Published online by Cambridge University Press: 12 April 2016
Analysis of the radial velocity variation of θ Virginis A has revealed that, superposed on an orbital variation with a period of 17 years, there is present an ultrashort periodic variation of 0.15-day. This secondary cycle is attributed to pulsation. The question of what type of pulsating star θ Virginis A may represent is discussed.
El análisis de la variación de la velocidad radial de θ Virginis A ha revelado que superpuesta a la variación orbital de 17 años de periodo, existe un período de variación ultracorto de 0.15 días. Este ciclo secundario se atribuye a pulsaciones. Se discute el tipo de estrella pülstante que θ Virginis A puede ser.