Understanding the GD-1 Stellar Stream and Dark Matter
Author Information
Author(s): Zhang Xingyu, Yu Hai-Bo, Yang Daneng, Nadler Ethan O.
Primary Institution: Department of Physics, Tsinghua University, Beijing, People's Republic of China
Hypothesis
Can a core-collapsed self-interacting dark matter halo explain the high density of the GD-1 stellar stream perturber?
Conclusion
A core-collapsed self-interacting dark matter halo can account for the high density of the GD-1 stellar stream perturber.
Supporting Evidence
- The GD-1 stellar stream shows structures that suggest interactions with a dense substructure.
- Self-interacting dark matter models can lead to higher central densities than standard cold dark matter models.
- Simulations indicate that a self-interacting dark matter halo can evolve to match the properties of the GD-1 perturber.
Takeaway
The study shows that a special type of dark matter can create a dense region that affects the stars in a stream, helping us understand how dark matter works.
Methodology
High-resolution controlled N-body simulations were conducted to model the evolution of a self-interacting dark matter halo in the Milky Way's tidal field.
Potential Biases
Potential biases in density profile fitting due to resolution limits in simulations.
Limitations
Numerical artifacts may lead to underestimation of inner density profiles in simulations of core-collapsing halos.
Digital Object Identifier (DOI)
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