Discussion Overview
The discussion revolves around the gravitational dynamics at the center of spiral galaxies, particularly in relation to the concept of low pressure in vortex systems and its implications for gravity. Participants explore how these ideas might relate to supermassive black holes (SMBHs) and the behavior of matter in their vicinity.
Discussion Character
- Exploratory
- Debate/contested
- Technical explanation
Main Points Raised
- One participant suggests that if the center of a spiral galaxy behaves like a vortex with low pressure, an object at the center might experience zero net gravity due to equal forces from surrounding mass.
- Another participant counters that while a body at the center would not be pulled in any direction, the analogy to vortices is limited, as galaxies do not exhibit the same fluid dynamics.
- It is noted that only gas in a galaxy can be treated as a fluid, while stars and dark matter are considered collisionless, complicating the fluid model application.
- Participants discuss the necessity for objects to lose angular momentum to fall into a SMBH, mentioning three-body interactions and the formation of accretion disks as mechanisms for this process.
- There is a claim that angular momentum absorbed by a black hole increases its spin, but this is clarified to apply only to matter that actually falls into the black hole.
- One participant emphasizes that while matter may orbit the black hole due to angular momentum, it can eventually form an unstable accretion disk, leading to material falling into the SMBH.
Areas of Agreement / Disagreement
Participants express differing views on the applicability of fluid dynamics to galaxies and the implications for gravitational behavior at the centers of galaxies. There is no consensus on the validity of the vortex analogy or the mechanisms by which matter interacts with SMBHs.
Contextual Notes
Participants highlight limitations in applying fluid dynamics to galaxies, noting the collisionless nature of stars and dark matter. The discussion also reflects uncertainty regarding the stability of accretion disks and the processes involved in angular momentum transfer.