description LL Pegasi Overview
LL Pegasi is a carbon-rich star within a prominent spiral nebula. This young, protoplanetary nebula formed due to continuous mass ejection from a binary star system. The resulting structure, characterized by distinct dust rings, offers astronomers a unique opportunity to study the processes of stellar evolution and planetary formation around aging stars. It’s particularly relevant for research into binary star systems and the dynamics of nebular development.
insights Ranking position
LL Pegasi ranks #106 of 562 in the Nebula ranking, behind IC 4604, ahead of Sh2-129.
help LL Pegasi FAQ
Why does the nebula around LL Pegasi form a spiral?
LL Pegasi is losing material in a stellar wind while orbiting with a companion star. The orbital motion winds the expanding dust into a regularly spaced spiral, much like a rotating sprinkler pattern.
Is LL Pegasi the same object as AFGL 3068?
Yes, LL Pegasi is commonly identified with AFGL 3068. The latter designation is frequently used in astronomical discussions of its carbon-rich envelope and striking spiral.
Can the LL Pegasi spiral be seen with an amateur telescope?
The famous spiral was resolved in observations from the Hubble Space Telescope and is not a normal backyard visual target. Dust also obscures the central star at visible wavelengths, making infrared observations especially useful.
Will LL Pegasi become a planetary nebula?
LL Pegasi is an evolved carbon star shedding its outer layers late in the asymptotic giant branch phase. That expelled material may later be illuminated as a planetary nebula after the central star becomes much hotter.
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