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High-Resolution X-Ray Spectroscopy of Supernova Remnants

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High-Resolution X-ray Spectroscopy

Part of the book series: Springer Series in Astrophysics and Cosmology ((SSAC))

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Abstract

Thermal X-ray spectra from supernova remnants (SNRs) are dominated by a number of line emission from various elements. Resolving the individual lines is critically important for a variety of scientific topics such as diagnosing high-temperature and low-density non-equilibrium plasmas, identifying spectral features like charge exchange and resonance line scattering, revealing kinematics and elemental abundances of SN ejecta and the circumstellar medium, and studying the interstellar medium or planets’ atmospheres from extinction features seen in X-ray spectra of very bright SNRs. This chapter reviews high-resolution X-ray spectroscopy of SNRs obtained so far. Most results were derived with dispersive spectrometers aboard Einstein, Chandra, and XMM-Newton satellites. Because these dispersive spectrometers were slitless, one has to select small objects with angular sizes less than a few arcminutes to successfully perform high-resolution spectroscopy. Despite this limitation, the three satellites delivered fruitful scientific results in the last few decades. Arrays of low-temperature microcalorimeters offer excellent opportunities for high-resolution X-ray spectroscopy of SNRs, as they are non-dispersive spectrometers that work for largely extended sources as well as point-like sources. The microcalorimeter aboard the Hitomi satellite already delivered pioneering results during its short lifetime. The upcoming X-Ray Imaging and Spectroscopy Mission, which is a recovery mission of Hitomi, will truly open the new discovery window to high-resolution X-ray spectroscopy of SNRs.

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Change history

  • 05 November 2023

    A correction has been published.

Notes

  1. 1.

    Note that equation (3) in [81] should be better replaced to \(v_\textrm{fs} = (1-\gamma )/2 \times v_\textrm{sg} +(1+\gamma )/2 \times v_\textrm{ej}\) to take account of the motion of the unshocked ejecta knot. This change has no impact on the interpretation related to the reverse-shock scenario. I thank Pat Slane for pointing it out.

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Acknowledgements

I am grateful to Dr. Casey T. DeRoo and Dr. Takashi Okajima for their kind explanations on X-ray grating spectrometers and X-ray optics. I would also like to thank Dr. Hiroyuki Uchida for a long-term collaboration on high-resolution X-ray spectroscopy of SNRs and for providing me with the idea for Fig. 13.1. This work was supported by the Grants-in-Aid for Scientific Research from the Japanese Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan, No. JP20K20935, JP20H00174, and JP21H01121. I also deeply appreciate the Observational Astrophysics Institute at Saitama University for supporting the research fund.

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    Satoru Katsuda

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  2. Institute of Astronomy, University of Cambridge, Cambridge, UK

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Katsuda, S. (2023). High-Resolution X-Ray Spectroscopy of Supernova Remnants. In: Bambi, C., Jiang, J. (eds) High-Resolution X-ray Spectroscopy. Springer Series in Astrophysics and Cosmology. Springer, Singapore. https://doi.org/10.1007/978-981-99-4409-5_13

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