TESS Science Conference 2
Published July 23, 2021 | Version v1
Poster Open

On the extreme period change of the RR Lyrae variable BE Dor

Creators

  • 1. ELTE Eötvös Loránd University, Gothard Astrophysical Observatory, Szombathely, Hungary; MTA-ELTE Exoplanet Research Group, 9700 Szombathely, Szent Imre h. u. 112, Hungary
  • 2. The Observatories of the Carnegie Institution for Sciences, 813 Santa Barbara Street, Pasadena, CA 91101, USA
  • 3. Department of Experimental Physics, University of Szeged, H-6720 Szeged, Dóm tér 9, Hungary
  • 4. Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eotvos Lorand Research Network (ELKH), Konkoly Thege Miklos ut 15-17, H-1121 Budapest, Hungary; MTA CSFK Lendulet Near-Field Cosmology Research Group, 1121, Budapest, Konkoly Thege Miklós út 15-17, Hungary
  • 5. Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eotvos Lorand Research Network (ELKH), Konkoly Thege Miklos ut 15-17, H-1121 Budapest, Hungary
  • 6. Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eotvos Lorand Research Network (ELKH), Konkoly Thege Miklos ut 15-17, H-1121 Budapest, Hungary; ELTE Eötvös Loránd University, Institute of Physics, Pazmany Peter setany 1/A, 1117 Budapest, Hungary; Sydney Institute for Astronomy, School of Physics A29, University of Sydney, NSW 2006, Australia
  • 7. Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716, Warsaw, Poland
  • 8. Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlarska 2, 61137 Brno, Czech Republic; Astronomical Institute, Czech Academy of Sciences, Fricova 298, 25165, Ondrejov, Czech Republic

Contributors

Description

BE Dor is a 15th magnitude first-overtone RR Lyrae variable star in the foreground of the Large Magellanic Cloud, located at about 8.7+/-3.3 kpc from the Sun. Previous investigations have revealed a cyclic period modulation with a period of 8 yr that is associated with a very stable light curve shape. To review and update our knowledge of the seemingly pure phase modulation, we collected all photometric data from the literature and extracted the light curves from all TESS Full Frame Image observations of the star. We extend the time base of earlier studies with another ~10 yrs, supplemented with new spectroscopic observations, and uncover further hints on the true physical nature of this intriguing pulsating star.

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Additional details

References

  • Derekas A., et al,, 2004, MNRAS, 354, 821
  • Hart, J. et al., 1996, PASP, 108, 220
  • Munari U., Sordo R., Castelli F., Zwitter T., 2005, A&A, 442, 1127
  • Lenz P., Breger, M., 2005, Commun. Asteroseismol., 146, 53
  • Ricker, G. R., et al., 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003
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