Draft version July 31, 2020 Typeset using L A T E X twocolumn style in AASTeX63 Changes in cosmic-ray transport properties connect the high-energy features in the electron and proton data O. Fornieri, 1, 2, 3 D. Gaggero, 3 D. Guberman, 2 L. Brahimi, 4 and A. Marcowith 4 1 Department of Physical Sciences, Earth and Environment, University of Siena, Italy 2 INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo 3, 56127 Pisa, Italy 3 Instituto de F´ ısica Te´ orica UAM-CSIC, Campus de Cantoblanco, E-28049 Madrid, Spain 4 Laboratoire Universe et Particules de Montpellier (LUPM) Un. Montpellier, CNRS IN2P3, CC72, place E. Bataillon, 34095, Montpellier Cedex 5, France Submitted to ApJL ABSTRACT In this Letter we simultaneously interpret the spectral feature at ∼ 10TeV in the cosmic-ray proton spectrum recently reported by the DAMPE Collaboration together with the spectral break at ∼ 1 TeV measured by H.E.S.S. in the lepton spectrum as signatures of one nearby hidden cosmic-ray accelerator. We show that this interpretation is consistent with the anisotropy data as long as the rigidity scaling of the diffusion coefficient features a hardening at ∼ 200 GV, as suggested by the light nuclear data measured with high accuracy by the AMS-02 Collaboration. The spectral feature is applied consistently to the large-scale diffuse cosmic-ray sea as well as to the particles injected by the source. 1. INTRODUCTION The past years have witnessed a remarkable increase in the accuracy of both hadronic and leptonic cosmic-ray (CR) data. This advance allowed to pinpoint spectral features in many different species at different energies, which offer a unique opportunity to shed light on the long-standing questions regarding the origin and trans- port of the non-thermal population of high-energy cos- mic particles in our Galaxy Gabici et al. (2019). In par- ticular, the AMS-02 Collaboration measured the fluxes of light nuclei and showed that the spectral index of several species progressively hardens at high rigidities (∼ 250 GeV), Aguilar et al. (2015a, 2016). However, the observed hardening in secondary hadronic species is twice as large as the one observed in primaries (Aguilar et al. (2018)), suggesting a diffusive origin for this fea- ture, as discussed for instance in G´ enolini et al. (2017). More recently, the DAMPE Collaboration has confirmed this feature in the high-energy CR proton spectra and reported a softening at 13.6 TeV, with the spectral index changing from 2.60 to 2.85 (An et al. (2019)). This spec- tral bump — independently measured by the ATIC and NUCLEON experiments — might be originated from a nearby Supernova Remnant (SNR). However, in order to reconcile this possibility with the current anisotropy data, an anomalous slow-diffusion zone around the rem- nant has been invoked in several recent analyses (Fang et al. (2020); Yuan et al. (2020)). In absence of such a high-confinement region, the predicted anisotropy would overshoot the observed data by more than one order of magnitude. On the other hand, in the lepton do- main, the H.E.S.S. (Aharonian et al. (2009); Kerszberg (2017)), CALET (Adriani et al. (2018)) and DAMPE (Ambrosi et al. (2017)) collaborations have consistently measured a spectral break at ∼ 1 TeV, possibly point- ing towards a nearby old remnant, as shown originally in Recchia et al. (2019) and later elaborated in a wider context in Fornieri et al. (2020). Moreover, attempts to assign the high-energy (E ≥ 1 TeV) observed leptons to known nearby sources — such as Vela and Cygnus Loop — using radio data have recently revealed their sub- dominant contributions (see for example Manconi et al. (2019)). In this paper, we propose a comprehensive scenario that correctly reproduces all these spectral features. The idea is that a nearby old Supernova Remnant is responsible for both the hadronic bump measured by DAMPE/NUCLEON/ATIC and the leptonic break re- ported by H.E.S.S. To do this, we consider a transport scenario featur- ing a rigidity scaling that progressively hardens, as sug- gested by AMS-02 light nuclei data, and show that — within such transport scenario — the anisotropy con- straints are satisfied. arXiv:2007.15321v1 [astro-ph.HE] 30 Jul 2020