The Sun exhibits differential rotation, with its equator rotating faster than its poles, a phenomenon observed through helioseismology. The tachocline, located at approximately 0.7 solar radii, marks the boundary where the Sun transitions from differential to nearly rigid body rotation. The core of the Sun likely rotates at a different rate than the outer layers, and understanding these dynamics is crucial for studying stellar evolution, particularly in stars approaching supernova. The discussion highlights the importance of these rotational characteristics in understanding pulsar spins and the mechanisms behind them.
PREREQUISITESAstronomers, astrophysicists, and students interested in solar dynamics, stellar evolution, and the mechanisms behind pulsar spins will benefit from this discussion.
Chronos said:A curious thought. We know the sun rotates [spins]. Does it rotate like a solid body, or do the interior layers spin at different rates? If so, does the 'core' of a sun rotate faster or slower than the outer layers? Is it as difficult to calculate this as I suspect it might be? What would be the observational consequences?
My main interest is in the core spin of stars about to go supernova. Your comment is very insightful. I am wondering if stellar cores 'spin up' just before they detonate. I'm trying to figure out pulsar spins and looking for a mechanism that does not require recoil. Recoil does not seem to work because it appears to be mostly lateral, not tangential. Proper motion, especially in binary pairs, just do not seem to explain it. So I'm trying to come up with a reason.neurocomp2003 said:when you say "do layers rotate at different rates" are you talking about spherical shells, the different types of burning OR also convection?