For the S Doradus Instability Strip, see Luminous blue variable.
The unqualified term instability strip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating variable stars:[1] Delta Scuti variables, SX Phoenicis variables, and rapidly oscillating Ap stars (roAps) near the main sequence; RR Lyrae variables where it intersects the horizontal branch; and the Cepheid variables where it crosses the supergiants.
RV Tauri variables are also often considered to lie on the instability strip, occupying the area to the right of the brighter Cepheids (at lower temperatures), since their stellar pulsations are attributed to the same mechanism.
^Gautschy, A.; Saio, H. (1996). "Stellar Pulsations Across the HR Diagram: Part 2". Annual Review of Astronomy and Astrophysics. 34: 551–606. Bibcode:1996ARA&A..34..551G. doi:10.1146/annurev.astro.34.1.551.
The unqualified term instabilitystrip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating...
cross the instabilitystrip during a blue loop are thought to become W Virginis variables. More massive stars, crossing the instabilitystrip during a...
lie along a diagonal band in the H–R diagram called the S Doradus InstabilityStrip, with the more luminous examples having hotter temperatures. The standard...
hypergiants occupy a region of the Hertzsprung–Russell diagram above the instabilitystrip, a region where relatively few stars are found and where those stars...
composition. A nearly vertical region of the HR diagram, known as the instabilitystrip, is occupied by pulsating variable stars known as Cepheid variables...
secular redward (lower temperature) evolution across the Cepheid instabilitystrip, but it may be due to interference between the primary and the first-overtone...
yellow supergiants are in a region of the HR diagram known as the instabilitystrip because their temperatures and luminosities cause them to be dynamically...
can cause it to become a variable star. An example of this is the instabilitystrip, a region of the H-R diagram that includes Delta Scuti, RR Lyrae and...
luminosity over time due to instabilities within their interiors, but these are small except for two distinct instability regions where luminous blue...
star (IMS) first evolves away from the main sequence, it crosses the instabilitystrip very rapidly while the hydrogen shell is still burning. When the helium...
known periods range between 5 and 23 minutes. They lie in the δ Scuti instabilitystrip on the main sequence. The first roAp star to be discovered was HD...
unstable, leading to the instabilitystrip on the HR diagram where the majority of stars are pulsating variables. The instabilitystrip reaches from the main...
cluster has no stars in this region of its CMD. The gap occurs at the instabilitystrip, where many pulsating stars are found. These pulsating horizontal-branch...
stars are the RV Tauri variables, AGB or post-AGB stars lying on the instabilitystrip and showing distinctive semi-regular variations. Red supergiants develop...
types of variables amongst the supergiants are well defined. The instabilitystrip crosses the region of supergiants, and specifically many yellow supergiants...
dwarf binary system with a carbon-oxygen accretion disk. G 117-B15A Instabilitystrip Stellar pulsation Koester & Chanmugam 1990, p. 891–895. Murdin, Paul...
group consists of several kinds of pulsating stars, all found on the instabilitystrip, that swell and shrink very regularly caused by the star's own mass...
massive than the sun cross the Cepheid instabilitystrip, called the first crossing since they may cross the strip again later on a blue loop. In the 2...
region of the Hertzsprung–Russell diagram known as the S Doradus instabilitystrip, where the least luminous have a temperature around 10,000 K and a...
temperatures, some becoming unstable pulsating stars in the yellow instabilitystrip (RR Lyrae variables), whereas some become even hotter and can form...
O'Brien, M. S. (2000). "The Extent and Cause of the Pre–White Dwarf InstabilityStrip". The Astrophysical Journal. 532 (2): 1078–1088. arXiv:astro-ph/9910495...
Cardoso; Paolo Pani; Mariano Cadoni; Marco Cavaglia (2008). "Ergoregion instability of ultra-compact astrophysical objects". Physical Review D. 77 (12):...
Global Information