Using TESS 20-sec cadence data, we have discovered an unusual combination of pulsating stars in what we infer to be a binary system. The binary consists of a standard δ Scuti star with pulsations over the range 32-41 d−1; this is in a likely wide orbit with a hot subdwarf B (sdB) star, which itself has a large-amplitude p-mode pulsation at 524 d−1. We establish constraints on the period of the putative binary by using radial velocity measurements of the δ~Scuti star and show that any sdB companion star must orbit with a period greater than a few tens of days. Our identification of this sdB binary serves as an important addition to the relatively small number of sdB binaries known to have orbital periods longer than a few days. We model such a binary using {\tt MESA} and find that this system could be formed through stable, nonconservative mass transfer from either a low- or intermediate-mass progenitor, without undergoing a common envelope phase.
@article{arxiv.2111.12098,
title = {TIC 5724661: A Long-Period Binary with a Pulsating sdB Star and $\delta$ Scuti Variable},
author = {Rahul Jayaraman and Saul Rappaport and Lorne Nelson and Donald W. Kurtz and George Dufresne and Gerald Handler and Abdel Senhadji and David W. Latham and George Zhou and Allyson Bieryla and George Ricker},
journal= {arXiv preprint arXiv:2111.12098},
year = {2022}
}