Toloza Castillo, Odette Fabiola

2019-04-05, Manser, Christopher J., Gänsicke, Boris T., Eggl, Siegfried, Hollands, Mark, Izquierdo, Paula, Koester, Detlev, Landstreet, John D., Lyra, Wladimir, Marsh, Thomas R., Meru, Farzana, Mustill, Alexander J., Rodríguez-Gil, Pablo, Toloza, Odette, Veras, Dimitri, Wilson, David J., Burleigh, Matthew R., Davies, Melvyn B., Farihi, Jay, Fusillo, Nicola Gentile, de Martino, Domitilla, Parsons, Steven G., Quirrenbach, Andreas, Raddi, Roberto, Reffert, Sabine, Santo, Melania Del, Schreiber, Matthias R., Silvotti, Roberto, Toonen, Silvia, Villaver, Eva, Wyatt, Mark, Xu, Siyi, Zwart, Simon Portegies

A low-mass planet around a white dwarf Numerous exoplanets have been detected around Sun-like stars. These stars end their lives as white dwarfs, which should inherit any surviving planetary systems. Manser et al. found periodic shifts in emission lines from a disc of gas orbiting around a white dwarf (see the Perspective by Fossati). They used numerical simulations to show that the most likely explanation for the spectral shifts is a low-mass planet orbiting within the disc. The planet must be unusually small and dense to avoid being ripped apart by tidal forces. The authors speculate that it may be the leftover core of a planet whose outer layers have been removed. Science , this issue p. 66 ; see also p. 25

2023-07-01, Toloza, Odette, Gänsicke, Boris T., Guzmán-Rincón, Laura M., Marsh, Tom R., Szkody, Paula, Schreiber, Matthias R., de Martino, Domitilla, Zorotovic, Monica, El-Badry, Kareem, Koester, Detlev, Lagos, Felipe

ABSTRACT White dwarfs that accrete from non-degenerate companions show anomalous carbon and nitrogen abundances in the photospheres of their stellar components have been postulated to be descendants of supersoft X-ray binaries. Measuring the carbon-to-nitrogen abundance ratio may provide constraints on their past evolution. We fit far-ultraviolet spectroscopy of the cataclysmic variable HS 0218 + 3229 taken with the Cosmic Origins Spectrograph using Markov chain Monte Carlo methods, and found the carbon-to-nitrogen ratio is about one tenth of the Solar value $(\rm{\log \mathrm{[C/N]}}=-0.56\pm 0.15)$. We also provide estimates of the silicon and aluminium abundances, and upper limits for iron and oxygen. Using the parameters we derived for HS 0218 + 3229 we reconstruct its past. We calculated a grid of mesa models and implemented Gaussian process fits in order to determine its most likely initial binary configuration. We found that an initial mass of the donor of $M_{\rm donor;i}=0.90-0.98,\rm{\mathrm{M}_{\odot }}$ and an initial orbital period of Porb; i = 2.88 d (Porb; i = 3.12–3.16 d) for an assumed initial white dwarf mass of $\rm{M_{\mathrm{WD}}}_\mathrm{;i}=0.83\, \rm{\mathrm{M}_{\odot }}$$(\rm{M_{\mathrm{WD}}}_{\rm ;i}=0.60\, \rm{\mathrm{M}_{\odot }})$ can replicate the measured parameters. The low mass ratio, $M_{\rm donor;i} / \rm{M_{\mathrm{WD}}}_{\rm ;i} =1.08-1.18\, (1.5-1.63)$, suggests that the system did not go through a phase of hydrogen-burning on the white dwarf’s surface. However, we can not exclude a phase of thermal time-scale mass transfer in the past. We predict that HS 0218 + 3229 will evolve below the ≃ 76.2 ± 1 min period minimum for normal cataclysmic variables.