Solar-Like Cycle in Asymptotic Giant Branch Stars

Details Solar-Like Cycle in Asymptotic Giant Branch Stars Solar-Like Cycle in Asymptotic Giant Branch Stars

2000-01-16

arxiv.org/abs/astro-ph/0001281v1

Astronomy and Astrophysics

Astrophysics

10 pages, submitted to ApJ

Scientific paper

10.1086/309326

I propose that the mechanism behind the formation of concentric semi-periodic shells found in several planetary nebulae (PNs) and proto-PNs, and around one asymptotic giant branch (AGB) star, is a solar-like magnetic activity cycle in the progenitor AGB stars. The time intervals between consecutive ejection events is about 200-1,000 years, which is assumed to be the cycle period (the full magnetic cycle can be twice as long, as is the 22-year period in the sun). The magnetic field has no dynamical effects; it regulates the mass loss rate by the formation of magnetic cool spots. The enhanced magnetic activity at the cycle maximum results in more magnetic cool spots, which facilitate the formation of dust, hence increasing the mass loss rate. The strong magnetic activity implies that the AGB star is spun up by a companion, via a tidal or common envelope interaction. The strong interaction with a stellar companion explains the observations that the concentric semi-periodic shells are found mainly in bipolar PNs.

Affiliated with

Also associated with

No associations

Rating

Solar-Like Cycle in Asymptotic Giant Branch Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Solar-Like Cycle in Asymptotic Giant Branch Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Solar-Like Cycle in Asymptotic Giant Branch Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-17047