Unusual neutron-capture nucleosynthesis in a carbon-rich Galactic bulge star. (arXiv:1812.07574v1 [astro-ph.GA])

Unusual neutron-capture nucleosynthesis in a carbon-rich Galactic bulge star. (arXiv:1812.07574v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Koch_A/0/1/0/all/0/1">A. Koch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichert_M/0/1/0/all/0/1">M. Reichert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hansen_C/0/1/0/all/0/1">C.J. Hansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hampel_M/0/1/0/all/0/1">M. Hampel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stancliffe_R/0/1/0/all/0/1">R.J. Stancliffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karakas_A/0/1/0/all/0/1">A. Karakas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcones_A/0/1/0/all/0/1">A. Arcones</a>

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 known to date. This begs the question whether the processes
that produced their abundance distribution were governed by a comparable
nucleosynthesis in similar stellar sites as for their more numerous
counterparts in the halo. Recently, two contenders of such stars were
discovered in the bulge, at [Fe/H] = $-1.5$ and $-$2.5 dex, both of which show
enhancements in [C/Fe] of 0.4 and 1.4 dex, [Ba/Fe] in excess of 1.3 dex, and
also elevated nitrogen. The more metal-poor of the stars is matched by standard
$s$-process nucleosynthesis in low-mass Asymptotic Giant Branch (AGB)
polluters. The other star shows an abnormally high [Rb/Fe] ratio. Here, we
investigate the origin of the abundance peculiarities in the Rb-rich star by
new, detailed measurements of heavy element abundances and by comparing the
chemical element ratios of 36 species to models of neutron-capture
nucleosynthesis. The $i$-process with intermediate neutron densities between
those of the $s$- and $r$-processes has been previously found to provide good
matches of CEMP stars with enhancements in both $r$- and $s$-process elements,
rather than invoking a superposition of yields from the respective individual
processes. However, the peculiar bulge star is incompatible with a pure
$i$-process from a single ingestion event. Instead, it can, statistically, be
better reproduced by models accounting for two proton ingestion events, or by
an $i$-process component in combination with $s$-process nucleosynthesis in
low-to-intermediate mass AGB stars, indicating multiple polluters. [abridged]

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 known to date. This begs the question whether the processes
that produced their abundance distribution were governed by a comparable
nucleosynthesis in similar stellar sites as for their more numerous
counterparts in the halo. Recently, two contenders of such stars were
discovered in the bulge, at [Fe/H] = $-1.5$ and $-$2.5 dex, both of which show
enhancements in [C/Fe] of 0.4 and 1.4 dex, [Ba/Fe] in excess of 1.3 dex, and
also elevated nitrogen. The more metal-poor of the stars is matched by standard
$s$-process nucleosynthesis in low-mass Asymptotic Giant Branch (AGB)
polluters. The other star shows an abnormally high [Rb/Fe] ratio. Here, we
investigate the origin of the abundance peculiarities in the Rb-rich star by
new, detailed measurements of heavy element abundances and by comparing the
chemical element ratios of 36 species to models of neutron-capture
nucleosynthesis. The $i$-process with intermediate neutron densities between
those of the $s$- and $r$-processes has been previously found to provide good
matches of CEMP stars with enhancements in both $r$- and $s$-process elements,
rather than invoking a superposition of yields from the respective individual
processes. However, the peculiar bulge star is incompatible with a pure
$i$-process from a single ingestion event. Instead, it can, statistically, be
better reproduced by models accounting for two proton ingestion events, or by
an $i$-process component in combination with $s$-process nucleosynthesis in
low-to-intermediate mass AGB stars, indicating multiple polluters. [abridged]

http://arxiv.org/icons/sfx.gif