TY - JOUR
T1 - Pulsations in hot subdwarf stars
T2 - Recent advances and prospects for testing stellar physics
AU - Charpinet, Stéphane
AU - Van Grootel, V.
AU - Fontaine, G.
AU - Brassard, P.
AU - Randall, S. K.
AU - Green, E. M.
N1 - Publisher Copyright:
© International Astronomical Union 2016.
PY - 2015
Y1 - 2015
N2 - The evolved, core helium burning, extreme horizontal branch stars (also known as hot B subdwarfs) host several classes of pulsators showing either p- or g-modes, or both. They offer particularly favorable conditions for probing with asteroseismology their internal structure, thus constituting arguably the most interesting seismic window for this intermediate stage of stellar evolution. G-modes in particular have the power to probe deep inside these stars, down to the convective He-burning core boundary where uncertain physics (convection, overshooting, semi-convection) is at work. Space data recently obtained with CoRoT and Kepler are offering us the possibility to probe these regions in detail and possibly shed new light on how these processes shape the core structure. In this short paper, we present the most recent advances that have taken place in this field and we provide hints of the foreseen future achievements of hot subdwarf asteroseismology.
AB - The evolved, core helium burning, extreme horizontal branch stars (also known as hot B subdwarfs) host several classes of pulsators showing either p- or g-modes, or both. They offer particularly favorable conditions for probing with asteroseismology their internal structure, thus constituting arguably the most interesting seismic window for this intermediate stage of stellar evolution. G-modes in particular have the power to probe deep inside these stars, down to the convective He-burning core boundary where uncertain physics (convection, overshooting, semi-convection) is at work. Space data recently obtained with CoRoT and Kepler are offering us the possibility to probe these regions in detail and possibly shed new light on how these processes shape the core structure. In this short paper, we present the most recent advances that have taken place in this field and we provide hints of the foreseen future achievements of hot subdwarf asteroseismology.
KW - stars : oscillations
KW - subdwarfs
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U2 - 10.1017/S1743921316006153
DO - 10.1017/S1743921316006153
M3 - Article
AN - SCOPUS:84992623555
SN - 1743-9213
VL - 11
SP - 581
EP - 588
JO - Proceedings of the International Astronomical Union
JF - Proceedings of the International Astronomical Union
IS - A29B
ER -