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- A. C. Fabian
- 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
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- S. A. Walker
- 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
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- H. R. Russell
- 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
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- C. Pinto
- 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
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- J. S. Sanders
- 2Max-Planck-Institut für Extraterrestrische Physik, Giessenbackstrasse 1, D-85748 Garching, Germany
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- C. S. Reynolds
- 3Department of Astronomy, University of Maryland, College Park, MD 20712-2421, USA
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説明
<jats:title>Abstract</jats:title> <jats:p>The level of random motions in the intracluster gas lying between 20 and 60 kpc radius in the core of the Perseus cluster has been measured by the Hitomi Soft X-ray Spectrometer (SXS) at 164 ± 10 km s−1. The maximum energy density in turbulent motions on that scale is therefore low. If dissipated as heat, the turbulent energy will be radiated away in less than 80 Myr and cannot spread across the core. A higher velocity is needed to prevent a cooling collapse. Gravity waves are shown to travel too slowly in a radial direction. Here we investigate propagation of energy by sound waves. The energy travels at ∼ 1000 km s−1 and can cross the core in a cooling time. We show that the displacement velocity amplitude of the gas required to carry the power is consistent with the Hitomi result and that the inferred density and temperature variations are consistent with Chandra observations.</jats:p>
収録刊行物
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- Monthly Notices of the Royal Astronomical Society: Letters
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Monthly Notices of the Royal Astronomical Society: Letters 464 (1), L1-L5, 2016-08-30
Oxford University Press (OUP)
