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

Title: Constraining Dissipative Dark Matter Self-Interactions

Abstract

We study the gravothermal evolution of dark matter halos in the presence of dissipative dark matter self-interactions. Dissipative interactions are present in many particle-physics realizations of the dark-sector paradigm and can significantly accelerate the gravothermal collapse of halos compared to purely elastic dark matter self-interactions. This is the case even when the dissipative interaction timescale is longer than the free-fall time of the halo. Using a semianalytical fluid model calibrated with isolated and cosmological $N$-body simulations, we calculate the evolution of the halo properties -- including its density profile and velocity dispersion profile -- as well as the core-collapse time as a function of the particle model parameters that describe the interactions. A key property is that the inner density profile at late times becomes cuspy again. Using 18 dwarf galaxies that exhibit a corelike dark matter density profile, we derive constraints on the strength of the dissipative interactions and the energy loss per collision.

Authors:
 [1];  [2];  [3]; ORCiD logo [4]
  1. YITP, Stony Brook
  2. Fermilab
  3. UC, Riverside
  4. Boston U.
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:
1562565
Alternate Identifier(s):
OSTI ID: 1497096
Report Number(s):
arXiv:1809.01144; FERMILAB-PUB-18-437-A
oai:inspirehep.net:1692779
Grant/Contract Number:  
AC02-07CH11359; SC0017938; SC0008541; SC0015845
Resource Type:
Published Article
Journal Name:
Phys.Rev.Lett.
Additional Journal Information:
Journal Volume: 123; Journal Issue: 12
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS

Citation Formats

Essig, Rouven, Mcdermott, Samuel D., Yu, Hai-Bo, and Zhong, Yi-Ming. Constraining Dissipative Dark Matter Self-Interactions. United States: N. p., 2019. Web. doi:10.1103/PhysRevLett.123.121102.
Essig, Rouven, Mcdermott, Samuel D., Yu, Hai-Bo, & Zhong, Yi-Ming. Constraining Dissipative Dark Matter Self-Interactions. United States. doi:10.1103/PhysRevLett.123.121102.
Essig, Rouven, Mcdermott, Samuel D., Yu, Hai-Bo, and Zhong, Yi-Ming. Thu . "Constraining Dissipative Dark Matter Self-Interactions". United States. doi:10.1103/PhysRevLett.123.121102.
@article{osti_1562565,
title = {Constraining Dissipative Dark Matter Self-Interactions},
author = {Essig, Rouven and Mcdermott, Samuel D. and Yu, Hai-Bo and Zhong, Yi-Ming},
abstractNote = {We study the gravothermal evolution of dark matter halos in the presence of dissipative dark matter self-interactions. Dissipative interactions are present in many particle-physics realizations of the dark-sector paradigm and can significantly accelerate the gravothermal collapse of halos compared to purely elastic dark matter self-interactions. This is the case even when the dissipative interaction timescale is longer than the free-fall time of the halo. Using a semianalytical fluid model calibrated with isolated and cosmological $N$-body simulations, we calculate the evolution of the halo properties -- including its density profile and velocity dispersion profile -- as well as the core-collapse time as a function of the particle model parameters that describe the interactions. A key property is that the inner density profile at late times becomes cuspy again. Using 18 dwarf galaxies that exhibit a corelike dark matter density profile, we derive constraints on the strength of the dissipative interactions and the energy loss per collision.},
doi = {10.1103/PhysRevLett.123.121102},
journal = {Phys.Rev.Lett.},
number = 12,
volume = 123,
place = {United States},
year = {2019},
month = {9}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: 10.1103/PhysRevLett.123.121102

Save / Share: