skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Possible evidence for the stochastic acceleration of secondary antiprotons by supernova remnants

Abstract

In this paper, the antiproton-to-proton ratio in the cosmic-ray spectrum is a sensitive probe of new physics. Using recent measurements of the cosmic-ray antiproton and proton fluxes in the energy range of 1–1000 GeV, we study the contribution to the $$\bar{p}$$/p ratio from secondary antiprotons that are produced and subsequently accelerated within individual supernova remnants. We consider several well-motivated models for cosmic-ray propagation in the interstellar medium and marginalize our results over the uncertainties related to the antiproton production cross section and the time-, charge-, and energy-dependent effects of solar modulation. We find that the increase in the $$\bar{p}$$/p ratio observed at rigidities above ~100 GV cannot be accounted for within the context of conventional cosmic-ray propagation models, but is consistent with scenarios in which cosmic-ray antiprotons are produced and subsequently accelerated by shocks within a given supernova remnant. In light of this, the acceleration of secondary cosmic rays in supernova remnants is predicted to substantially contribute to the cosmic-ray positron spectrum, accounting for a significant fraction of the observed positron excess.

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]
  1. The Johns Hopkins Univ., Baltimore, MD (United States)
  2. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, Chicago, IL (United States)
  3. The Ohio State Univ., Columbus, OH (United States)
Publication Date:
Research Org.:
Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
OSTI Identifier:
1345609
Alternate Identifier(s):
OSTI ID: 1363982
Report Number(s):
FERMILAB-PUB-17-010-A; arXiv:1701.04406
Journal ID: ISSN 2470-0010; PRVDAQ; 1509337
Grant/Contract Number:  
AC02-07CH11359; FG02-13ER41958; SC0009924
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 95; Journal Issue: 12; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS

Citation Formats

Cholis, Ilias, Hooper, Dan, and Linden, Tim. Possible evidence for the stochastic acceleration of secondary antiprotons by supernova remnants. United States: N. p., 2017. Web. doi:10.1103/PhysRevD.95.123007.
Cholis, Ilias, Hooper, Dan, & Linden, Tim. Possible evidence for the stochastic acceleration of secondary antiprotons by supernova remnants. United States. doi:10.1103/PhysRevD.95.123007.
Cholis, Ilias, Hooper, Dan, and Linden, Tim. Wed . "Possible evidence for the stochastic acceleration of secondary antiprotons by supernova remnants". United States. doi:10.1103/PhysRevD.95.123007. https://www.osti.gov/servlets/purl/1345609.
@article{osti_1345609,
title = {Possible evidence for the stochastic acceleration of secondary antiprotons by supernova remnants},
author = {Cholis, Ilias and Hooper, Dan and Linden, Tim},
abstractNote = {In this paper, the antiproton-to-proton ratio in the cosmic-ray spectrum is a sensitive probe of new physics. Using recent measurements of the cosmic-ray antiproton and proton fluxes in the energy range of 1–1000 GeV, we study the contribution to the $\bar{p}$/p ratio from secondary antiprotons that are produced and subsequently accelerated within individual supernova remnants. We consider several well-motivated models for cosmic-ray propagation in the interstellar medium and marginalize our results over the uncertainties related to the antiproton production cross section and the time-, charge-, and energy-dependent effects of solar modulation. We find that the increase in the $\bar{p}$/p ratio observed at rigidities above ~100 GV cannot be accounted for within the context of conventional cosmic-ray propagation models, but is consistent with scenarios in which cosmic-ray antiprotons are produced and subsequently accelerated by shocks within a given supernova remnant. In light of this, the acceleration of secondary cosmic rays in supernova remnants is predicted to substantially contribute to the cosmic-ray positron spectrum, accounting for a significant fraction of the observed positron excess.},
doi = {10.1103/PhysRevD.95.123007},
journal = {Physical Review D},
number = 12,
volume = 95,
place = {United States},
year = {Wed Jun 14 00:00:00 EDT 2017},
month = {Wed Jun 14 00:00:00 EDT 2017}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record

Citation Metrics:
Cited by: 8 works
Citation information provided by
Web of Science

Save / Share: