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Table · dataset · 2006

Radial velocity of gamma Pegasi

Listed in IVOA Registry (Virtual Observatory)

High resolution and high signal to noise ratio spectroscopic observations of the classical {beta} Cephei star {gamma} Peg were obtained between 1991 and 2005.

Description

The analysis of these data combined with previously published results shows that {gamma} Peg is a spectroscopic binary with an orbital period of 370.5d. We discovered three new frequencies in addition to the well-known 6.5897d^-1^ (0.15175d) one.

That at 6.01d^-1^ is a typical Cephei frequency. The two others at 0.68 and 0.87d^-1^ are similar to the high degree g-mode frequencies found in SPB stars. Thus, {gamma} Peg is a hybrid {beta} Cephei-SPB star.

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Its position in the HR diagram is compatible with such a status. In addition, a small increase of the main period has been detected between the 1995 and 2005 observations.

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Documentation and papers

Catalogue records · 2

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Stated by source
Optical
Provenance · 1 source records, 8 field assertions
SourceKeyLast seenRaw
IVOA Registry (Virtual Observatory)ivo://cds.vizier/j/a+a/448/69714 d agoJSON v1
FieldAssertionExtractorEvidence
access_levelsource · IVOA Registryconnector:ivoa_registry@1.0.0
concepts[field].local:field:astronomymapping · IVOA Registryconnector:ivoa_registry@1.0.0
concepts[modality].ivoa_waveband:opticalsource · IVOA Registryconnector:ivoa_registry@1.0.0
descriptionsource · IVOA Registryconnector:ivoa_registry@1.0.0rr.resource.res_description
license_textsource · IVOA Registryconnector:ivoa_registry@1.0.0
publication_datesource · IVOA Registryconnector:ivoa_registry@1.0.0
titlesource · IVOA Registryconnector:ivoa_registry@1.0.0rr.resource.res_title
updated_datesource · IVOA Registryconnector:ivoa_registry@1.0.0