Zobrazeno 1 - 10
of 380
pro vyhledávání: '"Stancliffe R"'
Autor:
Dimoff, A. J., Hansen, C. J., Stancliffe, R. J., Kubatova, B., Stateva, I., Kucinskas, A., Dobrovolskas, V.
Around half of the heavy elements in the universe are formed through the slow neutron capture (s-) process, which takes place in thermally pulsing asymptotic giant branch (AGB) stars with masses $1-6\;M_{\odot}$. The nucleosynthetic imprint of the s-
Externí odkaz:
http://arxiv.org/abs/2409.16761
Autor:
Decin, L., Homan, W., Danilovich, T., de Koter, A., Engels, D., Waters, L. B. F. M., Muller, S., Gielen, C., García-Hernández, D. A., Stancliffe, R. J., Sande, M. Vande, Molenberghs, G., Kerschbaum, F., Zijlstra, A. A., Mellah, I. El
Publikováno v:
Nature Astronomy, 2019
In 1981, the idea of a superwind that ends the life of cool giant stars was proposed. Extreme OH/IR-stars develop superwinds with the highest mass-loss rates known so far, up to a few 10^(-4) Msun/yr, informing our understanding of the maximum mass-l
Externí odkaz:
http://arxiv.org/abs/1902.09259
Autor:
Koch, A., Reichert, M., Hansen, C. J., Hampel, M., Stancliffe, R. J., Karakas, A., Arcones, A.
Publikováno v:
A&A 622, A159 (2019)
Metal-poor stars in the Galactic halo often show strong enhancements in carbon and/or neutron-capture elements. However, the Galactic bulge is notable for its paucity of carbon-enhanced metal-poor (CEMP) and/or CH-stars, with only two such objects kn
Externí odkaz:
http://arxiv.org/abs/1812.07574
Autor:
Liu, Zheng-Wei, Tauris, T. M., Roepke, F. K., Moriya, T. J., Kruckow, M., Stancliffe, R. J., Izzard, R. G.
The progenitors of many core-collapse supernovae (CCSNe) are expected to be in binary systems. By performing a series of three-dimensional hydrodynamical simulations, we investigate how CCSN explosions affect their binary companion. We find that the
Externí odkaz:
http://arxiv.org/abs/1811.08556
Autor:
Matrozis, E., Stancliffe, R. J.
Publikováno v:
A&A 606, A55 (2017)
Carbon-enhanced metal-poor stars with s-process enrichment (CEMP-s) are believed to be the products of mass transfer from an AGB companion, which has long since become a white dwarf. The surface abundances of CEMP-s stars are thus commonly assumed to
Externí odkaz:
http://arxiv.org/abs/1707.09434
Publikováno v:
A&A 606, A137 (2017)
The chemically peculiar barium stars, CH stars, and most CEMP stars are all believed to be the products of mass transfer in binary systems from a now extinct AGB primary star. The mass of the AGB star and the orbital parameters of the system are the
Externí odkaz:
http://arxiv.org/abs/1707.08224
Autor:
Buntain, J. F., Doherty, C. L., Lugaro, M., Lattanzio, J. C., Stancliffe, R. J., Karakas, A. I.
The production of the elements heavier than iron via slow neutron captures (the s process) is a main feature of the contribution of asymptotic giant branch (AGB) stars of low mass (< 5 Msun) to the chemistry of the cosmos. However, our understanding
Externí odkaz:
http://arxiv.org/abs/1706.05802
Autor:
De Nutte, R., Decin, L., Olofsson, H., Lombaert, R., de Koter, A., Karakas, A., Milam, S., Ramstedt, S., Stancliffe, R. J., Homan, W., Van de Sande, M.
Publikováno v:
A&A 600, A71 (2017)
The aim of this paper is to investigate the $^{17}$O/$^{18}$O ratio for a sample of AGB stars, containing M-, S- and C-type stars. These ratios are evaluated in relation to fundamental stellar evolution parameters: the stellar initial mass and pulsat
Externí odkaz:
http://arxiv.org/abs/1606.07445
Autor:
Matrozis, E., Stancliffe, R. J.
Publikováno v:
A&A 592, A29 (2016)
A significant fraction of all metal-poor stars are carbon-rich. Most of these carbon-enhanced metal-poor (CEMP) stars also show enhancement in elements produced mainly by the s-process (CEMP-s stars) and evidence suggests that the origin of these non
Externí odkaz:
http://arxiv.org/abs/1605.02791
We assess the systematic uncertainties in stellar evolutionary calculations for low- to intermediate-mass, main-sequence stars. We compare published stellar tracks from several different evolution codes with our own tracks computed using the stellar
Externí odkaz:
http://arxiv.org/abs/1601.03054