J/A+A/691/A260 BF Vel and RR Lep times of minima (Liakos+, 2024)
Modelling of eclipsing binary systems with pulsating components and tertiary
companions: BF Vel and RR Lep.
Liakos A., Moriarty D.J.W., Erdem A., West J.F., Evans P.
<Astron. Astrophys. 691, A260 (2024)>
=2024A&A...691A.260L 2024A&A...691A.260L (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Binaries, spectroscopic ;
Radial velocities ; Optical
Keywords: binaries: close - binaries: eclipsing -
stars: fundamental parameters - stars: individual: BF Vel -
stars: individual: RR Lep - stars: variables: delta Scuti
Abstract:
This research paper presents a comprehensive analysis of RR Lep and
BF Vel, two southern short-period semi-detached oscillating Algols
(oEA stars), which are shown to be triple systems. Spectral types of
the primary components were determined and radial velocities
calculated from spectra observed with the Australian National
University's 2.3m telescope andWide Field Spectrograph. Spectra of the
NaI D doublet confirmed the presence of tertiary components which were
apparent in the broadening function analyses and, with Hα
spectra during primary eclipses, indicated chromospherical activity in
their secondary components. Ground-based telescopes were used for
observations in several pass bands for photometric analyses. These
observations were complemented by data from the Transiting Exoplanet
Survey Satellite (TESS) mission to enable the modelling of the light
curves, followed by a detailed analysis of pulsations. Eclipse-timing
variation (ETV) analyses of both systems were used to determine the
most likely mechanisms modulating the orbital period. We found mass
values M1=2.9M☉ and M2=0.75M☉ for the components of RR
Lep, and M1=1.93M☉ and M2=0.97M☉ for those of BF Vel. By
integrating information from photometry, spectroscopy and ETV
analysis, we found that tertiary components revolve around both
systems. The primary star of RR Lep pulsates in 36 frequencies, of
which five were identified as independent modes, with the dominant one
being 32.28d-1. The pulsating component of BF Vel oscillates in 37
frequencies, with the frequency 46.73d-1 revealed as the only
independent mode. For both systems, many frequencies were found to be
related to the orbital frequency. Their physical properties were
compared with other oEA stars in Mass-Radius and Hertzsprung-Russell
diagrams, and the pulsational properties of their delta Sct components
were compared with currently known systems of this type within the
orbital-pulsation period and log g-pulsation period diagrams.
Description:
The catalogue contains radial velocity values and Times of Minima for
the systems RR Lep and BF Vel.
Objects:
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RA (2000) DE Designation(s)
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05 12 10.51 -13 11 58.5 RR Lep = HD 33789
08 56 27.03 -39 58 36.0 BF Vel = CD-39 4980
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 48 45 Radial velocities
tableb1.dat 60 203 Times of minima
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- System System name
8- 18 F11.5 d Time Modified Julian date
20- 22 F3.1 --- Phase Phase
24- 29 F6.1 m/s RV1 Radial velocity of the primary
31- 35 F5.1 m/s (O-C)1 O-C for the primary
37- 42 F6.1 m/s RV2 Radial velocity of the secondary
44- 48 F5.1 m/s (O-C)2 O-C for the secondary
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- System System name
8- 20 F13.5 d ToM Time of minima (HJD)
22- 29 A8 --- ObsType Type of observation
31- 60 A30 --- Source Source
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Acknowledgements:
A. Liakos, alliakos(at)noa.gr
(End) Patricia Vannier [CDS] 07-Sep-2024