white unfix

Job offers

of Cepheid Properties

SB2 Cepheids
Classical Cepheids
Type II Cepheids

by category
by first author
by target



Visitors so far: 20031.

Fig. 1. (top) Configuration of the binary system based on radial velocity curves supported by the expected mass from evolutionary models. (bottom) Model of the radial velocity curves.

Discovery of a binary Cepheid with a 59-d orbital period

Relevant publication:

Discovery of a binary-origin classical Cepheid in a binary system with a 59-day orbital period

Pilecki B., Thompson, I. B., Espinoza-Arancibia, F., Anderson R. I., Gieren W., Narloch W., Minniti, J., Pietrzyński G., Taormina M., Bono, G., Hajdu, G.

2022, ApJL, 940, L48 (← click to see the publication at ADS/arXiv)


We report the discovery of a surprising binary configuration of the double-mode Cepheid OGLE-LMC-CEP-1347 pulsating in the first (P1=0.690d) and second overtone (P2=0.556d) modes. The orbital period (Porb=59d) of the system is five times shorter than the shortest known to date (310d) for a binary Cepheid. The Cepheid itself is also the shortest-period one ever found in a binary system and the first double-mode Cepheid in a spectroscopically double-lined binary.

OGLE-LMC-CEP-1347 is most probably on its first crossing through the instability strip, as inferred from both its short period and fast period increase, consistent with evolutionary models, and from the short orbital period (not expected for binary Cepheids whose components have passed through the red giant phase). Our evolutionary analysis yielded a first-crossing Cepheid with a mass in the range of 2.9-3.4 M⊙ (lower than any measured Cepheid mass), consistent with observations.

The companion is a stable star, at least two times fainter and less massive than the Cepheid (preliminary mass ratio q=0.55), while also redder and thus at the subgiant or more advanced evolutionary stage. To match these characteristics, the Cepheid has to be a product of binary interaction, most likely a merger of two less massive stars, which makes it the second known classical Cepheid of binary origin. Moreover, further evolution of the components may lead to another binary interaction.


We gratefully acknowledge financial support for this work from the Polish National Science Centre grant SONATA BIS 2020/38/E/ST9/00486.