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

2023-04-01, Izquierdo, Paula, Gänsicke, Boris T., Rodríguez-Gil, Pablo, Koester, Detlev, TOLOZA CASTILLO, ODETTE FABIOLA, Gentile Fusillo, Nicola P., Pala, Anna F., Tremblay, Pier Emmanuel

Abstract White dwarf photospheric parameters are usually obtained by means of spectroscopic or photometric analysis. These results are not always consistent with each other, with the published values often including just the statistical uncertainties. The differences are more dramatic for white dwarfs with helium-dominated photospheres, so to obtain realistic uncertainties we have analysed a sample of 13 of these white dwarfs, applying both techniques to up to three different spectroscopic and photometric data sets for each star. We found mean standard deviations of $\left\langle \sigma {T_{\mathrm{eff}}}\right\rangle = 524$ K, $\left\langle \sigma {\log g}\right\rangle = 0.27$ dex and $\left\langle \sigma {\log (\mathrm{H/He})}\right\rangle = 0.31$ dex for the effective temperature, surface gravity, and relative hydrogen abundance, respectively, when modelling diverse spectroscopic data. The photometric fits provided mean standard deviations up to $\left\langle \sigma {T_{\mathrm{eff}}}\right\rangle = 1210$ K and $\left\langle \sigma {\log g}\right\rangle = 0.13$ dex. We suggest these values to be adopted as realistic lower limits to the published uncertainties in parameters derived from spectroscopic and photometric fits for white dwarfs with similar characteristics. In addition, we investigate the effect of fitting the observational data adopting three different photospheric chemical compositions. In general, pure helium model spectra result in larger Teff compared to those derived from models with traces of hydrogen. The log g shows opposite trends: smaller spectroscopic values and larger photometric ones when compared to models with hydrogen. The addition of metals to the models also affects the derived atmospheric parameters, but a clear trend is not found.