High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants
High-resolution X-ray spectroscopy of Galactic supernova remnants (SNRs), based on grating spectrometers onboard XMM-Newton and Chandra, has been revealing a variety of new astrophysical phenomena. Broadened oxygen lines for a northwestern compact knot in SN 1006 clearly show a high oxygen temperatu...
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| Language: | English |
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Czech Technical University in Prague
2014-12-01
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| Series: | Acta Polytechnica CTU Proceedings |
| Online Access: | https://ojs.cvut.cz/ojs/index.php/APP/article/view/2386 |
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| author | Satoru Katsuda Hiroshi Tsunemi |
| author_facet | Satoru Katsuda Hiroshi Tsunemi |
| author_sort | Satoru Katsuda |
| collection | DOAJ |
| description | High-resolution X-ray spectroscopy of Galactic supernova remnants (SNRs), based on grating spectrometers onboard XMM-Newton and Chandra, has been revealing a variety of new astrophysical phenomena. Broadened oxygen lines for a northwestern compact knot in SN 1006 clearly show a high oxygen temperature of ~300 keV. The high temperature together with a lower electron temperature (<em>kT<sub>e</sub></em> ~ 1 keV) can be reasonably interpreted as temperature non-equilibration between electrons and oxygen behind a collisionless shock. An ejecta knot in the Puppis A SNR shows blueshifted line emission by ~ 1500kms<sup>-1</sup>. The line widths are fairly narrow in contrast to the SN 1006's knot; an upper limit of 0.9 eV is obtained for O VIII Lyα, which translates to an oxygen temperature of <em>kT<sub>O</sub></em> < 30 keV. The low temperature suggests that the knot was heated by a reverse shock whose velocity is 4 times slower than that of a forward shock. Anomalous intensity ratios in O VII Heα lines, i.e., a stronger forbidden line than a resonance line, is found in a cloud-shock interaction region in Puppis A. The line ratio can be best explained by the charge-exchange emission that should arise at interfaces between the cold/warm clouds and the hot plasma. There are several other targets for which we plan to analyze high-quality grating data prior to the operation of the soft X-ray spectrometer onboard Astro-H. |
| format | Article |
| id | doaj-art-32a1d1aa8ffd4e06a48784188775381f |
| institution | Kabale University |
| issn | 2336-5382 |
| language | English |
| publishDate | 2014-12-01 |
| publisher | Czech Technical University in Prague |
| record_format | Article |
| series | Acta Polytechnica CTU Proceedings |
| spelling | doaj-art-32a1d1aa8ffd4e06a48784188775381f2025-08-20T03:33:02ZengCzech Technical University in PragueActa Polytechnica CTU Proceedings2336-53822014-12-011120020410.14311/APP.2014.01.02002198High-Resolution X-Ray Spectroscopy of Galactic Supernova RemnantsSatoru Katsuda0Hiroshi Tsunemi1RIKEN (The Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, Saitama 351-0198,Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka, 560-0043, JapanHigh-resolution X-ray spectroscopy of Galactic supernova remnants (SNRs), based on grating spectrometers onboard XMM-Newton and Chandra, has been revealing a variety of new astrophysical phenomena. Broadened oxygen lines for a northwestern compact knot in SN 1006 clearly show a high oxygen temperature of ~300 keV. The high temperature together with a lower electron temperature (<em>kT<sub>e</sub></em> ~ 1 keV) can be reasonably interpreted as temperature non-equilibration between electrons and oxygen behind a collisionless shock. An ejecta knot in the Puppis A SNR shows blueshifted line emission by ~ 1500kms<sup>-1</sup>. The line widths are fairly narrow in contrast to the SN 1006's knot; an upper limit of 0.9 eV is obtained for O VIII Lyα, which translates to an oxygen temperature of <em>kT<sub>O</sub></em> < 30 keV. The low temperature suggests that the knot was heated by a reverse shock whose velocity is 4 times slower than that of a forward shock. Anomalous intensity ratios in O VII Heα lines, i.e., a stronger forbidden line than a resonance line, is found in a cloud-shock interaction region in Puppis A. The line ratio can be best explained by the charge-exchange emission that should arise at interfaces between the cold/warm clouds and the hot plasma. There are several other targets for which we plan to analyze high-quality grating data prior to the operation of the soft X-ray spectrometer onboard Astro-H.https://ojs.cvut.cz/ojs/index.php/APP/article/view/2386 |
| spellingShingle | Satoru Katsuda Hiroshi Tsunemi High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants Acta Polytechnica CTU Proceedings |
| title | High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants |
| title_full | High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants |
| title_fullStr | High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants |
| title_full_unstemmed | High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants |
| title_short | High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants |
| title_sort | high resolution x ray spectroscopy of galactic supernova remnants |
| url | https://ojs.cvut.cz/ojs/index.php/APP/article/view/2386 |
| work_keys_str_mv | AT satorukatsuda highresolutionxrayspectroscopyofgalacticsupernovaremnants AT hiroshitsunemi highresolutionxrayspectroscopyofgalacticsupernovaremnants |