Optical observations and CYCLOPS post-shock region modelling of the polar V348 Pav

Autor(es)

Oliveira, Alexandre S. ^[1] ; Rodrigues, Claudia V. ^[2] ; Palhares, Matheus S. ^[1] ; Diaz, Marcos P. ^[3] ; Belloni, Diogo ^{[2, 4]} ; Silva, Karleyne M. G. ^[5]

Afiliação do(s) autor(es)

^[1] Univ Vale Paraiba, IP&D, Av Shishima Hifume 2911, BR-12244000 Sao Jose Dos Campos, SP - Brazil

^[2] Inst Nacl Pesquisas Espaciais, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil

^[3] Univ Sao Paulo, IAG, Rua Matao 1226, BR-05508090 Sao Paulo, SP - Brazil

^[4] Univ Valparaiso, Inst Fis & Astron, Av Gran Bretana 1111, Casilla 5030, Valparaiso - Chile

^[5] European Southern Observ, Alonso de Cordova 3107, Casilla 19001, Santiago - Chile

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 489, n. 3, p. 4032-4042, NOV 2019.
• Citações Web of Science: 0

Resumo

Post-shock regions (PSR) of polar cataclysmic variables (CVs) produce most of their luminosity and give rise to high circular polarization in optical wavelengths and strong variability on the white dwarf (WD) rotation period, which are distinctive features of these systems. To investigate the polar candidate V348 Pav, we obtained a comprehensive observational set including photometric, polarimetric, and spectroscopic data, which was used to constrain the post-shock properties of the system. The object presents high circular polarization (similar to 30 per cent) and high He II 4686 angstrom to H beta line ratio, confirming it is a polar. From both radial velocities and light curves, we determined an orbital period of 79.98 min, close to the orbital period minimum of CVs. The H beta radial velocity curve has a semi-amplitude of 141.4 +/- 1.5 km s(-1). Doppler tomography showed that most of the spectral line emission in this system is originated in the region of the companion star facing the WD, possibly irradiated by the emission related to the PSR. We modelled the PSR using the CYCLOPS code. The PSR density and temperature profiles, obtained by a proper solution of the hydrothermodynamic equations, were used in a 3D radiative transfer solution that takes into account the system geometry. We could reproduce the V348 Pav B, V, R, and I photometric and polarimetric data using a model with a WD magnetic field of similar to 28 MG, a WD mass of similar to 0.85M(circle dot), and a low (similar to 25 degrees) orbital inclination. These values for the WD mass and orbital inclination are consistent with the measured radial velocities. (AU)

• Processo FAPESP: 17/14289-3 - Variáveis cataclísmicas magnéticas: evolução secular com o código BSE e modelagem de emissão com o código CYCLOPS
• Beneficiário: Diogo Teixeira Belloni
• Linha de fomento: Bolsas no Brasil - Pós-Doutorado
• Processo FAPESP: 13/26258-4 - Matéria superdensa no universo
• Beneficiário: Manuel Máximo Bastos Malheiro de Oliveira
• Linha de fomento: Auxílio à Pesquisa - Temático
• Processo FAPESP: 18/23562-8 - Investigando a origem de supernovas do Tipo Ia com o código BSE
• Beneficiário: Diogo Teixeira Belloni
• Linha de fomento: Bolsas no Exterior - Estágio de Pesquisa - Pós-Doutorado