http://202.127.29.3/~shen/wiki/index.php?action=history&feed=atom&title=%E6%98%9F%E7%B3%BB%E7%9A%84X-ray
星系的X-ray - 版本历史
2026-06-03T02:21:54Z
本wiki上该页面的版本历史
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2024年6月25日 (二) 07:47 Shen
2024-06-25T07:47:11Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2024年6月25日 (二) 07:47的版本</td>
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<td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
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<td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的<ins style="font-weight: bold; text-decoration: none;">[[热气体</ins>晕<ins style="font-weight: bold; text-decoration: none;">]]</ins>，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*只有4个大质量旋涡星系探测到X-ray的热气体晕，NGC1961，UGC12591，NGC6753，NGC266</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*只有4个大质量旋涡星系探测到X-ray的热气体晕，NGC1961，UGC12591，NGC6753，NGC266</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*在相对较低温度的CGM中，重原子没有完全电离，因此线辐射会更强</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*在相对较低温度的CGM中，重原子没有完全电离，因此线辐射会更强</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>:星系团中,如果温度很高，原子完全电离，就主要以热韧致辐射为主</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>:星系团中,如果温度很高，原子完全电离，就主要以热韧致辐射为主</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*https://arxiv.org/abs/2406.03254 X-ray-to-Hα ratio can help us to differentiate galaxies whose X-ray flux is dominated by an AGN {from galaxies with} central X-ray binaries and other stellar X-ray sources</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*https://arxiv.org/abs/2406.03254 X-ray-to-Hα ratio can help us to differentiate galaxies whose X-ray flux is dominated by an AGN {from galaxies with} central X-ray binaries and other stellar X-ray sources</div></td>
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Shen
http://202.127.29.3/~shen/wiki/index.php?title=%E6%98%9F%E7%B3%BB%E7%9A%84X-ray&diff=4066&oldid=prev
2024年6月6日 (四) 09:33 Shen
2024-06-06T09:33:42Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2024年6月6日 (四) 09:33的版本</td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*在相对较低温度的CGM中，重原子没有完全电离，因此线辐射会更强</div></td>
<td class="diff-marker"></td>
<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*在相对较低温度的CGM中，重原子没有完全电离，因此线辐射会更强</div></td>
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<td class="diff-marker"></td>
<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>:星系团中,如果温度很高，原子完全电离，就主要以热韧致辐射为主</div></td>
<td class="diff-marker"></td>
<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>:星系团中,如果温度很高，原子完全电离，就主要以热韧致辐射为主</div></td>
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<td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>*https://arxiv.org/abs/2406.03254 X-ray-to-Hα ratio can help us to differentiate galaxies whose X-ray flux is dominated by an AGN {from galaxies with} central X-ray binaries and other stellar X-ray sources</div></td>
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Shen
http://202.127.29.3/~shen/wiki/index.php?title=%E6%98%9F%E7%B3%BB%E7%9A%84X-ray&diff=3258&oldid=prev
2020年1月29日 (三) 08:28 Shen
2020-01-29T08:28:54Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2020年1月29日 (三) 08:28的版本</td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
<td class="diff-marker"></td>
<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*只有4个大质量旋涡星系探测到X-ray的热气体晕，NGC1961，UGC12591，NGC6753，NGC266</div></td>
<td class="diff-marker"></td>
<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*只有4个大质量旋涡星系探测到X-ray的热气体晕，NGC1961，UGC12591，NGC6753，NGC266</div></td>
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<td class="diff-marker" data-marker="+"></td>
<td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>*在相对较低温度的CGM中，重原子没有完全电离，因此线辐射会更强</div></td>
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<td class="diff-marker" data-marker="+"></td>
<td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>:星系团中,如果温度很高，原子完全电离，就主要以热韧致辐射为主</div></td>
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Shen
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2018年6月1日 (五) 02:56 Shen
2018-06-01T02:56:51Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2018年6月1日 (五) 02:56的版本</td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
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<td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div></td>
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Shen
http://202.127.29.3/~shen/wiki/index.php?title=%E6%98%9F%E7%B3%BB%E7%9A%84X-ray&diff=2229&oldid=prev
Shen：创建页面，内容为“*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]”
2016-04-08T07:55:11Z
<p>创建页面，内容为“*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]”</p>
<p><b>新页面</b></p><div>*大质量椭圆星系的X-ray的晕，是维里化的，Lx主要与T相关 参见 [https://arxiv.org/abs/1604.01764]</div>
Shen