Explore: Instability Strip (astrophysics)

The unqualified term instability strip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating

cross the instability strip during a blue loop are thought to become W Virginis variables. More massive stars, crossing the instability strip during a

lie along a diagonal band in the H–R diagram called the S Doradus Instability Strip, with the more luminous examples having hotter temperatures. The standard

yellow supergiants are in a region of the HR diagram known as the instability strip because their temperatures and luminosities cause them to be dynamically

in a section of the diagram called the instability strip. Cepheid variables also fall on the instability strip, at higher luminosities. The H-R diagram

composition. A nearly vertical region of the HR diagram, known as the instability strip, is occupied by pulsating variable stars known as Cepheid variables

for the hydrogen-free ejecta of pulsational pair-instability supernovae". Astronomy and Astrophysics. 640: A56. arXiv:2002.05077. Bibcode:2020A&A...640A

hypergiants occupy a region of the Hertzsprung–Russell diagram above the instability strip, a region where relatively few stars are found and where those stars

known periods range between 5 and 23 minutes. They lie in the δ Scuti instability strip on the main sequence. The first roAp star to be discovered was HD

star (IMS) first evolves away from the main sequence, it crosses the instability strip rapidly while the hydrogen shell is still burning. When the helium