期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 484, 期 4, 页码 5437-5452出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz340
关键词
methods: numerical; galaxies: haloes; dark matter
资金
- MIT RSC award
- Kavli Research Investment Fund
- NASA ATP grant [NNX17AG29G]
- NSF [AST-1814053, AST-1814259]
- Grant of Excellence from the Icelandic Research Fund [173929 - 051]
- Office of High Energy Physics of the U.S. Department of Energy [DE-SC00012567, DE-SC0013999]
- Hertz Foundation Fellowship
- National Science Foundation Graduate Research Fellowship
Self-interacting dark matter provides a promising alternative for the cold dark matter paradigm to solve potential small-scale galaxy formation problems. Nearly all self-interacting dark matter simulations so far have considered only elastic collisions. Here we present simulations of a galactic halo within a generic inelastic model using a novel numerical implementation in the AREPO code to study arbitrary multistate inelastic dark matter scenarios. For this model we find that inelastic self-interactions can: (i) create larger subhalo density cores compared to elastic models for the same cross-section normalization; (ii) lower the abundance of satellites without the need for a power spectrum cut-off; (iii) reduce the total halo mass by about 10 per cent; (iv) inject the energy equivalent of O(100) million Type II supernovae in galactic haloes through level de-excitation; (v) avoid the gravothermal catastrophe due to removal of particles from halo centres. We conclude that a similar to 5 times larger elastic cross-section is required to achieve the same central density reduction as the inelastic model. This implies that well-established constraints on self-interacting cross-sections have to be revised if inelastic collisions are the dominant mode. In this case significantly smaller cross-sections can achieve the same core density reduction thereby increasing the parameter space of allowed models considerably.
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