Vol 18, No 11 (2018) / Paunzen

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The search for roAp stars: null results and new candidates from Strömgren-Crawford photometry

Ernst Paunzen, Gerald Handler, Kateřina Hoňková, Jakub Juryšek, Martin Mašek, Marek Dróżdż, Jan Janı́k, Waldemar Ogłoza, Lars Hermansson, Mats Johansson, Martin Jelı́nek, Marek Skarka, Miloslav Zejda


The rapidly oscillating Ap (roAp) stars exhibit pulsational photometric and/or radial velocity variations on time scales of several minutes, which are essential to test current pulsation models as well as our assumptions of atmospheric structure characteristics. In addition, their chemical peculiarity makes them very interesting for probing stellar formation and evolution in the presence of a global magnetic field. To date, a limited number of only 61 roAp stars is known to show photometric variability. On the other hand, a literature survey yields 619 unique stars that have unsuccessfully been searched for variability of this kind. Strömgren-Crawford uvbyβ photometry of stars from both subgroups was used to investigate whether there is a selection bias for the investigated stars. We also present new photometric measurements (202 hours on 59 different nights) of 55 roAp candidates. We did not detect any new roAp star. Although our detection limits are comparable to other surveys, we also did not find pulsations in the known roAp star HD 12098, which may be a consequence of temporal amplitude changes. On the other hand, we do find some evidence for photometric variability of beta CrB at its spectroscopically derived pulsation period. From the uvbyβ photometry we conclude that the blue border of the roAp instability strip appears observationally well defined, whereas the red border is rather poorly known and studied. Within these boundaries, a total of 4646 candidates were identified which appear worth investigating for short-term pulsational variability.


stars: chemically peculiar — stars: early-type — stars: variables: general — techniques: photometric

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DOI: https://doi.org/10.1088/1674–4527/18/11/135


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