Delta Scuti variableとは 意味・読み方・使い方

A Delta Scuti variable (sometimes termed dwarf cepheid) is a variable star which exhibits variations in its luminosity due to both radial and non-radial pulsations of the star's surface. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes in V over a period of a few hours, although the amplitude and period of the fluctuations can vary greatly. The stars are usually A0 to F5 type giant or main sequence stars. The high-amplitude Delta Scuti variables are also called AI Velorum stars. They are the second most abundant variable source in the Milky Way after white dwarfs. δ – Scuti stars exhibit both radial and non-radial luminosity pulsations. Non-radial pulsations are when parts of the surface move inwards and some move outwards at the same time. Radial pulsations are a special case when the star expands and contracts around it’s equilibrium state by altering the radius to maintain it’s spherical shape. The variations are due to the swelling and shrinking of the star through the Eddington Valve (or Kappa) Mechanism. The stars have a helium rich atmosphere. As helium is heated it becomes more ionised, which is more opaque. This is because helium only has two electrons, so when it becomes (singly or doubly) ionised either only (one or no) electrons remain in its shell to emit any light. So at the dimmest part in the cycle the star has highly ionised opaque helium in its atmosphere blocking part of the light from escaping. The energy from this “blocked light” causes the helium to heat up, expand, ionise, become more transparent and therefore allow more light through. As more light is let through the star appears brighter and, with the expansion, the helium begins to cool down. Hence the helium contracts and heats up again and the cyclical process continues. Throughout their lifetime Delta Scuti stars exhibit pulsation when they are situated on the classical Cepheid instability strip. They then move across from the main sequence into the giant branch.