Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter
Abstract
Self-interacting dark matter offers 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 introduce 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 |$$10{{\ \rm per\ cent}}$$| ; (iv) inject the energy equivalent of |$$\mathcal {O}(100)$$| 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 ~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.
- Authors:
-
- Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- Center for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland
- Berkeley Center for Theoretical Physics, University of California, Berkeley, CA 94720, USA
- Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA, Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- Publication Date:
- Research Org.:
- Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP); Hertz Foundation; National Science Foundation (NSF); Icelandic Research Fund; Kavli Research Investment Fund
- OSTI Identifier:
- 1494943
- Alternate Identifier(s):
- OSTI ID: 1596615
- Report Number(s):
- MIT-CTP-5014
Journal ID: ISSN 0035-8711
- Grant/Contract Number:
- SC0013999; SC00012567
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 484 Journal Issue: 4; Journal ID: ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; methods: numerical; galaxies: haloes; dark matter
Citation Formats
Vogelsberger, Mark, Zavala, Jesús, Schutz, Katelin, and Slatyer, Tracy R. Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter. United Kingdom: N. p., 2019.
Web. doi:10.1093/mnras/stz340.
Vogelsberger, Mark, Zavala, Jesús, Schutz, Katelin, & Slatyer, Tracy R. Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter. United Kingdom. https://doi.org/10.1093/mnras/stz340
Vogelsberger, Mark, Zavala, Jesús, Schutz, Katelin, and Slatyer, Tracy R. Wed .
"Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter". United Kingdom. https://doi.org/10.1093/mnras/stz340.
@article{osti_1494943,
title = {Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter},
author = {Vogelsberger, Mark and Zavala, Jesús and Schutz, Katelin and Slatyer, Tracy R.},
abstractNote = {Self-interacting dark matter offers 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 introduce 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 |$10{{\ \rm per\ cent}}$| ; (iv) inject the energy equivalent of |$\mathcal {O}(100)$| 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 ~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.},
doi = {10.1093/mnras/stz340},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 4,
volume = 484,
place = {United Kingdom},
year = {2019},
month = {2}
}
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