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<ri:Resource created="2019-09-12T14:33:32Z" status="active" updated="2026-02-10T20:07:44Z" 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>X-ray activity from different types of stars</title><shortName>J/other/RAA/19.9</shortName><identifier>ivo://CDS.VizieR/J/other/RAA/19.98</identifier><altIdentifier>doi:10.26093/cds/vizier/dx/bjkji</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>He L.</name></creator><creator><name>Wang S.</name></creator><creator><name>Xu X.-J.</name></creator><creator><name>Soria R.</name></creator><creator><name>Liu J.-F.</name></creator><creator><name>Li X.-D.</name></creator><creator><name>Bai Y.</name></creator><creator><name>Bai Z.-R.,Guo J.-C.</name></creator><creator><name>Qiu Y.-L.</name></creator><creator><name>Zhang Y.</name></creator><creator><name>Xu R.-C.</name></creator><creator><name>Qian K.-C.</name></creator><date role="Updated">2026-02-10T20:07:44Z</date><date role="Created">2019-09-12T14:33:32Z</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>late-type-stars</subject><subject>x-ray-sources</subject><description>X-ray emission is an important indicator of stellar activity. In this paper, we study stellar X-ray activity using the XMM-Newton and LAMOST data for different types of stars. We provide a sample including 1259 X-ray-emitting stars, of which 1090 have accurate stellar parameter estimations. Our sample size is much larger than those used in previous works. We find a bimodal distribution of the X-ray to optical flux ratio (log(fX/fV)) for G and K stars. We interpret that this bimodality is due to two subpopulations with different coronal heating rates. Furthermore, using the full widths at half maxima calculated from H{alpha} and H{beta} lines, we show that these stars in the inactive peaks have smaller rotational velocities. This is consistent with the magnetic dynamo theory that presumes stars with low rotational velocities have low levels of stellar activity. We also examine the correlation between log(fX/fV) and luminosity of the excess emission in the H{alpha} line, and find a tight relation between the coronal and chromospheric activity indicators.</description><source format="bibcode">2019RAA....19...98H</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/RAA/19.98</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/IX/46">IX/46 : XMM-Newton Serendipitous Source Catalogue 3XMM-DR5 (XMM-SSC, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/153">V/153 : LAMOST DR4 catalogs (Luo+, 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