Interpretations of the cosmic ray secondary-to-primary ratios measured by DAMPE

doi:10.1007/s11467-023-1257-7

Front. Phys.

2023, Vol. 18

Issue (4) : 44301 https://doi.org/10.1007/s11467-023-1257-7

RESEARCH ARTICLE

Interpretations of the cosmic ray secondary-to-primary ratios measured by DAMPE

Peng-Xiong Ma¹, Zhi-Hui Xu^1,², Qiang Yuan^1,²(

), Xiao-Jun Bi^3,⁴, Yi-Zhong Fan^1,², Igor V. Moskalenko⁵, Chuan Yue¹

¹. Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
². School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
³. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
⁴. University of Chinese Academy of Sciences, Beijing 100049, China
⁵. W. W. Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA

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Abstract

Precise measurements of the boron-to-carbon and boron-to-oxygen ratios by DAMPE show clear hardenings around 100 GeV/n, which provide important implications on the production, propagation, and interaction of Galactic cosmic rays. In this work we investigate a number of models proposed in literature in light of the DAMPE findings. These models can roughly be classified into two classes, driven by propagation effects or by source ones. Among these models discussed, we find that the re-acceleration of cosmic rays, during their propagation, by random magnetohydrodynamic waves may not reproduce sufficient hardenings of B/C and B/O, and an additional spectral break of the diffusion coefficient is required. The other models can properly explain the hardenings of the ratios. However, depending on simplifications assumed, the models differ in their quality in reproducing the data in a wide energy range. The models with significant re-acceleration effect will under-predict low-energy antiprotons but over-predict low-energy positrons, and the models with secondary production at sources over-predict high-energy antiprotons. For all models high-energy positron excess exists.

Keywords cosmic rays propagation

Corresponding Author(s): Qiang Yuan

About author:

Changjian Wang and Zhiying Yang contributed equally to this work.

Issue Date: 27 February 2023

Cite this article:

Peng-Xiong Ma,Zhi-Hui Xu,Qiang Yuan, et al. Interpretations of the cosmic ray secondary-to-primary ratios measured by DAMPE[J]. Front. Phys. , 2023, 18(4): 44301.

URL:

https://academic.hep.com.cn/fop/EN/10.1007/s11467-023-1257-7
https://academic.hep.com.cn/fop/EN/Y2023/V18/I4/44301

Fig.1 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the NLB model.

Tab.1 Data used in the fitting.

Model	B	B′	D	E	F	G

$D 0$ ( $1028$ $c m 2$ · $s − 1$ )	6.02	3.32	8.14	...	7.30	6.94
$δ$	0.40	0.46	0.60	...	0.47	0.43
$z h$ (kpc)	5.77	3.61	8.48	...	6.23	6.29
$δ h$	...	0.25	...	...	...	...
$R h$ (GV)	...	212.5	...	...	...	...
$v A$ (km·s⁻¹)	30.0	22.4	10.3	...	35.4	32.5
$η$	−0.10	−0.61	−0.42	...	−0.27	−0.33
$ξ$	...	...	...	...	...	...
$ξ δ$	...	...	0.02	...	...	...
$h$ (kpc)	...	...	0.41	...	...	...
$τ$ (Myr)	...	...	...	...	0.46	0.24
$R a c$ (GV)	...	...	...	...	...	4.0 × 10³
$γ 0$	0.19	0.41	0.13	0.85	0.46	0.45
$γ 1$	2.36	2.35	2.38	2.37	2.31	2.34
$γ 2$	2.34	2.42	...	...	2.15	2.18
$R b r, 1$ (GV)	0.93	1.02	1.03	1.75	1.05	1.05
$R b r, 2$ (GV)	243.2	142.3	...	...	467.0	467.0
$ϕ$ (GV)	0.71	0.69	0.71	0.68	0.71	0.69

Tab.2 Parameters of the models discussed in Section 3.

Fig.2 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the re-acceleration model. Red thick lines show the results for the diffusion coefficient of Eq. (2), and blue thin lines show the results for the diffusion coefficient with an additional high-energy break. Dashed lines are the spectra in the local ISM, and solid lines are modulated spectra near the Earth. Sub-panels of bottom ones show the residuals of the model fittings to the C and O spectra. The open symbols are for model B and filled symbols are for model B

′

Fig.3 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the model with re-acceleration by a nearby source.

Fig.4 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the spatially-dependent propagation model. Dashed lines are the spectra in the local ISM, and solid lines are modulated spectra near the Earth. Sub-panels of bottom ones show the residuals of the model fittings to the C and O spectra.

Fig.5 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the Self-generated turbulence model. Dashed lines are the spectra in the local ISM, and solid lines are modulated spectra near the Earth. Sub-panels of bottom ones show the residuals of the model fittings to the C and O spectra.

Fig.6 B/C and B/O ratios (top panels), and C, O fluxes (bottom panels) for the models with secondary production (model F; red thin lines) and acceleration (model G; green thick lines) at source. Dashed lines are the spectra in the local ISM, and solid lines are modulated spectra near the Earth. Sub-panels of bottom ones show the residuals of the model fittings to the C and O spectra. The filled symbols are for model F and open symbols are for model G.

Fig.7 Spectra of protons (top panels), antiprotons (middle panels), and positrons (bottom panels) for the model predictions, compared with the data [14, 41, 98-100]. The left panels show the predictions of models B, B′, D, E, and the right panels show the predictions of models F and G. The solar modulation potential is about

0.7

GV for all species.

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