000003406 001__ 3406
000003406 005__ 20180116112342.0
000003406 0247_ $$2DOI$$a10.1051/epjconf/201715205010
000003406 037__ $$aSCART-2018-0019
000003406 100__ $$aIrrgang, A.
000003406 245__ $$aThe evolved slowly pulsating B star 18 Peg. A testbed for upper main sequence stellar evolution
000003406 260__ $$c2017
000003406 520__ $$aThe predicted width of the upper main sequence in stellar evolution models depends on the empirical calibration of the convective overshooting parameter. Despite decades of discussions, its precise value is still unknown and further observational constraints are required to gauge it. Irrgang et al. ([1]) showed that the B3 III giant 18 Peg is one of the most evolved members of the class of slowly pulsating B (SPB) stars and, thus, bears tremendous potential to derive a tight lower limit for the width of the upper main sequence. In addition, 18 Peg turns out to be part of a single-lined spectroscopic binary system with an eccentric, more than 6-year orbit. The orbital solution, in combination with the absence of additional signatures of the secondary component in the spectroscopic data and the spectral energy distribution, lead to the conclusion that all the observations of 18 Peg are fully compatible with the assumption that the secondary component is either a main-sequence star with a mass of 1-4 M⊙ or a neutron star.
000003406 594__ $$aNO
000003406 700__ $$aDe Cat, P. 
000003406 700__ $$aTkachenko, A.
000003406 773__ $$c1-2$$nid. 05010$$pEPJ Web of Conferences$$v152$$y2017
000003406 8560_ $$fpeter@observatoire.be
000003406 85642 $$ahttps://www.epj-conferences.org/articles/epjconf/abs/2017/21/epjconf_puls2017_05010/epjconf_puls2017_05010.html
000003406 8564_ $$s134748$$uhttp://publi2-as.oma.be/record/3406/files/Irrgang2017_EPJWC152_05010.pdf
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000003406 905__ $$apublished in
000003406 980__ $$aNONREF