Beta Cephei

E538669

Beta Cephei is a class of hot, massive B-type pulsating variable stars whose brightness variations are driven by pressure and gravity mode oscillations.

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Statements (48)

Predicate Object
instanceOf B-type variable star
class of variable stars
pulsating variable star type
belongsToSpectralClass B-type
hasAbbreviation BCEP NERFINISHED
hasAlternativeName Beta Cep-type variable
Beta Cephei variable NERFINISHED
β Cep-type variable
β Cephei variable
hasDiscoveryCentury 20th century
hasEnvironment OB associations NERFINISHED
open clusters
young stellar populations
hasLightVariationCause non-radial pulsations
radial pulsations
hasPhotometricBandVariability optical
ultraviolet
hasPrototype Beta Cephei (star) NERFINISHED
hasPulsationDriver gravity mode oscillations
pressure mode oscillations
hasPulsationMechanism kappa mechanism
hasPulsationModes low-order g-modes
low-order p-modes
hasPulsationPeriodRange 0.1–0.6 days
hasTypicalAgeRange tens of millions of years
hasTypicalAmplitudeRange a few hundredths of a magnitude
hasTypicalEffectiveTemperatureRange 18,000–30,000 K
hasTypicalLocationInHRDiagram near the main-sequence turnoff of massive stars
hasTypicalLuminosityClass III
IV
V
hasTypicalMassRange 7–20 solar masses
hasTypicalMetallicity near-solar
hasTypicalRadialVelocityVariations tens of km/s
hasTypicalSpectralType B0
B1
B2
hasTypicalSurfaceGravity high
hasVariabilityTimescale short-period
hasVariabilityType pulsating
isCataloguedIn General Catalogue of Variable Stars NERFINISHED
isLocatedIn upper main sequence
isNamedAfter star Beta Cephei
isObservedIn Magellanic Clouds NERFINISHED
Milky Way NERFINISHED
isUsedFor asteroseismology of massive stars
studying internal structure of B-type stars
testing stellar opacity calculations

Referenced by (2)

Full triples — surface form annotated when it differs from this entity's canonical label.

Beta Crucis hasVariabilityType Beta Cephei
Mimosa hasVariabilityType Beta Cephei