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<ri:Resource created="2020-12-21T12:54:52Z" status="active" updated="2025-06-13T15:25:00Z" 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>Cool WD atmosphere models. IV. Spectral evolution</title><shortName>J/ApJ/878/63</shortName><identifier>ivo://CDS.VizieR/J/ApJ/878/63</identifier><altIdentifier>doi:10.26093/cds/vizier.18780063</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Blouin S.</name></creator><creator><name>Dufour P.</name></creator><creator><name>Thibeault C.</name></creator><creator><name>Allard N.F.</name></creator><date role="Updated">2022-09-05T12:46:49Z</date><date role="Created">2020-12-21T12:54:52Z</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>white-dwarf-stars</subject><subject>astronomical-models</subject><subject>stellar-atmospheres</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>Wide-band photometry</subject><subject>trigonometric-parallax</subject><subject>stellar-masses</subject><subject>chemical-abundances</subject><description>As a result of competing physical mechanisms, the atmospheric composition of white dwarfs changes throughout their evolution, a process known as spectral evolution. Because of the ambiguity of their atmospheric compositions and the difficulties inherent to the modeling of their dense atmospheres, no consensus exists regarding the spectral evolution of cool white dwarfs (Teff&lt;6000K). In the previous papers of this series, we presented and observationally validated a new generation of cool white dwarf atmosphere models that include all the necessary constitutive physics to accurately model those objects. Using these new models and a homogeneous sample of 501 cool white dwarfs, we revisit the spectral evolution of cool white dwarfs. Our sample includes all spectroscopically identified white dwarfs cooler than 8300K for which a parallax is available in Gaia DR2 and photometric observations are available in Pan-STARRS1 and 2MASS. Except for a few cool carbon-polluted objects, our models allow an excellent fit to the spectroscopic and photometric observations of all objects included in our sample. We identify a decrease of the ratio of hydrogen- to helium-rich objects between 7500 and 6250K, which we interpret as the signature of convective mixing. After this decrease, hydrogen-rich objects become more abundant up to 5000K. This puzzling increase, reminiscent of the non-DA gap, has yet to be explained. At lower temperatures, below 5000K, hydrogen-rich white dwarfs become rarer, which rules out the scenario in which the accretion of hydrogen from the interstellar medium dominates the spectral evolution of cool white dwarfs.</description><source format="bibcode">2019ApJ...878...63B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/878/63</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/II/246">II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/349">II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/133/413">J/ApJS/133/413 : BVRIJHK photometry of cool white dwarfs (Bergeron+, 2001)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/126/1023">J/AJ/126/1023 : White Dwarfs in the SDSS (Harris+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/156/47">J/ApJS/156/47 : DA white dwarfs from the Palomar Green Survey (Liebert+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/582">J/AJ/131/582 : Cool white dwarfs in the SDSS (Kilic+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/643/402">J/ApJ/643/402 : Cool white dwarfs in the solar neighborhood (Kawka+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/132/676">J/AJ/132/676 : SDSS hot DB white dwarfs (Eisenstein+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/167/40">J/ApJS/167/40 : SDSS4 confirmed white dwarfs catalog (Eisenstein+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/134/252">J/AJ/134/252 : New nearby white dwarf systems (Subasavage+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/663/1291">J/ApJ/663/1291 : DZ stars in SDSS DR4 (Dufour+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/190/77">J/ApJS/190/77 : Detailed analysis of cool WDs in the SDSS (Kilic+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/413/1121">J/MNRAS/413/1121 : SDSS post-common env. binaries. 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