Confronting the DAMPE excess with the scotogenictype-II seesaw model

Ran Ding; Zhi-Long Han; Lei Feng; Bin Zhu

doi:10.1088/1674-1137/42/8/083104

Chinese Physics C> 2018, Vol. 42> Issue(8) : 083104 DOI: 10.1088/1674-1137/42/8/083104

Confronting the DAMPE excess with the scotogenictype-II seesaw model

Ran Ding ¹ ,
Zhi-Long Han ² ,
Lei Feng ³ ,
Bin Zhu ⁴

1.
Center for High Energy Physics, Peking University, Beijing 100871, China
2.
School of Physics and Technology, University of Jinan, Jinan 250022, China
3.
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
4.
Department of Physics, Yantai University, Yantai 264005, China

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Abstract：
The DArk Matter Particle Explorer (DAMPE) has observed a tentative peak at E～1.4 TeV in the cosmic-ray electron spectrum. In this paper, we interpret this excess in the scotogenic type-II seesaw model. This model extends the canonical type-II seesaw model with dark matter (DM) candidates and a loop-induced vacuum expectation value of the triplet scalars, v△, resulting in small neutrino masses naturally even for TeV scale triplet scalars. Assuming a nearby DM subhalo, the DAMPE excess can be explained by DM annihilating into a pair of triplet scalars which subsequently decay to charged lepton final states. Spectrum fitting of the DAMPE excess indicates it potentially favors the inverted neutrino mass hierarchy. We also discuss how to evade associated neutrino flux in our model.
- dark matter ,
- radiative neutrino mass model ,
- DAMPE excess

References

[1]	G. Ambrosi et al (DAMPE Collaboration), arXiv:1711.10981[astro-ph.HE]
[2]	X. J. Huang, Y. L. Wu, W. H. Zhang, and Y. F. Zhou, arXiv:1712.00005[astro-ph.HE]
[3]	A. Fowlie, Phys. Lett. B, 780:181 (2018) doi:10.1016/j.physletb.2018.03.006[arXiv:1712.05089[hep-ph]]
[4]	F. Aharonian et al (H.E.S.S. Collaboration), Phys. Rev. Lett., 101:261104 (2008)[arXiv:0811.3894[astro-ph]] F. Aharonian et al (H.E.S.S. Collaboration), Astron. Astrophys., 508:561 (2009)[arXiv:0905.0105[astro-ph.HE]]
[5]	Q. Yuan et al, arXiv:1711.10989[astro-ph.HE]
[6]	Y. Bai and J. Berger, JHEP, 1408:153 (2014)[arXiv:1402.6696[hep-ph]]
[7]	Y. Z. Fan, W. C. Huang, M. Spinrath, Y. L. S. Tsai, and Q. Yuan, Phys. Lett. B, 781:83 (2018) doi:10.1016/j.physletb.2018.03.066[arXiv:1711.10995[hep-ph]]
[8]	P. H. Gu and X. G. He, arXiv:1711.11000[hep-ph] G. H. Duan, L. Feng, F. Wang, L. Wu, J. M. Yang, and R. Zheng, arXiv:1711.11012[hep-ph] L. Zu, C. Zhang, L. Feng, Q. Yuan, and Y. Z. Fan, arXiv:1711.11052[hep-ph] Y. L. Tang, L. Wu, M. Zhang, and R. Zheng, arXiv:1711.11058[hep-ph] W. Chao and Q. Yuan, arXiv:1711.11182[hep-ph] P. H. Gu, arXiv:1711.11333[hep-ph] P. Athron, C. Balazs, A. Fowlie, and Y. Zhang, arXiv:1711.11376[hep-ph] J. Cao, L. Feng, X. Guo, L. Shang, F. Wang, and P. Wu, arXiv:1711.11452[hepph] G. H. Duan, X. G. He, L. Wu, and J. M. Yang, arXiv:1711.11563[hep-ph] X. Liu and Z. Liu, arXiv:1711.11579[hepph] X. J. Huang, Y. L. Wu, W. H. Zhang, and Y. F. Zhou, arXiv:1712.00005[astro-ph.HE] W. Chao, H. K. Guo, H. L. Li, and J. Shu, arXiv:1712.00037[hep-ph] Y. Gao and Y. Z. Ma, arXiv:1712.00370[astro-ph.HE] J. S. Niu, T. Li, R. Ding, B. Zhu, H. F. Xue, and Y. Wang, arXiv:1712.00372[astroph.HE] P. H. Gu, arXiv:1712.00922[hep-ph] T. Nomura and H. Okada, arXiv:1712.00941[hep-ph] R. Zhu and Y. Zhang, arXiv:1712.01143[hep-ph] K. Ghorbani and P. H. Ghorbani, arXiv:1712.01239[hep-ph] J. Cao, L. Feng, X. Guo, L. Shang, F. Wang, P. Wu, and L. Zu, arXiv:1712.01244[hepph] F. Yang and M. Su, arXiv:1712.01724[astro-ph.HE]
[9]	S. Kanemura and H. Sugiyama, Phys. Rev. D, 86:073006 (2012)[arXiv:1202.5231[hep-ph]]
[10]	P. Fileviez Perez, T. Han, G. y. Huang, T. Li, and K. Wang, Phys. Rev. D, 78:015018 (2008)[arXiv:0805.3536[hep-ph]]
[11]	I. Gogoladze, N. Okada, and Q. Shafi, Phys. Lett. B, 679:237 (2009)[arXiv:0904.2201[hep-ph]]
[12]	P. S. B. Dev, D. K. Ghosh, N. Okada, and I. Saha, Phys. Rev. D, 89:095001 (2014)[arXiv:1307.6204[hep-ph]]
[13]	C. H. Chen and T. Nomura, JHEP, 1409:120 (2014)[arXiv:1404.2996[hep-ph]]
[14]	C. H. Chen, C. W. Chiang, and T. Nomura, Phys. Lett. B, 747:495 (2015)[arXiv:1504.07848[hep-ph]]
[15]	C. H. Chen, C. W. Chiang, and T. Nomura, arXiv:1712.00793[hep-ph]
[16]	T. Li, N. Okada, and Q. Shafi, Phys. Lett. B, 779:130 (2018) doi:10.1016/j.physletb.2018.02.006[arXiv:1712.00869[hepph]]
[17]	E. Ma, Phys. Rev. Lett., 115(1):011801 (2015)[arXiv:1502.02200[hep-ph]]
[18]	S. Fraser, C. Kownacki, E. Ma, and O. Popov, Phys. Rev. D, 93(1):013021 (2016)[arXiv:1511.06375[hep-ph]]
[19]	S. Y. Guo, Z. L. Han, and Y. Liao, Phys. Rev. D, 94(11):115014 (2016)[arXiv:1609.01018[hep-ph]]
[20]	C. Bonilla, J. W. F. Valle, and J. C. Romao, Phys. Rev. D, 91(11):113015 (2015)[arXiv:1502.01649[hep-ph]]
[21]	W. Wang and Z. L. Han, Phys. Rev. D, 94(5):053015 (2016)[arXiv:1605.00239[hep-ph]]
[22]	W. Wang, R. Wang, Z. L. Han, and J. Z. Han, arXiv:1705.00414[hep-ph]
[23]	W. Wang and Z. L. Han, Phys. Rev. D, 92:095001 (2015)[arXiv:1508.00706[hep-ph]]
[24]	A. Arhrib, R. Benbrik, M. Chabab, G. Moultaka, M. C. Peyranere, L. Rahili, and J. Ramadan, Phys. Rev. D, 84:095005 (2011)[arXiv:1105.1925[hep-ph]]
[25]	Z. L. Han, R. Ding, and Y. Liao, Phys. Rev. D, 91:093006 (2015)[arXiv:1502.05242[hep-ph]]
[26]	Z. L. Han, R. Ding, and Y. Liao, Phys. Rev. D, 92(3):033014 (2015)[arXiv:1506.08996[hep-ph]]
[27]	A. Melfo, M. Nemevsek, F. Nesti, G. Senjanovic, and Y. Zhang, Phys. Rev. D, 85:055018 (2012)[arXiv:1108.4416[hep-ph]]
[28]	M. Aaboud et al (ATLAS Collaboration), arXiv:1710.09748[hep-ex] G. Aad et al (ATLAS Collaboration), JHEP, 1503:041 (2015)[arXiv:1412.0237[hep-ex]]
[29]	C. Patrignani et al (Particle Data Group], Chin. Phys. C, 40:no. 10, 100001 (2016).
[30]	A. G. Akeroyd, M. Aoki, and H. Sugiyama, Phys. Rev. D, 79:113010 (2009)[arXiv:0904.3640[hep-ph]] T. Fukuyama, H. Sugiyama, and K. Tsumura, JHEP, 1003:044 (2010)[arXiv:0909.4943[hep-ph]]
[31]	I. Esteban, M. C. Gonzalez-Garcia, M. Maltoni, I. MartinezSoler, and T. Schwetz, JHEP, 1701:087 (2017)[arXiv:1611.01514[hep-ph]]
[32]	A. Alloul, N. D. Christensen, C. Degrande, C. Duhr, and B. Fuks, Comput. Phys. Commun., 185:2250 (2014)[arXiv:1310.1921[hep-ph]]
[33]	G. BWlanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun., 192:322 (2015)[arXiv:1407.6129[hepph]]
[34]	P. A. R. Ade et al (Planck Collaboration), Astron. Astrophys., 594:A13 (2016)[arXiv:1502.01589[astro-ph.CO]]
[35]	D. S. Akerib et al (LUX Collaboration), Phys. Rev. Lett., 118(2):021303 (2017)[arXiv:1608.07648[astro-ph.CO]]
[36]	E. Aprile et al (XENON Collaboration), Phys. Rev. Lett., 119(18):181301 (2017)[arXiv:1705.06655[astro-ph.CO]]
[37]	X. Cui et al (PandaX-Ⅱ Collaboration), Phys. Rev. Lett., 119(18):181302 (2017)[arXiv:1708.06917[astro-ph.CO]]
[38]	Y. Zhao, K. Fang, M. Su, and M. C. Miller, arXiv:1712.03210[astro-ph.HE]
[39]	J. Alwall et al, JHEP, 1407:079 (2014) doi:10.1007/JHEP07(2014)079[arXiv:1405.0301[hep-ph]]
[40]	M. G. Aartsen et al (IceCube Collaboration), Eur. Phys. J. C, 77(9):627 (2017) doi:10.1140/epjc/s10052-017-5213-y[arXiv:1705.08103[hep-ex]]
[41]	M. Cirelli et al, JCAP, 1103:051 (2011); JCAP, 1210:E01 (2012)[arXiv:1012.4515[hep-ph]]
[42]	J. F. Navarro, C. S. Frenk, and S. D. M. White, Astrophys. J., 462:563 (1996)[astro-ph/9508025]
[43]	J. F. Navarro, C. S. Frenk, and S. D. M. White, Astrophys. J., 490:493 (1997)[astro-ph/9611107]
[44]	A. W. Strong and I. V. Moskalenko, Astrophys. J., 509:212 (1998)[astro-ph/9807150]
[45]	I. V. Moskalenko and A. W. Strong, Astrophys. J., 493:694 (1998)[astro-ph/9710124]
[46]	M. Aguilar et al (AMS Collaboration), Phys. Rev. Lett., 113:121102 (2014)
[47]	S. Abdollahi et al (Fermi-LAT Collaboration), Phys. Rev. D, 95(8):082007 (2017)[arXiv:1704.07195[astro-ph.HE]]

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Ran Ding, Zhi-Long Han, Lei Feng and Bin Zhu. Confronting the DAMPE excess with the scotogenictype-II seesaw model[J]. Chinese Physics C, 2018, 42(8): 083104. doi: 10.1088/1674-1137/42/8/083104

Ran Ding, Zhi-Long Han, Lei Feng and Bin Zhu. Confronting the DAMPE excess with the scotogenictype-II seesaw model[J]. Chinese Physics C, 2018, 42(8): 083104. doi: 10.1088/1674-1137/42/8/083104 shu

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Confronting the DAMPE excess with the scotogenictype-II seesaw model

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