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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21b.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34P/3HPBBCA
Repositorysid.inpe.br/mtc-m21b/2015/01.14.11.05.41
Last Update2015:01.15.15.15.50 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m21b/2015/01.14.11.05.42
Metadata Last Update2018:06.04.03.04.44 (UTC) administrator
DOI10.1093/mnras/stu1624
ISSN0035-8711
Labelisi 2015-01 OliveiraLimSteBorCie:2014:OrPeV
Citation KeyOliveiraLimSteBorCie:2014:OrPeV
TitleThe orbital period of the V Sge star candidate QU Carinae
ProjectFAPESP (grants 03/12618-7 and 10/12805-5).
Year2014
MonthNov.
Access Date2024, May 18
Type of Workjournal article
Secondary TypePRE PI
Number of Files1
Size1364 KiB
2. Context
Author1 Oliveira, A. S.
2 Lima, H. J. F.
3 Steiner, J. E.
4 Borges, B. W.
5 Cieslinski, Deonisio
Resume Identifier1
2
3
4
5 8JMKD3MGP5W/3C9JGTL
Group1
2
3
4
5 DAS-CEA-INPE-MCTI-GOV-BR
Affiliation1 Univ Vale Paraiba
2 Univ Vale Paraiba
3 Univ Sao Paulo
4 Univ Fed Santa Catarina
5 Instituto Nacional de Pesquisas Espaciais (INPE)
e-Mail Addressmarcelo.pazos@inpe.br
JournalMonthly Notices of the Royal Astronomical Society
Volume444
Number3
Pages2692-2699
History (UTC)2018-06-04 03:04:44 :: administrator -> marcelo.pazos@inpe.br :: 2014
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
Keywordsbinaries: close
stars: individual: QU Car
novae
cataclysmic variables
supernovae: general
X-rays: binaries
AbstractClose binary supersoft X-ray sources (CBSS) are considered strong candidates to Type Ia supernova progenitors, but very few CBSS are known in our Galaxy. The Galactic counterparts of the CBSS may be the V Sge stars, not detected in X-rays due to the strong absorption by the interstellar gas. Nevertheless, the number of members in the V Sge class is still small. In order to find new members, we selected QU Car for photometric and spectroscopic observations. The orbital period of this system was published in the literature as 10.9 h, determined from radial velocity data taken in 1979-1980, but posterior analysis of data taken in 2006-2007 did not confirm this period. We analysed the high variability of its emission line profiles with the temporal variance spectrum (TVS) technique. Besides, we recovered the 10.9 h orbital period from the radial velocities of the He II 4686 angstrom emission line and, for the first time, detected what may be the orbital modulation in the photometric data. This photometric modulation is present only in the lower brightness state data, when the flickering is attenuated. The inclusion of QU Car in the V Sge class is supported by many features like high/low states, strong winds, nebular lines and He II 4686 angstrom/H beta emission line ratios. However, the non-detection of the characteristic O VI 3811-34 angstrom lines in its spectrum claims against this classification. These lines, though, may be highly variable so additional spectra analysed with the TVS technique can, possibly, solve this question.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDAS > The orbital period...
doc Directory Contentaccess
source Directory Contentthere are no files
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4. Conditions of access and use
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zipped data URLhttp://mtc-m21b.sid.inpe.br/zip/8JMKD3MGP3W34P/3HPBBCA
Languageen
Target FileMNRAS-2014-Oliveira-2692-9.pdf
User Groupadministrator
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Reader Groupadministrator
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Visibilityshown
Archiving Policyallowpublisher allowfinaldraft
Read Permissionallow from all
Update Permissionnot transferred
5. Allied materials
LinkingTrabalho não Vinculado à Tese/Dissertação
Next Higher Units8JMKD3MGPCW/3ETR8EH
Citing Item Listsid.inpe.br/mtc-m21/2012/07.13.14.44.33 3
DisseminationWEBSCI; PORTALCAPES; SCOPUS.
Host Collectionsid.inpe.br/mtc-m21b/2013/09.26.14.25.20
6. Notes
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