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dc.contributor.authorPala, A. F.en
dc.contributor.authorGänsicke, B. T.en
dc.contributor.authorTownsley, D.en
dc.contributor.authorBoyd, D.en
dc.contributor.authorCook, M. J.en
dc.contributor.authorDe Martino, D.en
dc.contributor.authorGodon, P.en
dc.contributor.authorHaislip, J. B.en
dc.contributor.authorHenden, A. A.en
dc.contributor.authorHubeny, I.en
dc.contributor.authorIvarsen, K. M.en
dc.contributor.authorKafka, S.en
dc.contributor.authorKnigge, C.en
dc.contributor.authorLaCluyze, A. P.en
dc.contributor.authorLong, K. S.en
dc.contributor.authorMarsh, T. R.en
dc.contributor.authorMonard, B.en
dc.contributor.authorMoore, J. P.en
dc.contributor.authorMyers, G.en
dc.contributor.authorNelson, P.en
dc.contributor.authorNogami, D.en
dc.contributor.authorOksanen, A.en
dc.contributor.authorPickard, R.en
dc.contributor.authorPoyner, G.en
dc.contributor.authorReichart, D. E.en
dc.contributor.authorRodriguez Perez, D.en
dc.contributor.authorSchreiber, M. R.en
dc.contributor.authorShears, J.en
dc.contributor.authorSion, E. M.en
dc.contributor.authorStubbings, R.en
dc.contributor.authorSzkody, P.en
dc.contributor.authorZorotovic, M.en
dc.date.accessioned2017-06-05T22:57:06Z
dc.date.available2017-06-05T22:57:06Z
dc.date.issued2017-04-21
dc.identifier.citationEffective temperatures of cataclysmic-variable white dwarfs as a probe of their evolution 2017, 466 (3):2855 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stw3293
dc.identifier.urihttp://hdl.handle.net/10150/623936
dc.description.abstractWe present HST spectroscopy for 45 cataclysmic variables (CVs), observed with HST/COS and HST/STIS. For 36 CVs, the white dwarf is recognisable through its broad Ly a absorption profile and we measure the white dwarf effective temperatures (T-eff) by fitting the HST data assuming log g = 8.35, which corresponds to the average mass for CV white dwarfs (similar or equal to 0.8M(circle dot)). Our results nearly double the number of CV white dwarfs with an accurate temperature measurement. We find that CVs above the period gap have, on average, higher temperatures (< T-eff > similar or equal to 23 000 K) and exhibit much more scatter compared to those below the gap (< T-eff >similar or equal to 15 000 K). While this behaviour broadly agrees with theoretical predictions, some discrepancies are present: ( i) all our new measurements above the gap are characterized by lower temperatures (T-eff similar or equal to 16 000-26 000 K) than predicted by the present-day CV population models (T-eff similar or equal to 38 000-43 000 K); (ii) our results below the gap are not clustered in the predicted narrow track and exhibit in particular a relatively large spread near the period minimum, which may point to some shortcomings in the CV evolutionary models. Finally, in the standard model of CV evolution, reaching the minimum period, CVs are expected to evolve back towards longer periods with mean accretion rates. M less than or similar to 2 x 10(-11)M(circle dot)yr(-1), corresponding to T-eff less than or similar to 11 500 K. We do not unambiguously identify any such system in our survey, suggesting that this major component of the predicted CV population still remains elusive to observations.
dc.description.sponsorshipNASA [NAS 5-26555]; European Research Council [320964]; Fondecyt [1141269]; STFC [ST/L000733]; Robert Martin Ayers Sciences Fund; [GO-9357]; [GO9724]; [GO-12870]; [GO-13807]; [ASI-INAF I/037/12/0]en
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttps://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3293en
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectstars: fundamental parametersen
dc.subjectnovae, cataclysmic variablesen
dc.subjectwhite dwarfsen
dc.subjectultraviolet: starsen
dc.titleEffective temperatures of cataclysmic-variable white dwarfs as a probe of their evolutionen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-11T19:54:32Z
html.description.abstractWe present HST spectroscopy for 45 cataclysmic variables (CVs), observed with HST/COS and HST/STIS. For 36 CVs, the white dwarf is recognisable through its broad Ly a absorption profile and we measure the white dwarf effective temperatures (T-eff) by fitting the HST data assuming log g = 8.35, which corresponds to the average mass for CV white dwarfs (similar or equal to 0.8M(circle dot)). Our results nearly double the number of CV white dwarfs with an accurate temperature measurement. We find that CVs above the period gap have, on average, higher temperatures (< T-eff > similar or equal to 23 000 K) and exhibit much more scatter compared to those below the gap (< T-eff >similar or equal to 15 000 K). While this behaviour broadly agrees with theoretical predictions, some discrepancies are present: ( i) all our new measurements above the gap are characterized by lower temperatures (T-eff similar or equal to 16 000-26 000 K) than predicted by the present-day CV population models (T-eff similar or equal to 38 000-43 000 K); (ii) our results below the gap are not clustered in the predicted narrow track and exhibit in particular a relatively large spread near the period minimum, which may point to some shortcomings in the CV evolutionary models. Finally, in the standard model of CV evolution, reaching the minimum period, CVs are expected to evolve back towards longer periods with mean accretion rates. M less than or similar to 2 x 10(-11)M(circle dot)yr(-1), corresponding to T-eff less than or similar to 11 500 K. We do not unambiguously identify any such system in our survey, suggesting that this major component of the predicted CV population still remains elusive to observations.


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