Oliveira, Alexandre S.
Rodrigues, Claudia V.
Palhares, Matheus S.
Diaz, Marcos P.
Silva, Karleyne M. G.
Total Authors: 6
 Univ Vale Paraiba, IP&D, Av Shishima Hifume 2911, BR-12244000 Sao Jose Dos Campos, SP - Brazil
 Inst Nacl Pesquisas Espaciais, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil
 Univ Sao Paulo, IAG, Rua Matao 1226, BR-05508090 Sao Paulo, SP - Brazil
 Univ Valparaiso, Inst Fis & Astron, Av Gran Bretana 1111, Casilla 5030, Valparaiso - Chile
 European Southern Observ, Alonso de Cordova 3107, Casilla 19001, Santiago - Chile
Total Affiliations: 5
Monthly Notices of the Royal Astronomical Society;
Web of Science Citations:
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)