Galactic cosmic ray propagation: sub-PeV diffuse gamma-ray and neutrino emission

doi:10.1007/s11467-022-1188-8

Front. Phys.

2022, Vol. 17

Issue (6) : 64501 https://doi.org/10.1007/s11467-022-1188-8

RESEARCH ARTICLE

Galactic cosmic ray propagation: sub-PeV diffuse gamma-ray and neutrino emission

Bing-Qiang Qiao¹, Wei Liu¹(

), Meng-Jie Zhao^1,²(

), Xiao-Jun Bi¹, Yi-Qing Guo^1,²

¹. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
². University of Chinese Academy of Sciences, Beijing 100049, China

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Abstract

The Tibet ASγ experiment just reported their measurement of sub-PeV diffuse gamma-ray emission from the Galactic disk, with the highest energy up to 957 TeV. These diffuse gamma rays are most likely the hadronic origin by cosmic ray (CR) interaction with interstellar gas in the galaxy. This measurement provides direct evidence to the hypothesis that the Galactic Cosmic Rays (GCRs) can be accelerated beyond PeV energies. In this work, we try to explain the sub-PeV diffuse gamma-ray spectrum with different CR propagation models. We find that there is a tension between the sub-PeV diffuse gamma-ray and the local CR spectrum. To describe the sub-PeV diffuse gamma-ray flux, it generally requires larger local CR flux than measurement in the knee region. We further calculate the PeV neutrino flux from the CR propagation model. Even all of these sub-PeV diffuse gamma rays originate from the propagation, the Galactic Neutrinos (GNs) only account for less than ~15% of observed flux, most of which are still from extragalactic sources.

Keywords galactic cosmic ray diffuse gamma ray neutrino

Corresponding Author(s): Wei Liu,Meng-Jie Zhao

Issue Date: 27 July 2022

Cite this article:

Bing-Qiang Qiao,Wei Liu,Meng-Jie Zhao, et al. Galactic cosmic ray propagation: sub-PeV diffuse gamma-ray and neutrino emission[J]. Front. Phys. , 2022, 17(6): 64501.

URL:

https://academic.hep.com.cn/fop/EN/10.1007/s11467-022-1188-8
https://academic.hep.com.cn/fop/EN/Y2022/V17/I6/64501

Fig.1 Calculation of B/C ratio to obtain the propagation parameters in HD, SDP-A and SDP-B models, with B/C data taken from the AMS-02 measurement [47].

Model	$D 0 (c m 2 ? s − 1)$	$δ 0$	$N m$	$ξ$	$n$	$v A (k m ? s − 1)$	$L (k p c)$

HD	4.75 × 10²⁸	0.46				22	5
SDP-A	5.64 × 10²⁸	0.56	0.51	0.1	3.5	6	5
SDP-B	5.84 × 10²⁸	0.55	0.49	0.1	3.5	6	5

Tab.1 Diffusion parameters of three propagation models.

Fig.2 Calculated proton and helium energy spectra in propagation models of HD, SDP-A and SDP-B. The proton and helium data are taken from AMS-02 [50, 51], CREAM-II [48], NUCLEON [52], DAMPE [49] and KASCADE [53], IceTop [54] and HAWC [55].

Model	Parameters	p	He	C	N	O	Ne	Mg	Si	Fe

HD	Normalization*	4420	401	16.8	2.26	19.3	2.24	2.78	4.20	2.92
	$10 − 5 [(m 2 ? s r ? s ? G e V) − 1]$	4420	401	16.8	2.26	19.3	2.24	2.78	4.20	2.92
	$ν$	2.32	2.26	2.31	2.37	2.32	2.31	2.31	2.41	2.27
	$R c (P V)$	7	7	7	7	7	7	7	7	7
SDP-A background	Normalization	4090	259		1.40	13.3	1.50	1.86	2.05	2.21
	$10 − 5 [(m 2 ? s r ? s ? G e V) − 1]$	4090	259		1.40	13.3	1.50	1.86	2.05	2.21
	$ν$	2.37	2.29	2.32	2.37	2.34	2.32	2.33	2.45	2.32
	$R c (P V)$	7	7	7	7	7	7	7	7	7
SDP-A local	$q 0$	2800	1400	36	5.2	40	6.2	6.6	5.7	5.2
	$1049 (G e V − 1)$	2800	1400	36	5.2	40	6.2	6.6	5.7	5.2
	$α$	2.10	2.10	2.05	2.05	2.05	2.05	2.05	2.05	2.05
	$R c ′ (T V)$	28	28	28	28	28	28	28	28	28
SDP-B	Normalization	4500	282	12.8	1.84	15.8	1.93	2.59	2.64	2.89
	$10 − 5 [(m 2 ? s r ? s ? G e V) − 1]$	4500	282	12.8	1.84	15.8	1.93	2.59	2.64	2.89
	$ν$	2.34	2.26	2.33	2.39	2.34	2.35	2.37	2.41	2.35
	$R c (P V)$	3.5	3.5	3.5	3.5	3.5	3.5	3.5	3.5	3.5

Tab.2 Injection parameters of the background and local sources in three propagation models.

Fig.3 Calculated all-particle spectra in three propagation models. The all-particle data are taken from Horandel [56], IceTop [54, 57], Tibet [5], HAWC [58], ARGO [59], ATIC [60], NUCLEON [61] and KASCADE [4].

Fig.4 Calculated diffuse gamma-ray spectra in three propagation models. The gamma ray data are taken from ARGO-YBJ [64] and Tibet AS+MD [19] experiments.

Fig.5 Diffuse neutrino flux calculated by the three propagation models. The data are taken from the ICECUBE

7.5

years’ observation [66]. The violet line is the power-law fitting to the data, with normalization

Φ = 6.37 × 1018

GeV⁻¹·cm⁻²·s⁻¹·sr⁻¹ at

100

TeV and power index

γ = − 2.87

. The orange bar with arrows exhibits the 90% C.L. upper limit for the neutrino flux of the Galactic plane using the ANTARES neutrino telescope[67], while the gray bar with arrows is the same as above except for using the IceCube 7 years data [68].

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[1]	Bing-Qiang Qiao, Wei Liu, Meng-Jie Zhao, Xiao-Jun Bi, Yi-Qing Guo. Galactic cosmic ray propagation: sub-PeV diffuse gamma-ray and neutrino emission[J]. Front. Phys. , 2022, 17(4): 44501-.
[2]	Miao He. Overview on neutrinos and the Daya Bay experiment[J]. Front. Phys. , 2013, 8(3): 242-247.

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