The origin and acceleration mechanisms of energetic particles in the universe remain enigmatic in contemporary astrophysics. Recent efforts have focused on identifying Galactic sources capable of accelerating particles to 1 PeV known as PeVatrons and also identifying sources contributing to the spectrum at lower energies. The different morphology of galactic supernova remnants is directly related to the type of stellar explosion and the existence of a possible Compact Central Object CCO which possess intense radiativegravitational fields on their surfaces. These CCOs due to their strong fields and interactions with surrounding magnetic clouds are potential candidates for gamma ray production. Through observations of the compact Xray source 1E 1207.45209 located near the remnant G296.510.0 and using the enhanced GALPROP code we analyze the emission of gammaray and cosmicray production through propagation. Additionally we calculate the contribution of the G296.510.0 source to the overall observed Galactic cosmicray flux taking into account cosmicray propagation within the Galaxy which includes energy losses and particle interactions. Our findings suggest that this setup offers a fertile environment for producing a wide range of cosmicray energies at low energy within the Galaxy.
['Astrophysics - High Energy Astrophysical Phenomena', 'Astrophysics - Solar and Stellar Astrophysics', 'High Energy Physics - Phenomenology', 'High Energy Physics - Theory']
Cosmicgammaray emission at lowluminosity from CCO 1E 1207.45209 and its Host SNR G296.510.0
{'Cosmic-gamma-ray emission at low-luminosity from CCO 1E 1207.4-5209 and its Host SNR G296.5+10.0': "Luana N. Padilha, a, 1 Rita C. dos Anjos, a,b,c,d Jaziel G. Coelho, d,e Luiz A. S. Pereira f  \n- a Programa de p'os-gradua¸c˜ao em F'ısica & Departamento de F'ısica, Universidade Estadual de Londrina (UEL), 86057-970 Londrina, PR, Brazil\n- b Departamento de Engenharias e Exatas, Universidade Federal do Paran'a (UFPR), Pioneiro, 2153, 85950-000 Palotina, PR, Brazil\n- c Applied Physics Graduation Program, Federal University of Latin-American Integration, 85867-670, Foz do Igua¸cu , PR, Brazil\n- d N'ucleo de Astrof'ısica e Cosmologia (Cosmo-Ufes) & Departamento de F'ısica, Universidade Federal do Esp'ırito Santo, 29075-910, Vit'oria, ES, Brazil\n- e Divis˜ao de Astrof'ısica, Instituto Nacional de Pesquisas Espaciais, Avenida dos Astronautas 1758, 12227-010, S˜ao Jos'e dos Campos, SP, Brazil\n- f Unidade Acadˆemica de F'ısica, Universidade Federal de Campina Grande, 58429-900, Campina Grande, PB, Brazil  \nE-mail: luana.natalie.padilha@uel.br, ritacassia@ufpr.br, jaziel.coelho@ufes.br,  \nluizstuani@uaf.ufcg.edu.br  \nAbstract. The origin and acceleration mechanisms of energetic particles in the universe remain enigmatic in contemporary astrophysics. Recent efforts have focused on identifying Galactic sources capable of accelerating particles to 1 PeV, known as PeVatrons, and also identifying sources contributing to the spectrum at lower energies. The different morphology of galactic supernova remnants is directly related to the type of stellar explosion and the existence of a possible Compact Central Object (CCO), which possess intense radiativegravitational fields on their surfaces. These CCOs, due to their strong fields and interactions with surrounding magnetic clouds, are potential candidates for gamma ray production. Through observations of the compact X-ray source 1E 1207.4-5209, located near the remnant G296.5+10.0, and using the enhanced GALPROP code, we analyze the emission of gamma-ray and cosmic-ray production through propagation. Additionally, we calculate the contribution of the G296.5+10.0 source to the overall observed Galactic cosmic-ray flux, taking into account cosmic-ray propagation within the Galaxy, which includes energy losses and particle interactions. Our findings suggest that this setup offers a fertile environment for producing a wide range of cosmic-ray energies at low energy within the Galaxy.", '1 Introduction': "Extensive research has revealed that many astrophysical objects within our galaxy are neutron stars (NS). Intriguingly, these discoveries often align with the locations of Supernova Remnants (SNRs) [1]. These sources, known as Compact Central Objects (CCOs), are identifiable by their intense thermal X-ray emissions and a notable absence of radio and gamma-ray emissions [2]. In particular, CCOs exhibit characteristics [see 3, 4] that make them ideal candidates for particle acceleration at extremely high energies. This potential is amplified by the fact that CCOs and their associated supernova remnants provide an excellent opportunity to integrate kinematic data from both the neutron star and the supernova shock wave [1].  \nSupernova remnants and the potential presence of compact central object CCOs are inherently linked to the type of explosion of the progenitor star. Consequently, they exhibit distinct morphologies, often influenced by the materials in their vicinity and the compression of diverse magnetic fields [5]. CCOs are astronomical entities located at the geometric centers of supernova remnants, characterized by thermal X-ray emissions in the hundreds of electronvolts (eV) range and luminosities ranging from 10 33 to 10 34 (erg / s -1 ) [see, e.g., 6, 7]. An intriguing characteristic of these objects is their minimal emissions in alternative energy bands [2, 7, 8]. Due to their elusive nature, only ten CCOs have been officially cataloged, with many more potentially existing but not yet discovered [see, e.g., 1]. Measurements of their rotational periods and decay rates indicate that these objects possess antimagnetic properties, with weak magnetic fields spanning the range of 10 10 to 10 11 G. These weak magnetic fields likely result from magnetic dipole braking, suggesting that CCOs are relatively young entities [see, e.g., 9].  \nMultimessenger astronomy approaches to the origin search of cosmic rays (CRs) are based on the inclusion of all available information from charged CRs and neutral secondaries generated near sources by interactions. In particular, neutron and gamma rays flux through the interaction of CRs with fields. Furthermore, accelerated electrons and positrons can produce radiation through the synchrotron emission, bremsstrahlung and Inverse Compton [10, 11]. The relationship between the propagation of cosmic rays and the integral flux of secondary gamma-rays from a source determined cosmic ray luminosities in models both inside and outside of our Galaxy [12-16].  \nThis paper calculates the contribution of the secondary gamma rays from charge particles by the CCO 1E 1207.4-5209 and its host SNR G296.5 + 10.0 association [17] using the v57 GALPROP release [18] with 3D maps of the Galactic magnetic field, diffuse interstellar  \nmedium (ISM) distributions, the interstellar radiation field (ISRF), and the gas distribution throughout the Galaxy. Our simulation model centers on CCO 1E 1207.4-5209 parameters, distinguished by their measured magnetic field. The description of the source is given precedence according to predetermined criteria, including location, age, period variation, and luminosity.  \nThis study was motivated by the coexistence of CCO 1E 1207.4-5209 within the vicinity of its host SNR G296.5+10.0 [17]. SNR G296.5+10.0 has been widely investigated as a high energy gamma-ray emitter, with a focus on the lepto-hadronic spectral energy distribution of the remnant for synchrotron, inverse Compton, Bremsstrahlung, and proton-proton processes [19-21]. In this context, this work aims to quantify a potential gamma-ray emission from the SNR G296.5+10.0 and CCO 1E 1207.4-5209 to the region, which cannot be ignored due to glitch processes associated with the spin-down rate [22] and changes in the pulsar's spin period [23].  \nThis manuscript is organized as follows. The next section presents in detail the association CCO 1E 1207.4-5209 and its host SNR G296.5 + 10.0. The third section presents the description of simulation models. Beyond that, in this section we describe our multimessenger analysis. The final section provides the main conclusions and discussions of this investigation.", '2 CCO 1E 1207.4-5209 and its host SNR G296.5 + 10.0': "The neutron star 1E 1207.4-5209 is a radio-quiet, fast-rotating object of the CCO class [24], which was detected near the core of SNR G296.5+10.0 by the Einstein satellite [25]. Situated at the geometric center of the supernova remnant G296.5+10.0 (also named PKS 1209-51), the CCO 1E 1207.4-5209 was the focus of a comprehensive XMM-Newton spacecraft observation in August 2002 [26]. Using the EPIC 12,13 instrument, the observations lasted approximately 36 hours and significantly advanced the study of its emission [27]. This CCO possesses a rotational period of 0.42413076 seconds, and its period derivative is constrained by an upper limit of 2 . 224 × 10 -17 s; s -1 (according to the ATNF catalog 1 ). Situated in the Centaurus constellation, it is positioned at a distance of 2 kiloparsecs [28]. As reported by [27], the light curve of this object spans an energy range from 0.2 to 4 keV.  \nIt is the second isolated neutron star (INS) candidate discovered inside a supernova remnant (SNR) thermally emitting [17]. The supernova remnant G296.5+10.0 exhibits intense X-ray and radio emissions concentrated in the southern, eastern, and southwestern regions [29]. It possesses a bilateral morphology, with symmetry axes parallel to the Galactic plane and two bright arms on the sides. Some experts suggest that the remnant features tangentially positioned filaments composed of compressed cold gas clouds [see 30], along with a shell consisting of H I [31].  \nThe pulsar 1E 1207.4-5209 is widely recognized as the first to exhibit strong absorption lines. It was suggested that a young age and a low level of magnetospheric activity are favorable conditions for detecting atomic spectral features of elements with Z > 1 [26]. In older objects, these elements would be overlaid by a thin layer of accumulated hydrogen or masked by non-thermal processes in young and energetic pulsars. Following that, the possible composition of the atmosphere was tightly restricted by subsequent research [32], indicating that the absorption characteristics are naturally linked to oxygen or neon with helium-like properties in a magnetic field of around ∼ 10 12 G. Consequently, pulsar's magnetosphere is  \nan environment rich in positrons and electrons and is subjected to acceleration through the pulsar's spin-down mechanism.  \nThis source stands out as a unique computational neutron star in which the magnetic field is directly measured, rather than being inferred, as in other objects of its class. The XMM-Newton telescope detected X-ray absorption lines in its spectrum, which can be interpreted as cyclotron resonance of electrons near the central object's surface. The cyclotron lines (0.7 keV) correspond to a magnetic field of approximately 8 × 10 10 G or 1 . 6 × 10 14 G [see 9, 27, 33, 34]. Another intriguing characteristic of this CCO is its age, as it is believed to have formed simultaneously with the associated supernova remnant, given its origin linked to the death of the progenitor star. However, the remarkable age of 1E 1207.4-5209 exceeds by three orders of magnitude the age of the supernova G296.5+10.0. This suggests the presence of a significant braking index, especially if the current rotation period of the star is approximated to its characteristic period [see, e.g., 33]. These features make this CCO notable among other known pulsars.", '3 Description of simulation models': "In its most recent version 57, the GALPROP program was utilized to create a realistic model. GALPROP solves the transport equation, Eq. 3.1, for a given source distribution while accounting for all spatial and energetic processes that the particles encounter during propagation [18].  \n∂N ∂t = Q ( x , p ) + ⃗ ∇ . ( D xx ⃗ ∇ N -⃗vN ) + ∂ ∂p p 2 D pp ∂ ∂p 1 p 2 N -∂ ∂p ( ˙ pN -p 3 ( ⃗ ∇ .⃗v ) N ) -2 ∑ i =1 N τ i , (3.1)  \nwhere Q is a source term for the injection of cosmic rays, including secondary creation of cosmic rays, and N ( x, p ) is the density of cosmic rays per unit of total particle momentum. The spatial diffusion coefficient in our model is D xx , the convection velocity is ⃗v , and the time scales for radioactive decay ( τ 1 ) and fragmentation ( τ 2 ). A power law with an index δ determines the diffusion coefficient, which is a scalar function homogeneous and isotropic throughout the Galaxy. It is expressed as D xx = βD 0 ,xx ( ρ/ρ 0 ) δ , where ρ 0 = 3 GV, D 0 ,xx is a diffusion constant, and β is the velocity expressed in units of light speed. The convection velocity ⃗v ( z ) is assumed to increase linearly with the distance z between the plane and the halo. In a single zone | z | > 1 kpc, cosmic-ray propagation is diffusive-convective [35]. At low energies, up to ∼ 1 GeV [36], both galactic wind and energy losses play a significant role. A momentum diffusion coefficient D pp determines the re-acceleration. It is related to the spatial coefficient D xx via D pp ∝ p 2 v 2 a /D xx , where the Alfv'en speed is denoted by v a , the momentum loss rate is ˙ p ≡ dp/dt , and the Kolmogorov spectrum of turbulence is taken into account.  \nThe transport equation is solved by the software using the Crank-Nicholson model of second order. Utilizing source abundance relations for isotope generation and the boroncarbon ratio in terms of the stiffness and dispersion characteristics, the diffusion coefficient is computed [see 16, for details]. The Galactic gas distribution was modeled using a high column density H model [37]. Energy losses from synchrotron and Compton scattering processes are taken into account by the GALPROP code, which calculates the losses using an observer centered on the solar system. Furthermore, the interstellar radiation field is modeled using an R12 model [see 38]. For the Galactic magnetic field, a basic exponential model is taken  \ninto account [39]. The magnetic field has cylindrical symmetry and was chosen to describe the synchrotron emission: B ( r, z ) = B 0 e ( R ⊙ -r ) /R B e -| z | /z B [40], where R ⊙ = 8 . 5 kpc is the Solar Radius, B 0 = 5 µ G , R B = 6 kpc and z B = 2 kpc are the radial and vertical scale lengths [41]. This model only accounts the random magnetic field distribution, which is related to the diffusive features of cosmic rays [42, 43]. The current model cannot account for significant magnetic fields near the galactic core [44]. An overview of the simulation parameters is provided in Table 1. The source function Q ( x , p ) is written as n ( x ) q ( p ), where  \nTable 1 : Simulation parameters  \nn ( x ) is the amount of energy injected by cosmic rays and electrons/positrons and q ( p ) is their spatial distribution. We use a differential injection spectrum that is based on a power law for momentum dq ( p ) /dp ∝ p -α , characterized by indices of 2.2 - 2.6 [45, 46]. The Models inject particles following a δ -function centered at the source.  \nThe spin-down model was the initial emission model considered for CCO 1E 1207.4520. In this scenario, dipole radiation is responsible for the pulsar's power loss and electron acceleration. We consider the contribution of a continuous source of energetic particles (electrons and positrons) to the spatial distribution at the position of the CCO 1E 1207.45209 vicinity. With an injection power that follows a power law with a smooth break and accelerated acceleration, the model implies that the spectrum is normalized by [16, 18, 47, 48]  \nL ( t ) = ηL 0 ( 1 + t τ 0 ) -2 , (3.2)  \nwhere L 0 = 1 . 0 × 10 33 erg s -1 [27, 28] is the initial rotational power of the source, η = 1 is the efficiency, and τ 0 = 3 . 63 × 10 5 yr is the time scale of the pulsar 2 . The rate of cosmic-ray production correlates with the spin down of pulsars [see 16, 48].  \nThe second model utilizes quiescent emission or magnetic energy injection to generate a cosmic-ray luminosity and afterwards derives a gamma-ray luminosity based on the upper limits set by the H.E.S.S. Collaboration [21]. Fermi-accelerated protons lose their energy by hadronic interaction (p-p), producing neutral pions that decay into photons and form the primary source of gamma-ray observations. Depending on the energy of the gamma rays, they can be observed with space- and ground-based instruments [49]. Very high gammaray emission (VHE) can result from interactions between protons or electrons, matter, and radiation. Extragalactic models suggest that the relationship between the total flux of GeVTeV gamma rays emitted by a source and the propagation of cosmic rays can establish an  \nupper limit on the overall luminosity of cosmic rays [12, 13]. Some sources have only an upper limit on the integral of the gamma-ray flux provided. For these objects, the upper limit constrains the total of the primary and secondary photon fluxes. We assume that the measured upper limit flux of GeV-TeV gamma rays is regarded as the upper limit on secondary gamma rays created by cosmic rays traveling from a distant source to Earth. In that case, we can determine the cosmic-ray luminosity.  \nThis paper presents an approach that establishes a correlation between the cosmic-ray luminosity and a measured upper limit to the integral flux of GeV-TeV gamma rays from SNR G296.5+10.0. An isotropic cosmic-ray emission is assumed. The luminosity of the cosmic-ray flux of SNR G296.5+10.0 is directly proportional to the secondary gamma-ray flux it generates. The gamma-ray production per unit volume is conservative and can be expressed as the following function of cosmic-ray luminosity:  \nI γ ( E γ ) ∼ n gas W CR 4 πd 2 ⟨ E 0 ⟩ K γ P γ ( E γ ) , (3.3)  \nwhere W CR is the total energy of the nuclei, n gas is the gas number density, and ⟨ E 0 ⟩ is the average energy, E γ is the gamma-ray energy, and K γ and P γ ( E γ ) are the gamma-ray number from cosmic-ray propagation and the gamma-ray energy distribution recorded on Earth, respectively [15, 16, 50, 51].  \nThe upper limit of (1 . 19 ± 0 . 11) × 10 -9 cm -2 s -1 for the integral flux in the 1 GeV < E < 1 TeV range was obtained by H.E.S.S at the confidence level (CL) 99. 5% [21]. The secondary gamma-ray flux generated by SNR G296.5 + 10.0 is proportional to its cosmic-ray flux or luminosity, according to the previously established model. The results derived for the gamma-ray emission and spectral energy distribution from these models are discussed in the following section. The simulations are based on the parameters of the association CCO 1E 1207.4-5209 + SNR G296.5+10.0.", '4 Discussions': 'This section contains the results of the transport models we developed. We begin by analyzing the spectra distributions of four elements in cosmic rays using distinct model emission. The 2D gas distribution of the interstellar gas was used to simulate the models [38, 52]. Figure 1 shows the spectral energy distribution of the gamma-ray emissions resulting from the proton in Supernova Remnant (SNR) G296.5 + 10.0 and electron/positron from CCO at the spectral indexes of 2.2 (a), 2.4 (b) and 2.6 (c). A range of values between 2.0 and 2.6 was selected according to the spectrum of individual sources and observations as described in [15, 45]. The key observation is that the CCO exerts a considerable influence on gamma rays in its vicinity at high energies (E > 10 6 MeV) through the inverse Compton process, as depicted in Figure 1-(c). It may be inferred that the rotating properties of the object lead to an injection power of electrons.  \nThe plot 1 illustrates the poor gamma-ray data/model of CCO 1E 1207.4-5209 and its corresponding Supernova Remnant (SNR) G296.5 + 10.0. This is based on the model proposed by [21] and the gamma-ray measurements conducted by [53]. The lines indicate a larger fraction of gamma radiation emission in the energy range of 10 2 -10 5 MeV, where the simulation data meet the CCO gamma emission data [53], for all spectral indexes in Fig. 1-(a,b,c). In the spin-down scenario, gamma-ray emission is mostly produced by Inverse Compton.  \nFigures 2 and 3 show the energy spectra for proton and other elements, respectively. The Fig. 2 describes how the source contributes to the overall proton cosmic ray flux, considering three different spectral indices: 2.2 (see Fig. 2 - (a)), 2.4 (see Fig. 2 - (b)), and 2.6 (see Fig. 2 (c)). The spectra demonstrated in Fig. 3 follow a pattern similar to that of Fig. 2. However, as expected, the impact of the source on the spectra of heavier elements is significantly diminished as a result of the reduced flux of these particles. The presence of a Central Compact Object (CCO) associated with a supernova event could lead to the emission of charged and multi-messenger particles at low energy. However, we have no evidence of nucleus acceleration by CCO [25]. Figure 4 illustrates the impact of source on electron and positron emissions compared to measurements from various experiments, and the spin-down model once more gives a contribution at E > 10 6 eV.  \nThe B / C ratio against the kinetic energy per nucleon for our models compared to the CR data is shown in Fig. 5. Since there is only one region source, the purpose of this illustration was not to elucidate the data. Instead, its objective was to establish a comparison between the contributions of the emission models to gamma-ray emission. Moreover, it becomes apparent that the spin-down contribution is effective in contributing with data.The main result indicates that although the association between CCO 1E 1207.4-5209 and its host SNR G296.5+10.0 contributes to the low energy gamma-ray spectrum, it is inefficient in accelerating particles to high energies. Finally, we investigate the impact of the gas distribution on the total predicted gamma-ray intensity for the spin-down model in Figure 6. The impact of alternate gas maps on the spectrum is discussed in detail in [46]. The figures depict the intensity calculated at both 1 GeV and 1 TeV for electron emissions through inverse Compton and bremsstrahlung processes, utilizing the 3D gas model. The three-dimensional spatial density model for neutral and molecular hydrogen was developed based on gas linesurvey data [37]. There is an increase in intensity at 1 TeV for both inverse Compton and bremsstrahlung processes.', '5 Summary': 'In this study, we generated gamma-ray spectra from particles through simulations involving the association of the only pulsar with an inferred magnetic field, CCO 1E 1207.4-5209, and the supernova remnant G296.5 + 10.0. We considered two different emission scenarios at the source. Our findings are a direct result of energy particle propagation processes up to 10 14 eV, emphasizing the need to construct and assess propagation models to understand the physics of Galactic cosmic rays and the emission zone of sources inside our Galaxy. The spin-down model contributed to our findings and showed that this CCO 1E 1207.4-5209, with its measured magnetic field, can contribute to the spectrum of gamma rays only at low energy.  \nAnother outcome demonstrating the inefficiency of association in acceleration is that, even when using the upper limit of the energy integral range in GeV-TeV, the resulting model favored a low-luminosity scenario. The association does not significantly impact the particle spectrum. However, the limited source emission data currently available restrict us from drawing more comprehensive conclusions. In the future, Cherenkov Telescope Array Observatory (CTAO) measurements [see 54] will offer enhanced insights and opportunities for modeling emissions from this CCO and other low gamma emission sources.', 'Acknowledgments': "We thank the anonymous referee for providing valuable suggestions, which helped improve this work. This study was financed in part by the Coordena¸c˜ao de Aperfei¸coamento de Pessoal de N'ıvel Superior - Brasil (CAPES) - Finance Code 001. J.G.C. is grateful for the support of FAPES (1020/2022, 1081/2022, 976/2022, 332/2023) and CNPq (311758/2021-5). The research of R.C.A. is supported by Conselho Nacional de Desenvolvimento Cient'ıfico e Tecnol'ogico (CNPq), grant number 310448/2021-2. R.C.A. and L.N.P are grateful for the support of L'Oreal Brazil, with partnership of ABC and UNESCO in Brazil. The authors acknowledge the National Laboratory for Scientific Computing (LNCC/MCTI, Brazil) for providing HPC resources of the SDumont supercomputer, which have contributed to the research results reported in this paper. URL: http://sdumont.lncc.br. J.G.C and R.C.A acknowledge the financial support of FAPESP Project No. 2021/01089-1. The authors acknowledge the financial support of NAPI Fenˆomenos Extremos do Universo of Funda¸c˜ao de Apoio a Ciˆencia, Tecnologia e Inova¸c˜ao do Paran'a.", 'References': "- [1] M.G.F. Mayer and W. Becker, A kinematic study of central compact objects and their host supernova remnants , A&A 651 (2021) A40 [ 2106.00700 ].\n- [2] A.K. Harding, The neutron star zoo , Frontiers of Physics 8 (2013) 679 [ 1302.0869 ].\n- [3] A.M. Hillas, Where do 10 19 eV cosmic rays come from? , Nuclear Physics B Proceedings Supplements 136 (2004) 139.\n- [4] K.V. Ptitsyna and S.V. 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Bigongiari et al., Cosmic-Ray Boron Flux Measured from 8.4 GeV /n to 3.8 TeV /n with the Calorimetric Electron Telescope on the International Space Station , PRL 129 (2022) 251103 [ 2212.07873 ].  \nFigure 1 : Spectral Energy Distribution of gamma-ray emissions resulting from electrons/positrons in CCO 1E 1207.4-5209 and protons from its associated Supernova Remnant (SNR) G296.5 + 10.0. The model spin-down includes contributions from inverse Compton scattering, and bremsstrahlung. The data points featured in the plots are derived from the model developed by Zeng et al. in 2021 [21] and from gamma-ray measurements conducted by Araya in 2013 [53], focusing on the CCO+SNR association. See text for details. These models utilize a 2D gas distribution as described by Johannesson in 2018 [52].  \n<!-- image -->  \nFigure 2 : Energy spectra for proton from quiescent model. The spectra are multiplied by E 2 . The models calculations are shown in comparison with the data considering a modulation of 0.30 GV. The data have been extracted from [55-61].  \n<!-- image -->  \n8  \nFigure 3 : Energy spectra for four elements: helium, carbon, nitrogen and iron from quiescent model. The spectra are multiplied by E 2 . The models calculations are shown in comparison with the data considering spectral index of 2 . 4 and a modulation of 0.30 GV. The data have been extracted [62-66].  \n<!-- image -->  \nFigure 4 : Energy spectra for electron/positron from spin-down and quiescent models. The spectra are multiplied by E 2 . The models are shown in comparison with the data considering spectral index of 2 . 4 and a modulation of 0.30 GV. The data have been extracted AMS [55], ATIC [67], HESS [68], Fermi-LAT [69], DAMPE [70] and CALET [71].  \n<!-- image -->  \nFigure 5 : B/C ratio for the quiescent model as a function of kinetic energy per nucleon, displayed in comparison with data from [72, 73].  \n<!-- image -->  \nFigure 6 : Gamma-ray intensity at 1 GeV and 1 TeV from CCO 1E 1207.4-5209 and its host star SNR G296.5 + 10.0 for the spin-down model. The maps show the production of gamma rays by inverse Compton scattering - (a,b) and bremsstrahlung - (c,d). The maps are in Galactic coordinates with (l, b) = (0, 0) at the center of the map.  \n<!-- image -->"}