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<ri:Resource created="2023-07-26T08:44:42Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>TESS A and B stars and the Maia variables</title><shortName>J/MNRAS/493/5871</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/493/5871</identifier><altIdentifier>doi:10.26093/cds/vizier.74935871</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Balona L.A.</name></creator><creator><name>Ozuyar D.</name></creator><date role="Updated">2024-09-02T20:15:47Z</date><date role="Created">2023-07-26T08:44:42Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>b-stars</subject><subject>early-type-stars</subject><subject>variable-stars</subject><subject>effective-temperature</subject><subject>stellar-spectral-types</subject><subject>visible-astronomy</subject><description>Classification of over 50000 TESS stars in sectors 1-18 has resulted in the detection of 766 pulsating main-sequence B stars as well as over 5000 {delta} Scuti, 2300 {gamma} Doradus, and 114 roAp candidates. Whereas it has been assumed that high-frequency pulsations among B-type main-sequence stars are confined to the early B-type {beta} Cephei stars, the observations indicate that high frequencies are to be found over the whole B-star range, eventually merging with {delta} Scuti stars. The cool B stars pulsating in high frequencies are called Maia variables. It is shown that Maia variables are not rapidly rotating and thus cannot be {beta} Cephei pulsators that appear to have lower temperatures due to gravity darkening. In the region where {beta} Cephei variables are found, the proportion of pulsating stars is larger and amplitudes are higher and a considerable fraction pulsate in a single mode and low rotation rate. There is no distinct region of slowly pulsating B stars (SPB stars). Stars pulsating solely in low frequencies are found among all B stars. At most, only one-third of B stars appear to pulsate. These results, as well as the fact that a large fraction of A and B stars show rotational modulation, indicate a need for a revision of current ideas regarding stars with radiative envelopes.</description><source format="bibcode">2020MNRAS.493.5871B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/493/5871</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/IV/39">IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 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