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Tipo de ReferênciaArtigo em Evento (Conference Proceedings)
Sitemtc-m21c.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP3W34R/3RFK4CL
Repositóriosid.inpe.br/mtc-m21c/2018/07.18.14.54
Última Atualização2020:09.29.12.41.30 simone
Metadadossid.inpe.br/mtc-m21c/2018/07.18.14.54.28
Última Atualização dos Metadados2020:09.29.12.41.31 simone
Chave SecundáriaINPE--PRE/
Chave de CitaçãoVieira:2018:EsSoLu
TítuloEstimate of the solar luminosity variability for cycles 23 and 24
Ano2018
Data de Acesso11 abr. 2021
Número de Arquivos1
Tamanho55 KiB
Área de contextualização
AutorVieira, Luís Eduardo Antunes
GrupoDIDGE-CGCEA-INPE-MCTIC-GOV-BR
AfiliaçãoInstituto Nacional de Pesquisas Espaciais (INPE)
Endereço de e-Mail do Autorluis.vieira@inpe.br
Nome do EventoCospar Scientific Assembly, 42
Localização do EventoPasadena, California
Data14-22 July
Tipo SecundárioPRE CI
Histórico2018-07-18 14:58:11 :: simone -> administrator :: 2018
2019-01-04 16:57:07 :: administrator -> simone :: 2018
2019-01-07 14:00:47 :: simone -> administrator :: 2018
2019-01-14 17:06:31 :: administrator -> simone :: 2018
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É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
ResumoThe effect of the solar activity on the solar luminosity, which is the total electromagnetic solar output, is one of the fundamental questions in solar physics. Changes of the solar luminosity can arise from changes of the energy flux in the convection zone that can also affects other solar parameters such as the surface temperature, the apparent radius and shape, and the symmetry of the radiative field itself. Additionally, understanding the latitudinal distribution of the flux density is needed to compare the solar variability and its stellar analogues. Nevertheless, our observations of the solar flux density are limited to a region near the ecliptic plane, which have provided just a raw estimate of the variability of the solar luminosity. Here we present a reconstruction of the solar flux density and solar luminosity for the solar cycle 23 and ascending phase of cycle 24. The reconstruction is based on a combination of a state-of-art solar surface magnetic flux transport model and a semi-empirical total and spectral irradiance model. The flux transport model is based on assimilation of MDI/ SOHO and HMI/SDO magnetograms. The irradiance models free parameters are estimated by minimizing the difference between the models output and the PMOD Composite of TSI measurements. We have obtained a good agreement between the models output and the measurements. The distribution of active regions leads to a clear low latitude brightening during the solar maximum. This brightening results from the balance of the contributions from bright (faculae and network) and dark features (sunspots) located in the solar surface, which peaks near the solar equator. As the effects of dark features are limited to a narrower region, the variability of the flux density at the poles is dominated by the evolution of faculae and network. The preliminary results indicate that the heat flux blocked by sunspots is lower than the flux leaked by bright features. Consequently, an increase of the luminosity through the cycle is observed as previously estimated based on near ecliptic measurements. This work also enables an assessment of the properties of solar variability when viewed from out of the ecliptic, i.e., such as we might be viewing other stars of solar activity level. Finally, the limitations of the model and future strategies to extend the reconstruction of the flux density and solar luminosity will be presented.
AreaCEA
ArranjoINPE > Produção > DIDGE > Estimate of the...
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agreement.html 18/07/2018 11:54 1.0 KiB 
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URL dos dadoshttp://urlib.net/rep/8JMKD3MGP3W34R/3RFK4CL
URL dos dados zipadoshttp://urlib.net/zip/8JMKD3MGP3W34R/3RFK4CL
Idiomaen
Arquivo Alvovieira_estimate.pdf
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Acervo Hospedeirourlib.net/www/2017/11.22.19.04
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