“AGN的反馈”的版本间差异
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（创建页面，内容为“*两种模式 *这两篇文章都说Outflow对恒星形成的抑制并不明显[http://arxiv.org/abs/1604.04577][http://arxiv.org/abs/1604.04290]”） |
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*两种模式 |
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*这两篇文章都说Outflow对恒星形成的抑制并不明显[http://arxiv.org/abs/1604.04577][http://arxiv.org/abs/1604.04290] |
*这两篇文章都说Outflow对恒星形成的抑制并不明显[http://arxiv.org/abs/1604.04577][http://arxiv.org/abs/1604.04290] |
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*射电源的年龄和[OIII]强度相关，反应了反馈的过程（ Our main conclusion is that the [OIII] gas is ∼3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at z<0.4. This changes to a factor of ∼2 at z>0.4.）[https://arxiv.org/abs/2407.06265] |
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2024年7月10日 (三) 01:39的最新版本
- 这两篇文章都说Outflow对恒星形成的抑制并不明显[1][2]
- 射电源的年龄和[OIII]强度相关，反应了反馈的过程（ Our main conclusion is that the [OIII] gas is ∼3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at z<0.4. This changes to a factor of ∼2 at z>0.4.）[3]