 (2012) [arXiv:1204.6599 [hep-ph]]; I. Picek and B. Radovcic, Phys. Lett. B 719, 404 (2013) [arXiv:1210.6449 [hep-ph]]. The same model is mentioned in Y. Liao, JHEP 1106, 098 (2011) [arXiv:1011.3633 [hep-ph]].
    • [42] M. Cirelli and A. Strumia, New J. Phys. 11 (2009) 105005 [arXiv:0903.3381 [hep-ph]].
    • [43] I. Picek and B. Radovcic, Phys. Lett. B 687, 338 (2010) [arXiv:0911.1374 [hepph]]; K. Kumericki, I. Picek and B. Radovcic, Phys. Rev. D 84, 093002 (2011) [arXiv:1106.1069 [hep-ph]].
  • No related research data.
  • No similar publications.

Share - Bookmark

Cite this article

Collected from