110 citations · 850 across the 39 of their papers we have counts for
7 papers · 1 filter
Low-mass low-metallicity AGB stars as an efficient i-process site explaining CEMP-rs stars
D. Karinkuzhi, S. Van Eck, S. Goriely +5
Among Carbon-Enhanced Metal-Poor (CEMP) stars, some are found to be enriched in s-process elements (CEMP-s), in r-process elements (CEMP-r) or in both s- and r-process elements (CE…
Li-rich K giants, dust excess, and binarity
A. Jorissen, H. Van Winckel, L. Siess +3
The origin of the Li-rich K giants is still highly debated. Here, we investigate the incidence of binarity among this family from a nine-year radial-velocity monitoring of a sample…
Weighing stars from birth to death: mass determination methods across the HRD
Aldo Serenelli, Achim Weiss, Conny Aerts +31
The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characteriza…
Binary evolution along the Red Giant Branch with BINSTAR: The barium star perspective
Ana Escorza, Lionel Siess, Hans Van Winckel +1
Barium (Ba), CH, and extrinsic or Tc-poor S-type stars are evolved low- and intermediate-mass stars that show enhancement of slow-neutron-capture-process elements on their surface,…
Recipes for bolometric corrections and Gaia luminosities of B-type stars: Application to an asteroseismic sample
May G. Pedersen, Ana Escorza, Peter I. Papics +1
We provide three statistical model prescriptions for the bolometric corrections appropriate for B-type stars as a function of: 1) T_eff, 2) T_eff, log g, and 3) T_eff, log g, [M/H]…
Discovery of technetium- and niobium-rich S stars: the case for bitrinsic stars
S. Shetye, S. Van Eck, S. Goriely +4
S stars are late-type giants with overabundances of s-process elements. They come in two flavours depending on the presence or not of technetium (Tc), an element without stable iso…
Spectroscopic orbits of three dwarf barium stars
P. L. North, A. Jorissen, A. Escorza +2
Barium stars are thought to result from binary evolution in systems wide enough to allow the more massive component to reach the asymptotic giant branch and eventually become a CO…