Free Access

This article has an erratum: [https://doi.org/10.1051/0004-6361/201525666e]


Fig. 1

image

Teff − log g diagram of the full sample of hot, subluminous, RV-variable stars. The size of the symbols scales with ΔRVmax. The black circles mark stars with hydrogen dominated atmospheres (log y< 0), while the red diamonds mark stars with helium dominated atmospheres. The helium main sequence (HeMS) and the HB band are superimposed with HB evolutionary tracks (dashed lines) for subsolar metallicity (log z = −1.48) from Dorman et al. (1993). The three tracks in the high temperature range correspond to helium core masses of 0.488, 0.490 and 0.495 M (from bottom-left to top-right). Those tracks mark the EHB evolution, since the stars do not reascend the giant branch in the helium shell-burning phase. The two tracks in the upper right correspond to core masses of 0.53 and 0.54 M. Blue horizontal branch stars following those tracks are expected to experience a second giant phase. The solid line marks the relevant part of the zero-age main sequence for solar metallicity taken from Schaller et al. (1992). The two dotted lines are post-AGB tracks for hydrogen-rich stars with masses of 0.546 (lower line) and 0.565 M (upper line) taken from Schönberner (1983). The two long-dashed lines are post-AGB tracks for helium-rich stars with masses of 0.53 (lower line) and 0.609 M (upper line) taken from Althaus et al. (2009).

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.