27th Young Scientists' Conference on Astronomy and Space Physics

V4142 Sgr a Double Periodic Variable with an accretor surrounded by the accretion-disk's atmosphere

28 Apr 2021, 15:00

50m

https://us02web.zoom.us/j/2709113918?pwd=ZnIyUml2VEN6YnkvSi90eTlwUzNLUT09

Stellar Astrophysics and Interstellar Medium

Speaker

Mr Rosales Guzmán Jaime Andrés (Department of Physics, North-West University, Private Bag X2046, Mmabatho 2735, South Africa; Departamento de Astronom ́ia, Universidad de Concepci ́on, Casilla 160-C, Concepci ́on,Chile)

Description

We present a a detailed study of the Double Periodic Variable V4142 Sgr based on photometric and spectroscopic analysis. We re-analized and improved an orbital period of $30.633\pm 0.002\mathrm{days}$ and a long cycle of $1201\pm 14\mathrm{days}$. Our spectral analysis reveals H$\alpha$ absorption with a persistent $V\le R$ asymmetry emission which is considered evidence of a possible wind in the hotspot region. In addition, we find an cold and evolved donor star of $M_{\mathrm{d}}=1.11\pm 0.2{\mathrm{M}}_{\odot }$, $T_{\mathrm{d}}=4500\pm 125\mathrm{K}$ and a $R_{\mathrm{d}}=19.4\pm 0.2{\mathrm{M}}_{\odot }$ and a rejuvenated B-dwarf companion of $M_{\mathrm{g}}=3.86\pm 0.3{\mathrm{M}}_{\odot }$, $T_{\mathrm{g}}=14380\pm 700\mathrm{K}$ and $R_{\mathrm{g}}=6.35\pm 0.2{\mathrm{R}}_{\odot }$. The gainer is surrounded by concave and geometrically thick disk creating its own atmosphere around of main component of a radial extension $R_{\mathrm{d}}=22.8\pm 0.3{\mathrm{R}}_{\odot }$, contributing ~ xx percent of the total luminosity of the system at the $V$-band.The disk is characterized by a hot-spot roughly placed where the stream hits the disk and an additional bright-spot separated $102.{}^{\circ }5\pm 0.{}^{\circ }04$ degree apart along the disk edge rim in the direction of the orbital motion. The system is seen under inclination $81.{}^{\circ }5\pm 0.{}^{\circ }3$ and to a distance $d=xx\pm xx\mathrm{pc}$. Doppler maps of the emission lines reveals sites of enhanced line emission in the 2th and 3th velocity quadrants, the first one corresponds to the hot-spot ad the second to the bright spot detected by the light curve analysis. In addition, the Balner line emission shown a disk with horseshoe-shaped.