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Can bars erode cuspy halos?

Published online by Cambridge University Press:  14 May 2020

Sandeep Kumar Kataria Open the ORCID record for Sandeep Kumar Kataria [Opens in a new window] ,
Mousumi Das  and
Stacy Mcgaugh
Sandeep Kumar Kataria
Affiliation:
Indian Institute of Astrophysics, Bangalore, 560034 and Indian Institute of Science, Bangalore, 560012, email: [email protected]
Mousumi Das
Affiliation:
Indian Institute of Astrophysics, Bangalore, 560034
Stacy Mcgaugh
Affiliation:
Department of Astronomy, Case Western Reserve University, Cleveland, OH44106, USA
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Abstract

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One of the major and widely known small scale problem with the Lambda CDM model of cosmology is the “core-cusp” problem. In this study we investigate whether this problem can be resolved using bar instabilities. We see that all the initial bars are thin (b/a < 0.3) in our simulations and the bar becomes thick ( b /a > 0.3) faster in the high resolution simulations. By increasing the resolution, we mean a larger number of disk particles. The thicker bars in the high resolution simulations transfer less angular momentum to the halo. Hence, we find that in the high resolution simulations it takes around 7 Gyr for the bar to remove inner dark matter cusp which is too long to be meaningful in galaxy evolution timescales. Physically, the reason is that as the resolution increases, the bar buckles faster and becomes thicker much earlier on.

Keywords

galaxies: kinematics and dynamics(cosmology:) dark mattermethods: n-body simulationsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 184 - 185
Copyright
© International Astronomical Union 2020

References

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