“Galaxy Merge”的版本间差异
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==Simulation== |
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* 'Identikit' software (Barnes & Hibbard 2009) : merge的状态 |
* 'Identikit' software (Barnes & Hibbard 2009) : merge的状态 |
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*星系的次并合对spin的影响不大，主并合又分两种情况[https://arxiv.org/abs/1703.00545]、 |
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:fast rotator : 质量较小的merge，气体较多，merge之后可以重新获得气体和恒星，从而获得spin |
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:slow rotator: 质量较大的merge，气体少，并合消耗spin，因而最终是slow rotator |
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*streams are a strong indication of nearly circular infall of a satellite (with a large angular momentum), whereas the appearance of shells clearly points to (nearly) radial satellite infall. [https://arxiv.org/pdf/1808.10454.pdf] |
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==mini-merge== |
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*质量比小于1:10 |
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*mini mergers can increase the size of the host disc significantly without changing the global shape of the galaxy, if the impact occurs along the disk plane, providing a possible explanation for extended low-surface brightness disks reported from observations [https://arxiv.org/pdf/1808.10454.pdf] |
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==galaxy pair== |
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*大星系周围的非常close的satellite计数 [http://adsabs.harvard.edu/abs/2014MNRAS.442..347R] |
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: If the satellites eventually infall into the host galaxies, the merger channel will be largely dominated by satellites with a mass ratio down to 1:10,(as these objects have 68 per cent of the total mass in satellites). |
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*HI轮廓的非对称性 arXiv:1907.09877 |
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*运动学上的非对称性，CALIFA的数据 [https://www.aanda.org/10.1051/0004-6361/201424935] |
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2019年7月24日 (三) 12:00的最新版本
Simulation
- 'Identikit' software (Barnes & Hibbard 2009) : merge的状态
- 星系的次并合对spin的影响不大，主并合又分两种情况[1]、
- fast rotator : 质量较小的merge，气体较多，merge之后可以重新获得气体和恒星，从而获得spin
- slow rotator: 质量较大的merge，气体少，并合消耗spin，因而最终是slow rotator
- streams are a strong indication of nearly circular infall of a satellite (with a large angular momentum), whereas the appearance of shells clearly points to (nearly) radial satellite infall. [2]
mini-merge
- 质量比小于1:10
- mini mergers can increase the size of the host disc significantly without changing the global shape of the galaxy, if the impact occurs along the disk plane, providing a possible explanation for extended low-surface brightness disks reported from observations [3]
galaxy pair
- 大星系周围的非常close的satellite计数 [4]
- If the satellites eventually infall into the host galaxies, the merger channel will be largely dominated by satellites with a mass ratio down to 1:10,(as these objects have 68 per cent of the total mass in satellites).
- HI轮廓的非对称性 arXiv:1907.09877
- 运动学上的非对称性，CALIFA的数据 [5]