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<ri:Resource created="2024-06-21T09:02:18Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>EX Hya spectra</title><shortName>J/A+A/686/A304</shortName><identifier>ivo://CDS.VizieR/J/A+A/686/A304</identifier><altIdentifier>doi:10.26093/cds/vizier.36860304</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Beuermann K.</name></creator><creator><name>Reinsch K.</name></creator><date role="Updated">2024-11-29T20:03:19Z</date><date role="Created">2024-06-21T09:02:18Z</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>spectroscopic-binary-stars</subject><subject>cataclysmic-variable-stars</subject><subject>spectroscopy</subject><subject>ultraviolet-astronomy</subject><subject>visible-astronomy</subject><description>EX Hya is one of the best studied, but still enigmatic intermediate polars. We present phase-resolved blue VLT/UVES high-resolution ({lambda}/{DELTA}{lambda}~=16.000) spectra of EX Hya taken in January 2004. Our analysis involves a unique decomposition of the Balmer line profiles into the spin-modulated line wings that represent streaming motions in the magnetosphere and the orbital-phase modulated line core that represents the accretion disk. Spectral analysis and tomography show that the division line between the two is solidly located at |v_rad_|~=1200km/s, defining the inner edge of the accretion disk at r_in_=~7x10^9^cm or ~10R1 (WD radii). This large central hole allows an unimpeded view of the tall accretion curtain at the lower pole with a shock height up to h_sh_~1R1 that is required by X-ray and optical observations. Our results contradict models that advocate a small magnetosphere and a small inner disk hole. Equating rin with the magnetospheric radius in the orbital plane allows us to derive a magnetic moment of the WD of {mu}1~=1.3x10^32^G.cm^3^ and a surface field strength B1~0.35MG. Given a polar field strength Bp~&lt;1.0MG, optical circular polarization is not expected. With an accretion rate dM/dt=3.9x10^-11^M_{sun}_/yr, the accretion torque is Gacc~=2.2x10^33^g.cm^2^/s^2^. The magnetostatic torque is of similar magnitude, suggesting that EX Hya is not far from being synchronized. We measured the orbital radial-velocity amplitude of the WD, K1=58.7+/-3.9km/s, and found a spin-dependent velocity modulation as well. The former is in perfect agreement with the mean velocity amplitude obtained by other researchers, confirming the published component masses M1~=0.79M_{sun}_ and M2~=0.11M_{sun}_ .</description><source format="bibcode">2024A&amp;A...686A.304B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/686/A304</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/461/1576">J/MNRAS/461/1576 : EX Hya mid-eclipse timings (Echevarria+, 2016)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/686/A304</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/686/A304</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/686/A304</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/686/A304</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/686/A304</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/686/A304</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface></capability><capability standardID="ivo://ivoa.net/std/TAP#aux"><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://tapvizier.cds.unistra.fr/TAPVizieR/tap</accessURL></interface></capability><coverage><footprint ivo-id="ivo://ivoa.net/std/moc"/><waveband>UV</waveband><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/A+A/686/A304/phases</name><description>Orbital and spin phases of the spectra</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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