A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

Gurian, James; Ryan, Michael P.; Schon, Sarah; Jeong, Donghui; Shandera, Sarah

doi:10.3847/2041-8213/ac997c

Cited by 16 publications

(9 citation statements)

References 49 publications

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“…The ADM, when present, constitutes 6% of the total DM, with its cooling physics determined by its fine-structure constant (a¢), proton mass ( ¢ m p ), electron mass ( ¢ m e ), and dark CMB temperature locally self-gravitating and Jeans-unstable are turned into "clump" particles over the freefall timescale. These dense clumps are expected to collapse in a runaway fashion into compact objects that effectively behave as collisionless particles at the resolved scale of the simulations; see, e.g., Gurian et al (2022b). The clump formation criteria for ADM gas are different from the ones used for stellar particles because baryons have further constraints on molecular gas fractions and a set density threshold.…”

Section: Simulationsmentioning

confidence: 99%

Simulating Atomic Dark Matter in Milky Way Analogs

Roy,

Shen,

Lisanti

et al. 2023

ApJL

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Dark sector theories naturally lead to multicomponent scenarios for dark matter where a subcomponent can dissipate energy through self-interactions, allowing it to efficiently cool inside galaxies. We present the first cosmological hydrodynamical simulations of Milky Way analogs where the majority of dark matter is collisionless cold dark matter (CDM) but a subcomponent (6%) is strongly dissipative minimal atomic dark matter (ADM). The simulations, implemented in GIZMO and utilizing FIRE-2 galaxy formation physics to model the standard baryonic sector, demonstrate that the addition of even a small fraction of dissipative dark matter can significantly impact galactic evolution despite being consistent with current cosmological constraints. We show that ADM gas with roughly standard model–like masses and couplings can cool to form a rotating “dark disk” with angular momentum closely aligned with the visible stellar disk. The morphology of the disk depends sensitively on the parameters of the ADM model, which affect the cooling rates in the dark sector. The majority of the ADM gas gravitationally collapses into dark “clumps” (regions of black hole or mirror star formation), which form a prominent bulge and a rotating thick disk in the central galaxy. These clumps form early and quickly sink to the inner ∼kiloparsec of the galaxy, affecting the galaxy’s star formation history and present-day baryonic and CDM distributions.

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Section: Simulationsmentioning

confidence: 99%

Simulating Atomic Dark Matter in Milky Way Analogs

Roy,

Shen,

Lisanti

et al. 2023

ApJL

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“…Another possible application is to the study of dissipative dark matter, which can itself cool to eventually form compact objects (Shandera et al 2018;Gurian et al 2022;Hippert et al 2022;Ryan & Radice 2022). These objects could have masses and compactnesses impossible under ordinary stellar astrophysics, leading to distinctive gravitational wave signatures.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Zero Metallicity with Zero CPU Hours: Masses of the First Stars on the Laptop

Gurian,

Jeong,

Liu

2024

ApJ

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We develop an analytic model for the mass of the first stars forming in the centers of primordial gas clouds as a function of host halo mass, redshift, and degree of rotation. The model is based on the estimation of key timescales determining the following three processes: the collapse of the gas cloud, the accretion onto the protostellar core, and the radiative feedback of the protostellar core. The final stellar mass is determined by the total mass accreted until the radiative feedback halts the accretion. The analytic estimation, motivated by the result of the full numerical simulations, leads to algebraic expressions allowing an extremely fast execution. Despite its simplicity, the model reproduces the stellar mass scale and its parameter dependencies observed in state-of-the-art cosmological zoom-in simulations. This work clarifies the basic physical principles undergirding such numerical treatments and provides a path to efficiently calibrating numerical predictions against eventual observations of the first stars.

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“…Atomic dark matter and the associated phenomenology has been explored extensively [7,. Dark stars as well as dark compact objects such as dark white dwarfs and dark neutron stars have been considered in [65][66][67][68][69][70][71][72].…”

Section: Jcap01(2024)064 2 Atomic Dark Mattermentioning

confidence: 99%

Dark black holes in the mass gap

Fernandez,

Ghalsasi,

Profumo

et al. 2024

J. Cosmol. Astropart. Phys.

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In the standard picture of stellar evolution, pair-instability — the energy loss in stellar cores due to electron-positron pair production — is predicted to prevent the collapse of massive stars into black holes with mass in the range between approximately 50 and 130 solar masses — a range known as the “black hole mass gap”. LIGO and Virgo detection of black hole binary mergers containing one or both black holes with masses in this mass gap thus challenges the standard picture, possibly pointing to an unexpected merger history, unanticipated or poorly understood astrophysical mechanisms, or new physics. Here, we entertain the possibility that a “dark sector” exists, consisting of dark electrons, dark protons, and electromagnetic-like interactions, but no nuclear forces. Dark stars would inevitably form given such dark sector constituents, possibly collapsing into black holes with masses within the mass gap. We study in detail the cooling processes necessary for successful stellar collapse in the dark sector and show that for suitable choices of the particle masses, we indeed predict populating the mass gap with dark sector black holes. In particular, we numerically find that the heavier of the two dark sector massive particles cannot be lighter than, approximately, the visible sector proton for the resulting dark sector black holes to have masses within the mass gap. We discuss constraints on this scenario and how to test it with future, larger black hole merger statistics.

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A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter

Cited by 16 publications

References 49 publications

Simulating Atomic Dark Matter in Milky Way Analogs

Simulating Atomic Dark Matter in Milky Way Analogs

Zero Metallicity with Zero CPU Hours: Masses of the First Stars on the Laptop

Dark black holes in the mass gap

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