The kappa opacity mechanism is the driving mechanism behind the changes in luminosity of many types of pulsating variable stars. The term Eddington valve has been used for this mechanism, but this is increasingly obsolete.[1]
Here, the Greek letter kappa (κ) is used to indicate the radiative opacity at any particular depth of the stellar atmosphere. In a normal star, an increase in compression of the atmosphere causes an increase in temperature and density; this produces a decrease in the opacity of the atmosphere, allowing energy to escape more rapidly. The result is an equilibrium condition where temperature and pressure are maintained in a balance. However, in cases where the opacity increases with temperature, the atmosphere becomes unstable against pulsations.[2] If a layer of a stellar atmosphere moves inward, it becomes denser and more opaque, causing heat flow to be checked. In return, this heat increase causes a build-up of pressure that pushes the layer back out again. The result is a cyclic process as the layer repeatedly moves inward and then is forced back out again.[3]
Stellar non-adiabatic pulsation resulting from the κ–mechanism occurs in regions where hydrogen and helium are partly ionized, or where there are negative hydrogen ions. An example of such a zone is in RR Lyrae variables where the partial second ionization of helium occurs.[2] Hydrogen ionization is most likely the cause of pulsation activity in Mira variables, rapidly oscillating Ap stars (roAp) and ZZ Ceti variables. In Beta Cephei variables, stellar pulsations occur at a depth where the temperature reaches approximately 200,000 K and there is an abundance of iron. The increase in the opacity of iron at this depth is known as the Z bump, where Z is the astronomical symbol for elements other than hydrogen and helium.[4]
References
- ^ Tao, Louis; Spiegel, Edward; Umurhan, O. Matt (1998). "Stellar Oscillations". APS Division of Fluid Dynamics Meeting Abstracts: LC.10. Bibcode:1998APS..DFD..LC10T.
- ^ a b Maeder, André (2009). Physics, formation and evolution of rotating stars. Astronomy and astrophysics library. Springer. p. 373. ISBN 978-3-540-76948-4.
- ^ de Boer, Klaas Sjoerds; Seggewiss, Wilhelm (2008). Stars and stellar evolution. L'Editeur: EDP Sciences. p. 172. ISBN 978-2-7598-0356-9.
- ^ LeBlanc, Francis (2010). An Introduction to Stellar Astrophysics. John Wiley and Sons. p. 196. ISBN 978-0-470-69957-7.
Further reading
- Princeton lesson on radial pulsation,with kappa and epsilon mechanism
- Pulsating Stars: Stars that Breathe, Presentation of Swinburne University of Technology, 2010
- Cox, John P. (1963). "On Second Helium Ionization as a Cause of Pulsational Instability in Stars". The Astrophysical Journal. 138: 487. Bibcode:1963ApJ...138..487C. doi:10.1086/147661.
- Stein, R. F.; Cameron, A. G. W. (1966). "Stellar evolution". Bibcode:1966stev.conf.....S.
{{cite journal}}: Cite journal requires|journal=(help) - John P. Cox (1980). Theory of Stellar Pulsation. Princeton University Press. ISBN 978-0-691-08253-0.
- Andre Maeder (19 December 2008). Physics, Formation and Evolution of Rotating Stars. Springer Science & Business Media. ISBN 978-3-540-76949-1. In Fig. 15.8 at p.399 there is a schematic representation of the variations of V magnitude, radial velocity, radius with respect to the minimum radius and effective temperature of a classical Cepheid (δ Ceph) over one period.
This page was last edited on 5 January 2021, at 16:18