YZ Boo

A Delta Scuti variable (sometimes termed dwarf cepheid) is a variable star (opens in a new tab) which exhibits variations in its luminosity (opens in a new tab) due to both radial and non-radial pulsations of the star’s surface. Typical brightness fluctuations are from 0.003 to 0.9 magnitudes (opens in a new tab) in V (opens in a new tab) over a period of a few hours, although the amplitude (opens in a new tab) and period (opens in a new tab) of the fluctuations can vary greatly. The stars are usually A0 to F5 type (opens in a new tab) giant (opens in a new tab) or main sequence (opens in a new tab) 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. The variability of period and amplitude of the high-amplitude δ Scuti star YZ Boo was thoroughly investigated by scientists based on a comprehensive analysis of new time-series photometry and other available data