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

Abstract
HTML
Reference
Related

PDF

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]]

[1]	Kai-Yu Zhang , Wan-Zhe Feng . Explaining the W boson mass anomaly and dark matter with a U(1) dark sector. Chinese Physics C, 2023, 47(2): 023107. doi: 10.1088/1674-1137/aca585
[2]	Ming-Jie Zhang , Shu-Min Zhao , Xing-Xing Dong , Zhong-Jun Yang , Tai-Fu Feng . Scalar neutrino dark matter in the BLMSSM. Chinese Physics C, 2021, 45(9): 093106. doi: 10.1088/1674-1137/ac0c0e
[3]	Yidian Chen , Xiao-Jun Bi , Mei Huang . Holographic technicolor model and dark matter. Chinese Physics C, 2020, 44(9): 093102. doi: 10.1088/1674-1137/44/9/093102
[4]	Wen Yin . Dark matter, neutrino mass, cutoff for cosmic-ray neutrino, and the Higgs boson invisible decay from a neutrino portal interaction. Chinese Physics C, 2019, 43(4): 045101. doi: 10.1088/1674-1137/43/4/045101
[5]	Yi Zhao , Xiao-Jun Bi , Su-Jie Lin , Peng-Fei Yin . Nearby dark matter subhalo that accounts for the DAMPE excess. Chinese Physics C, 2019, 43(8): 085101. doi: 10.1088/1674-1137/43/8/085101
[6]	Kun Wang , Fei Wang , Jingya Zhu , Quanlin Jie . The semi-constrained NMSSM in light of muon g-2, LHC, anddark matter constraints. Chinese Physics C, 2018, 42(10): 103109. doi: 10.1088/1674-1137/42/10/103109
[7]	Rui-Yun Guo , Jing-Fei Zhang , Xin Zhang . Exploring neutrino mass and mass hierarchy in the scenario of vacuum energy interacting with cold dark matter. Chinese Physics C, 2018, 42(9): 095103. doi: 10.1088/1674-1137/42/9/095103
[8]	Andrea Addazi , Antonino Marcianò . Gravitational waves from dark first order phase transitions and dark photons. Chinese Physics C, 2018, 42(2): 023107. doi: 10.1088/1674-1137/42/2/023107
[9]	Andrea Addazi , Stephon Alexander , Yi-Fu Cai , Antonino Marcianó . Dark matter and baryogenesis in the Fermi-bounce curvaton mechanism. Chinese Physics C, 2018, 42(6): 065101. doi: 10.1088/1674-1137/42/6/065101
[10]	Andrea Addazi , Pietro Donà , Antonino Marcianò . Dynamical interactions of dark energy and dark matter: Yang-Mills condensate and QCD axions. Chinese Physics C, 2018, 42(7): 075102. doi: 10.1088/1674-1137/42/7/075102
[11]	Liuyuan Shen , Yicen Mou , Yunlong Zheng , Mingzhe Li . Direct couplings of mimetic dark matter and their cosmological effects. Chinese Physics C, 2018, 42(1): 015101. doi: 10.1088/1674-1137/42/1/015101
[12]	Ran Ding , Zhi-Long Han , Li Huang , Yi Liao . Phenomenology of colored radiative neutrino mass model and its implications on cosmic-ray observations. Chinese Physics C, 2018, 42(10): 103101. doi: 10.1088/1674-1137/42/10/103101
[13]	Peyman Zakeri , Mohammad Moosavi , Mohammadreza Zakeri , Yaser Ayazi . A minimal model for two-component FIMP dark matter: A basic search. Chinese Physics C, 2018, 42(7): 073101. doi: 10.1088/1674-1137/42/7/073101
[14]	Guoli Liu , Fei Wang , Wenyu Wang , Jin-Min Yang . Explaining DAMPE results by dark matter with hierarchical lepton-specific Yukawa interactions. Chinese Physics C, 2018, 42(3): 035101. doi: 10.1088/1674-1137/42/3/035101
[15]	Shivaramakrishna Singirala . Implications of fermionic dark matter on recent neutrino oscillation data. Chinese Physics C, 2017, 41(4): 043102. doi: 10.1088/1674-1137/41/4/043102
[16]	Zhi-Ying Li , Zhi-Yong Zhang , Yi-Feng Wei , Chi Wang , Yun-Long Zhang , Si-Cheng Wen , Xiao-Lian Wang , Zi-Zong Xu , Guang-Shun Huang . Energy correction for the BGO calorimeter of DAMPE using an electron beam. Chinese Physics C, 2016, 40(8): 086202. doi: 10.1088/1674-1137/40/8/086202
[17]	Yi-Ming Hu , Jin Chang , Deng-Yi Chen , Jian-Hua Guo , Yun-Long Zhang , Chang-Qing Feng . Environmental test of the BGO calorimeterfor DArk Matter Particle Explorer. Chinese Physics C, 2016, 40(11): 116003. doi: 10.1088/1674-1137/40/11/116003
[18]	S. A. Alavi , F. S. Kazemian . Photonic dark matter portal and quantum physics. Chinese Physics C, 2016, 40(2): 025101. doi: 10.1088/1674-1137/40/2/025101
[19]	KANG Ke-Jun , YUE Qian , WU Yu-Cheng et al. (CDEX collaboration) and (TEXONO collaboration) . CDEX-1 1 kg point-contact germanium detector for low mass dark matter searches. Chinese Physics C, 2013, 37(12): 126002. doi: 10.1088/1674-1137/37/12/126002
[20]	CHANG Xue , LIU Chun , MA Feng-Cai , YANG Shuo . Supersymmetric extension of the minimal dark matter model. Chinese Physics C, 2012, 36(9): 810-817. doi: 10.1088/1674-1137/36/9/003

Access

Get Citation

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

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2018-04-10

Article Metric

Article Views(1609)
PDF Downloads(43)
Cited by(0)

Policy on re-use

To reuse of Open Access content published by CPC, for content published under the terms of the Creative Commons Attribution 3.0 license (“CC CY”), the users don’t need to request permission to copy, distribute and display the final published version of the article and to create derivative works, subject to appropriate attribution.

通讯作者: 陈斌, bchen63@163.com

1.
沈阳化工大学材料科学与工程学院沈阳 110142

Confronting the DAMPE excess with the scotogenictype-II seesaw model

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article

Confronting the DAMPE excess with the scotogenictype-II seesaw model

HTML

目录