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A Possible Intracluster Origin for the Excess Soft X-ray Component in Some Clusters
1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK.
Science (New York, N.Y.)
|January 3, 1997
Summary
The soft X-ray spectra of galaxy clusters suggest excess emission not explained by standard models. A turbulent mixing layer model offers a potential solution for this excess soft emission in galaxy clusters.
Area of Science:
- Astronomy and Astrophysics
- Plasma Physics
Background:
- Galaxy clusters emit X-rays from hot intracluster medium.
- Observed soft X-ray spectra of Virgo and Coma clusters deviate from standard models.
- Photoelectric absorption in our galaxy does not fully account for the observed spectra.
Purpose of the Study:
- Investigate the source of excess soft X-ray emission from galaxy clusters.
- Explain discrepancies between observed spectra and models of hot intracluster medium.
- Propose a new model to account for the observed soft X-ray excess.
Main Methods:
- Analysis of soft X-ray spectra from Virgo and Coma galaxy clusters.
- Comparison of observed spectra with models of hot intracluster medium and photoelectric absorption.
- Development and evaluation of a turbulent mixing layer model.
Main Results:
- Standard models fail to explain the soft X-ray spectra of galaxy clusters.
- Excess soft emission suggests thermal emission from cooler gas (approx. 1 million K).
- Rapid cooling of this gas presents challenges for its origin and fate.
Conclusions:
- A turbulent mixing layer model may explain the excess soft X-ray emission.
- This model proposes gas reheating after cooling, maintaining a small total mass.
- The model offers a potential solution to the cooling gas problem in galaxy clusters.