The Delta Scuti star 38 Eri from the ground and from space

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  • M. Paparo, Konkoly Observ Budapest, Hungarian Academy of Sciences, MTA CSFK
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  • Z. Kollath, Eotvos Lorand Univ, Eotvos Lorand University, Savaria Dept Phys
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  • R. R. Shobbrook, Australian Natl Univ, Australian National University, Siding Spring Observ
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  • J. M. Matthews, Univ British Columbia, University of British Columbia, Dept Phys & Astron
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  • V. Antoci
  • J. M. Benko, Konkoly Observ Budapest, Hungarian Academy of Sciences, MTA CSFK
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  • N. -K. Park, Avcorp Ind Inc
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  • M. T. Mirtorabi, Alzahra Univ, Alzahra University, Dept Phys
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  • K. Luedeke
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  • A. Kusakin, Fesenkov Astrophys Inst, Fesenkov Astrophysical Institute
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  • Zs. Bognar, Konkoly Observ Budapest, Hungarian Academy of Sciences, MTA CSFK
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  • A. Sodor, Konkoly Observ Budapest, Hungarian Academy of Sciences, MTA CSFK
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  • A. Garcia-Hernandez, Univ Granada UGR, University of Granada, Dept Theoret Phys & Cosmol
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  • J. H. Pena, Univ Nacl Autonoma Mexico, Universidad Nacional Autonoma de Mexico, Inst Astron, Unidad Acad Ensenada
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  • R. Kuschnig, Graz Univ Technol, Graz University of Technology, Inst Kommunikationsnetze & Satellitenkommun
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  • A. F. J. Moffat, Univ Montreal, University of Montreal, CRAQ, 15
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  • J. Rowe, Canadian Coast Guard Coll, Dept Arts Sci & Languages
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  • S. M. Rucinski, Univ Toronto, University of Toronto, Dept Astron & Astrophys
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  • D. Sasselov, Univ Western Australia, University of Western Australia, Int Ctr Radio Astron Res ICRAR
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  • W. W. Weiss, Univ Wien, University of Vienna, Inst Astron

We present and discuss the pulsational characteristics of the Delta Scuti star 38 Eri from photometric data obtained at two widely spaced epochs, partly from the ground (1998) and partly from space (MOST, 2011). We found 18 frequencies resolving the discrepancy among the previously published frequencies. Some of the frequencies appeared with different relative amplitudes at two epochs, however, we carried out investigation for amplitude variability for only the MOST (Microvariability and Oscillation of STars) data. Amplitude variability was found for one of the three frequencies that satisfy the necessary frequency criteria for linear-combination or resonant-mode coupling. Checking the criteria of beating and resonant-mode coupling we excluded them as possible reason for amplitude variability. The two recently developed methods of rotational splitting and sequence search were applied to find regular spacings based only on frequencies. Doublets or incomplete multiplets with l = 1, 2, and 3 were found in the rotational splitting search. In the sequence search method we identified four sequences. The averaged spacing, probably a combination of the large separation and the rotational frequency, is 1.724 +/- 0.092 d(-1). Using the spacing and the scaling relation (rho) over bar = [ 0.0394, 0.0554] g cm(-3) was derived. The shift of the sequences proved to be the integer multiple of the rotational splitting spacing. Using the precise MOST frequencies and multicolour photometry in a hybrid way, we identified four modes with l = 1, two modes with l = 2, two modes with l = 3, and two modes as l = 0 radial modes.

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Volume477
Issue4
Pages (from-to)4362-4379
Number of pages18
ISSN0035-8711
DOIs
Publication statusPublished - Jul 2018

    Research areas

  • space vehicles, techniques: photometric, stars: individual: 38 Eri, stars: interiors, stars: oscillations, Stars: variables: delta Scuti, RAPIDLY ROTATING STARS, WHOLE EARTH TELESCOPE, NONRADIAL OSCILLATIONS, MODE-IDENTIFICATION, PETERSEN DIAGRAMS, UNEXPECTED SERIES, REGULAR PATTERNS, SCT STARS, PHOTOMETRY, PULSATION

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