Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

Kawanaka, Norita; Yanagita, S.

doi:10.1103/physrevlett.120.041103

Cited by 16 publications

(13 citation statements)

References 64 publications

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“…We note that a similar mechanism was proposed by Kawanaka & Yanagita (2018) albeit with rather extreme assumption that the spectral hardening observed above 300 GV is due to the local SN Ia. In this model most of the protons, He, and lithium above the break are coming from the local source.…”

Section: Lithium Anomalysupporting

confidence: 74%

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

Boschini

Torre

Gervasi

et al. 2020

ApJ

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Local interstellar spectra (LIS) of secondary cosmic ray (CR) nuclei, lithium, beryllium, boron, and partially secondary nitrogen, are derived in the rigidity range from 10 MV to ∼200 TV using the most recent experimental results combined with the state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. The lithium spectrum appears somewhat flatter at high energies compared to other secondary species that may imply a primary lithium component. Two propagation packages, GALPROP and HELMOD, are combined to provide a single framework that is run to reproduce direct measurements of CR species at different modulation levels, and at both polarities of the solar magnetic field. An iterative maximum-likelihood method is developed that uses GALPROP-predicted LIS as input to HELMOD, which provides the modulated spectra for specific time periods of the selected experiments for the model-data comparison. The proposed LIS accommodate the low-energy interstellar spectra measured by Voyager 1, HEAO-3, and ACE/CRIS as well as the high-energy observations by PAMELA, AMS-02, and earlier experiments that are made deep in the heliosphere. The interstellar and heliospheric propagation parameters derived in this study are consistent with our earlier results for propagation of CR protons, helium, carbon, oxygen, antiprotons, and electrons.

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Section: Lithium Anomalysupporting

confidence: 74%

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

Boschini

Torre

Gervasi

et al. 2020

ApJ

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“…cellent opportunity to study the hardening of the CR nuclei spectra quantitatively. Some previous works have proposed different solutions to this problem: (i) adding a new break in high-energy region (∼ 300 GV) to the injection spectra (see, e.g., Korsmeier & Cuoco (2016); Boschini et al (2017b); Niu et al ( , 2017; Zhu et al (2018)); (ii) adding a new in high-rigidity break to the diffusion coefficient (see, e.g., Génolini et al (2017)); (iii) inhomogeneous diffusion (see, e.g., Blasi et al (2012); Tomassetti (2012Tomassetti ( , 2015a; Feng et al (2016); Guo & Yuan (2018)); (iv) the superposition of local and distant sources (see, e.g., Vladimirov et al (2012); Bernard et al (2013); Thoudam & Hörandel (2013); Tomassetti & Donato (2015); Kachelrieß et al (2015); Kawanaka & Yanagita (2018)).…”

Section: Introductionmentioning

confidence: 99%

Bayesian Analysis of the Hardening in AMS-02 Nuclei Spectra

Niu

Xue

2019

ApJ

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Based on the precise nuclei data released by AMS-02, we study the spectra hardening of both the primary (proton, helium, carbon, oxygen, and the primary component of nitrogen) and the secondary (anti-proton, lithium, beryllium, boron and the secondary component of nitrogen) cosmic ray (CR) nuclei. With the diffusion-reacceleration model, we consider two schemes to reproduce the hardening in the spectra: (i) A high-rigidity break in primary source injection; (ii) A high-rigidity break in diffusion coefficient. The global fitting results show that both schemes could reproduce the spectra hardening in current status. More precise multi-TV data (especially the data of secondary CR species) is needed if one wants to distinguish these two schemes. In our global fitting, each of the nuclei species is allocated an independent solar modulation potential and a re-scale factor (which accounts for the isotopic abundance for primary nuclei species and uncertainties of production cross section or inhomogeneity of CR sources and propagation for secondary nuclei species). The fitting values of these two parameter classes show us some hints on some new directions in CR physics. All the fitted re-scale factors of primary nuclei species have values that systematically smaller than 1.0, while that of secondary nuclei species are systematically larger than 1.0. Moreover, both the re-scale factor and solar modulation potential of beryllium have values which are obviously different from other species. This might indicate that beryllium has the specificity not only on its propagation in the heliosphere, but also on its production cross section. All these new results should be seriously studied in the future.

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“…The finding of spectral hardening brings about various alternatives of the traditional CR theory. Most of them fall into, but not limited to, three categories: acceleration process (Ohira & Ioka 2011;Malkov et al 2012;Biermann et al 2010;Yuan et al 2011;Khiali et al 2017), transport effect Tomassetti 2012;Vladimirov et al 2012;Thoudam & Hörandel 2014;Evoli & Yan 2014;Aloisio et al 2015;Tomassetti 2015a;Guo et al 2015;Feng et al 2016;Guo et al 2016;Jin et al 2016;Guo & Yuan 2017, 2018, and nearby source (Bernard et al 2012;Thoudam & Hörandel 2012, 2013Bernard et al 2013;Liu et al 2015;Tomassetti & Donato 2015;Tomassetti 2015b;Liu et al 2017;Kawanaka & Yanagita 2018). One of the popular scenarios is so-called spatialdependent propagation (SDP) model.…”

Section: Introductionmentioning

confidence: 99%

Revisiting the Spatially Dependent Propagation Model with the Latest Observations of Cosmic-Ray Nuclei

Liu¹,

Yao

Guo³

2018

ApJ

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Recently AMS-02 collaboration publish their measurements of light cosmic-ray nuclei, including lithium, beryllium, boron, carbon and oxygen. All of them reveal a prominent excess above ∼ 200 GV, coinciding with proton and helium. Particularly, the secondary cosmic rays even harden than the primary components above that break. One of the viable interpretations for above anomalies is the spatial-dependent diffusion process. Such model has been successfully applied to multiple observational phenomena, for example primary cosmic ray nuclei, diffuse gamma ray and anisotropy. In this work, we investigate the spatial-dependent propagation model in light of the new observational data. We find that such model is able to explain the upturn of secondary spectrum as well as the primary's. All the spectra can be well reproduced and the calculated ratios are also in good agreement with the observations.

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Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

Cited by 16 publications

References 64 publications

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays

Bayesian Analysis of the Hardening in AMS-02 Nuclei Spectra

Revisiting the Spatially Dependent Propagation Model with the Latest Observations of Cosmic-Ray Nuclei

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