Alternate Definitions for Delta Scuti variable stars

A member of a class of pulsating stars with periods less than 0.3 days, spectral types A or F, and visual light amplitudes in the range from a few thousands of a magnitude to about 0.8 mag. On the H-R diagram, δ Scuti stars form a group which lies in an instability strip which includes the classical Cepheids at its brightest end and the pulsating white dwarfs at its faintest limit. These stars can show very complex light variations since, while some of them are pulsating in one radial mode only, others may be pulsating simultaneously in several radial and non-radial modes.

A member of a class of pulsating stars with periods less than 0.3 days, spectral types A or F, and visual light amplitudes in the range from a few thousands of a magnitude to about 0.8 mag. On the H-R diagram, δ Scuti stars form a group which lies in an instability strip which includes the classical Cepheids at its brightest end and the pulsating white dwarfs at its faintest limit. These stars can show very complex light variations since, while some of them are pulsating in one radial mode only, others may be pulsating simultaneously in several radial and non-radial modes.

A member of a class of pulsating stars with periods less than 0.3 days, spectral types A or F, and visual light amplitudes in the range from a few thousands of a magnitude to about 0.8 mag. On the H-R diagram, δ Scuti stars form a group which lies in an instability strip which includes the classical Cepheids at its brightest end and the pulsating white dwarfs at its faintest limit. These stars can show very complex light variations since, while some of them are pulsating in one radial mode only, others may be pulsating simultaneously in several radial and non-radial modes.

A member of a class of pulsating stars with periods less than 0.3 days, spectral types A or F, and visual light amplitudes in the range from a few thousands of a magnitude to about 0.8 mag. On the H-R diagram, δ Scuti stars form a group which lies in an instability strip which includes the classical Cepheids at its brightest end and the pulsating white dwarfs at its faintest limit. These stars can show very complex light variations since, while some of them are pulsating in one radial mode only, others may be pulsating simultaneously in several radial and non-radial modes.