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Published November 1, 2024 | Published
Journal Article Open

TIC 435850195: The Second Triaxial Tidally Tilted Pulsator

Jayaraman, Rahul1 ORCID icon
Rappaport, Saul A.1 ORCID icon
Powell, Brian2 ORCID icon
Handler, Gerald3 ORCID icon
Omohundro, Mark4
Gagliano, Robert5 ORCID icon
Kostov, Veselin2, 6 ORCID icon
Fuller, Jim7 ORCID icon
Kurtz, Donald W.8, 9 ORCID icon
Zhang, Valencia10
Ricker, George1 ORCID icon
  • 1. ROR icon Massachusetts Institute of Technology
  • 2. ROR icon Goddard Space Flight Center
  • 3. ROR icon Polish Academy of Sciences
  • 4. ROR icon University of Oxford
  • 5. Amateur Astronomer, Glendale, AZ 85308, USA
  • 6. ROR icon Search for Extraterrestrial Intelligence
  • 7. ROR icon California Institute of Technology
  • 8. ROR icon North-West University
  • 9. ROR icon University of Central Lancashire
  • 10. ROR icon Phillips Academy

Abstract

The Transiting Exoplanet Survey Satellite (TESS) has enabled the discovery of numerous tidally tilted pulsators (TTPs), which are pulsating stars in close binaries where the presence of a tidal bulge has the effect of tilting the primary star's pulsation axes into the orbital plane. Recently, the modeling framework developed to analyze TTPs has been applied to the emerging class of triaxial pulsators, which exhibit nonradial pulsations about three perpendicular axes. In this work, we report on the identification of the second-ever discovered triaxial pulsator, with 16 robustly detected pulsation multiplets, of which 14 are dipole doublets separated by 2ν orb. We jointly fit the spectral energy distribution and TESS light curve of the star, and find that the primary is slightly evolved off the zero-age main sequence, while the less massive secondary still lies on the zero-age main sequence. Of the 14 doublets, we associate eight with Y 10x modes and six with novel Y 10y modes. We exclude the existence of Y 11x modes in this star and show that the observed pulsation modes must be Y 10y . We also present a toy model for the triaxial pulsation framework in the context of this star. The techniques presented here can be utilized to rapidly analyze and confirm future triaxial pulsator candidates.

Copyright and License

© 2024. The Author(s). Published by the American Astronomical Society.

Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Acknowledgement

R.J. would like to thank Kevin Burdge for discussions about light-curve fitting using Lcurve (C. M. Copperwheat et al. 2010), which we (unfortunately!) did not end up using as part of this work. R.J. would also like to thank Michael Fausnaugh for information about generating barycentric corrections for TESS light curves.

V.K., S.A.R., and B.P. acknowledge financial support from the NASA Citizen Science Seed Funding Program, grant No. 22-CSSFP22-0004. G.H. thanks the Polish National Center for Science (NCN) for supporting this study through grant 2021/43/B/ST9/02972.

This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Science Mission Directorate. The QLP data used in this work was obtained from MAST (C. X. Huang 2020), hosted by the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

This work also presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is https://www.cosmos.esa.int/web/gaia. The Gaia archive website is https://gea.esac.esa.int/archive/. This research has also made use of the VizieR catalog access tool, CDS, Strasbourg, France.

Facilities

TESS - , Gaia - .

Software References

astropy (Astropy Collaboration et al. 2013, 2018, 2022), lightkurve (Lightkurve Collaboration et al. 2018), matplotlib (J. D. Hunter 2007), numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), synphot (STScI Development Team 2018), TICA (M. M. Fausnaugh et al. 2020).

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Additional details

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November 4, 2024
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