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:
-
- Univ. of California, Berkeley, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
- 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.:
- Institute for Advanced Study, Princeton, NJ (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP); USDOE Office of Science (SC), Nuclear Physics (NP); 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. https://doi.org/10.1088/1475-7516/2019/07/015
Dunsky, David, Hall, Lawrence J., and Harigaya, Keisuke. Wed .
"CHAMP cosmic rays". United States. https://doi.org/10.1088/1475-7516/2019/07/015. https://www.osti.gov/servlets/purl/1596293.
@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 = {Wed Jul 10 00:00:00 EDT 2019},
month = {Wed Jul 10 00:00:00 EDT 2019}
}
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Figures / Tables:
FIG. 1: Shaded regions indicate the parameter space where CHAMPs fall into disks with baryons at a halo collapse redshift $z$vir, determined by setting $t$therm($z$vir) <$ t$coll($z$vir). Pre-reionization (left), the ion fraction is low and thermalization between X and the plasma is difficult. Post-reionization (right) the ion fraction is highmore »
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