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Title: CHAMP cosmic rays

Abstract

In this work, we study interactions of cosmological relics, $X$, of mass $m$ and electric charge $qe$ in the galaxy, including thermalization with the interstellar medium, diffusion through inhomogeneous magnetic fields and Fermi acceleration by supernova shock waves. We find that for $$m \mathop{}_{\textstyle \sim}^{\textstyle <} 10^{10} q \; ~{\rm GeV}$$, there is a large flux of accelerated $X$ in the disk today, with a momentum distribution $$\propto 1/p^{2.5}$$ extending to $$(\beta p)_{max} \sim 5 \times10^4 q \; ~{\rm GeV}$$. Even though acceleration in supernova shocks is efficient, ejecting $X$ from the galaxy, $X$ are continually replenished by diffusion into the disk from the halo or confinement region. For $$m \mathop{}_{\textstyle \sim}^{\textstyle >} 10^{10} q \; ~{\rm GeV}$$, $X$ cannot be accelerated above the escape velocity within the lifetime of the shock. The accelerated $X$ form a component of cosmic rays that can easily reach underground detectors, as well as deposit energies above thresholds, enhancing signals in various experiments. Additionally, we find that nuclear/electron recoil experiments place very stringent bounds on $X$ at low $q$; for example, $X$ as dark matter is excluded for $q$ above $$10^{-9}$$ for any $m$. For larger $q$, stringent bounds on the fraction of dark matter that can be $X$ are set by Cherenkov and ionization detectors. Nevertheless, very small $q$ is highly motivated by the kinetic mixing portal, and we identify regions of $(m,q)$ that can be probed by future experiments.

Authors:
 [1];  [1];  [2]
  1. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  2. Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Inst. for Advanced Study, Princeton, NJ (United States)
Publication Date:
Research Org.:
Inst. for Advanced Study, Princeton, NJ (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25); USDOE Office of Science (SC), Nuclear Physics (NP) (SC-26); National Science Foundation (NSF)
OSTI Identifier:
1596293
Grant/Contract Number:  
[SC0009988; AC02-05CH11231; PHY-1316783; PHY-1521446]
Resource Type:
Accepted Manuscript
Journal Name:
Journal of Cosmology and Astroparticle Physics
Additional Journal Information:
[ Journal Volume: 2019; Journal Issue: 07]; Journal ID: ISSN 1475-7516
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Dunsky, David, Hall, Lawrence J., and Harigaya, Keisuke. CHAMP cosmic rays. United States: N. p., 2019. Web. doi:10.1088/1475-7516/2019/07/015.
Dunsky, David, Hall, Lawrence J., & Harigaya, Keisuke. CHAMP cosmic rays. United States. doi:10.1088/1475-7516/2019/07/015.
Dunsky, David, Hall, Lawrence J., and Harigaya, Keisuke. Wed . "CHAMP cosmic rays". United States. doi:10.1088/1475-7516/2019/07/015.
@article{osti_1596293,
title = {CHAMP cosmic rays},
author = {Dunsky, David and Hall, Lawrence J. and Harigaya, Keisuke},
abstractNote = {In this work, we study interactions of cosmological relics, $X$, of mass $m$ and electric charge $qe$ in the galaxy, including thermalization with the interstellar medium, diffusion through inhomogeneous magnetic fields and Fermi acceleration by supernova shock waves. We find that for $m \mathop{}_{\textstyle \sim}^{\textstyle <} 10^{10} q \; ~{\rm GeV}$, there is a large flux of accelerated $X$ in the disk today, with a momentum distribution $\propto 1/p^{2.5}$ extending to $(\beta p)_{max} \sim 5 \times10^4 q \; ~{\rm GeV}$. Even though acceleration in supernova shocks is efficient, ejecting $X$ from the galaxy, $X$ are continually replenished by diffusion into the disk from the halo or confinement region. For $m \mathop{}_{\textstyle \sim}^{\textstyle >} 10^{10} q \; ~{\rm GeV}$, $X$ cannot be accelerated above the escape velocity within the lifetime of the shock. The accelerated $X$ form a component of cosmic rays that can easily reach underground detectors, as well as deposit energies above thresholds, enhancing signals in various experiments. Additionally, we find that nuclear/electron recoil experiments place very stringent bounds on $X$ at low $q$; for example, $X$ as dark matter is excluded for $q$ above $10^{-9}$ for any $m$. For larger $q$, stringent bounds on the fraction of dark matter that can be $X$ are set by Cherenkov and ionization detectors. Nevertheless, very small $q$ is highly motivated by the kinetic mixing portal, and we identify regions of $(m,q)$ that can be probed by future experiments.},
doi = {10.1088/1475-7516/2019/07/015},
journal = {Journal of Cosmology and Astroparticle Physics},
number = [07],
volume = [2019],
place = {United States},
year = {2019},
month = {7}
}

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