Dark matter and dark radiation

By Lotty Ackerman, Matthew R. Buckley, S. Carroll, M. Kamionkowski. 2008

356 citations recorded by the source corpus.

We explore the feasibility and astrophysical consequences of a new long-range U(1) gauge field ("dark electromagnetism") that couples only to dark matter, not to the Standard Model. The dark matter consists of an equal number of positive and negative charges under the new force, but annihilations are suppressed if the dark matter mass is sufficiently high and the dark fine-structure constant α is sufficiently small. The correct relic abundance can be obtained if the dark matter also couples to the conventional weak interactions, and we verify that this is consistent with particle-physics constraints. The primary limit on a comes from the demand that the dark matter be effectively collisionless in galactic dynamics, which implies α ≾ 10^(-3) for TeV-scale dark matter. These values are easily compatible with constraints from structure formation and primordial nucleosynthesis. We raise the prospect of interesting new plasma effects in dark matter dynamics, which remain to be explored. This proceedings is based on the work presented originally in.(1)

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/53c2df4a5b6cc6e4dcd9e9f6641dbc4c1b210a9d

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Citations in the corpus

Superradiance (2015, background): “For example, massive vector fields (“dark photons” [432, 433]) arise in the so-called hidden U(1) sector [434, 435, 436, 437, 438].”
What does the Bullet Cluster tell us about Self-Interacting Dark Matter? (2016, background): “Velocity-dependent cross-sections can arise naturally in models for SIDM (Ackerman et al. 2009; Buckley & Fox 2010; Loeb & Weiner 2011; van den Aarssen, Bringmann & Pfrommer 2012; Tulin, Yu & Zurek 2013a), and constraining such models requires a handle on the cross-section at different velocity…”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, background): “New light particles may arise in the form of axions and sterile neutrinos, or can appear as a byproduct of new symmteries that would explain the small mass of the Higgs boson [142, 143, 144, 145, 146, 147, 148, 10, 149, 150, 151, 152, 11, 153, 154, 141, 155, 12, 156, 157, 158, 159].”
Colliding clusters and dark matter self-interactions (2013, background): “Typical parameters of interest are α′ = 10−2 for mDM = 1 TeV (Ackerman et al. 2009).”
Constraining self-interacting dark matter with the Milky Way’s dwarf spheroidals (2012, background): “…proposed (Yoshida et al. 2000) and explored with cosmological simulations (Colı́n et al. 2002) a decade ago, its theoretical support has come up only recently (e.g. Ackerman et al. 2009; Feng et al. 2009, 2010; Buckley & Fox 2010; Loeb & Weiner 2011; van den Aarssen et al. 2012; Tulin et al. 2012).”
Search for New Physics with Atoms and Molecules (2017, background): “A closely related hypothesis is that of the dark photon, which would communicate a “dark” electromagnetic interaction between dark matter particles, and could be detectable via mixing with photons (Ackerman et al., 2009).”
New physics in light of the H0 tension: An alternative view (2019, unknown): “[248–266] for examples of such models.”
Gravitational probes of dark matter physics (2017, background): “Such deviations can occur if the SIDM model contains a relatively light force carrier, such as the dark photon discussed in the previous section [37, 192, 193, 39] or dark pion from a confining sector [194].”
Double-Disk Dark Matter (2013, background): “[16] and [17], which find that because of the low-velocity enhancement of Rutherford scattering the bounds exclude a thermal relic abundance.”
The Dark Photon (2020, background): “…for the galaxy NGC720, according to 2 The literature on the subject is already very extensive, see, for example, (van den Aarssen et al., 2012; Ackerman et al., 2009; Agrawal et al., 2017; Arkani-Hamed et al., 2009; Baldi, 2013; Boddy et al., 2014; Buckley and Fox, 2010; Buen-Abad et al.,…”
Hidden charged dark matter (2009, background): “It is therefore also critical to investigate whether this scenario is consistent with constraints on self-interacting dark matter from the Bullet Cluster [33], observed ellipticity of dark matter halos [34] and bounds from considerations of galactic dynamics [19].”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “…et al. 1993; de Laix et al. 1995; Spergel & Steinhardt 2000; Firmani et al. 2000), and are now recognized as generic consequences of hidden-sector extensions to the Standard Model (Pospelov et al. 2008; Arkani-Hamed et al. 2009; Ackerman et al. 2009; Feng et al. 2009, 2010; Loeb & Weiner 2011).”