J/A+A/663/A137 HM Pup, V632 Sco, and TT Vel analysis (Liakos+, 2022)
Comprehensive analysis of southern eclipsing systems with pulsating components:
The cases of HM Pup, V632 Sco, and TT Vel.
Liakos A., Moriarty D.J.W., Blackford M.G., West J.F., Evans P.,
Moriarty C.M., Sweet S.M.
<Astron. Astrophys. 663, A137 (2022)>
=2022A&A...663A.137L 2022A&A...663A.137L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Binaries, eclipsing ; Optical ;
Binaries, spectroscopic ; Radial velocities ; Spectroscopy
Keywords: binaries: eclipsing - stars: fundamental parameters -
binaries: close - stars: oscillations - stars: variables: delta Scuti
Abstract:
This work presents an extensive analysis of the properties of three
southern semi-detached eclipsing binaries hosting a pulsating
component, namely HM Pup, V632 Sco, and TT Vel. Systematic
multi-filtered photometric observations were obtained using telescopes
located in Australia and Chile mostly between 2018 and 2021. These
observations were combined with data from the Transiting Exoplanet
Survey Satellite (TESS) mission for a detailed analysis of pulsations.
Spectral types and radial velocities were determined from spectra
obtained with the Australian National University 2.3 m telescope and
Wide Field Spectrograph. The data are modelled and the absolute
parameters of all components are derived. The light curve residuals
are further analysed using Fourier transformation techniques for the
determination of the pulsation frequencies. Using theoretical models,
the most probable modes of the principal oscillations are also
identified. Eclipse-timing variation analysis is also carried out for
all systems and the most likely mechanisms modulating the orbital
period are proposed. The physical properties of these systems are
compared with other similar cases and the locations of their
components are plotted in the Mass-Radius (M-R) and
Hertzsprung-Russell (HR) diagrams. Finally, the pulsational properties
of the oscillating components are compared with currently known
systems of this type within the orbital-pulsation period and log
g-pulsation period diagrams. These systems are confirmed as
oscillating eclipsing Algol-type systems (oEA stars), as the primary
components are pulsating stars of delta Scuti type, with evidence of
mass flow from the evolved secondary components present in their NaI
D spectra.
Description:
The catalogue contains the reduced WiFes spectroscopic data for
HM Pup, V632 Sco, and TT Vel.
Objects:
-----------------------------------------------------------
RA (2000) DE Designation(s)
-----------------------------------------------------------
07 19 37.72 -48 39 13.0 HM Pup = V* HM Pup
17 20 30.40 -43 04 34.4 V632 Sco = V* V632 Sco
10 20 16.46 -46 14 04.4 TT Vel = V* TT Vel
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
fig2.dat 25 4514 Spectroscopic data for classification
fig4.dat 28 312 K and H emission peaks of the secondary
component of HM Pup
fig5.dat 29 4639 Spectra of the secondary component of HM Pup
fig6.dat 31 4339 NaID spectra of HM Pup in various orbital phases
fig7a.dat 41 1190 NaID spectra of V632 Sco
fig7b.dat 41 2288 NaID spectra of TT Vel
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Name of the system (HMPup, TTVel, V632Sco)
9 A1 --- m_Name [PS] The component of the system (1)
11- 18 F8.3 0.1nm lambda Wavelength
20- 25 F6.4 --- Int Normalised Intensity
--------------------------------------------------------------------------------
Note (1): P = Primary component, S = Secondary component
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Date Date of observation
(2018/04/30 or 2021/05/28)
12- 19 F8.3 0.1nm lambda Wavelength
21- 26 F6.4 10-20W/m2/arcsec2/nm Flux Flux (in 10-17erg/cm2/s/arcsec2/nm)
28 A1 --- Obs [1/2] Observation number
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Line Spectral lines name
9- 12 I4 yr Year The year of the observations
(2018 for 2018/04/30 or
2021 for 2021/05/28)
14- 21 F8.3 0.1nm lambda Wavelength
23- 29 F7.4 10-20W/m2/arcsec2/nm Flux Flux (in 10-17erg/cm2/s/arcsec2/nm)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Date Date of observation,
in YYYY/MM/DD format (1)
12- 15 F4.2 --- Phase Orbital phase of the system
17- 24 F8.3 0.1nm lambda wavelength
26- 31 F6.4 10-18W/m2/arcsec2/nm Flux Flux (in 10-15erg/cm2/s/arcsec2/nm)
--------------------------------------------------------------------------------
Note (1): Date of observations are 2016/03/20, 2017/02/13, 2017/05/16,
2020/11/01, 2020/11/02, 2020/12/01 or 2021/03/28.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig7?.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Name Name of the system (TTVel, V632Sco)
9- 18 A10 "date" Date Date of observation,
in YYYY/MM/DD format (1)
20- 23 F4.2 --- Phase Orbital phase of the system
25- 32 F8.3 0.1nm lambda Wavelength
34- 39 F6.4 10-18W/m2/arcsec2/nm Flux Flux (in 10-15erg/cm2/s/arcsec2/nm)
41 A1 --- Obs [1/2] Observation number
--------------------------------------------------------------------------------
Note (1): Date of observations are 2017/07/10 or 2018/06/01 for fig7a,
2021/03/28 or 2021/05/27 for fig7b.
--------------------------------------------------------------------------------
Acknowledgements:
Alexios Liakos, alliakos(at)noa.gr
(End) Patricia Vannier [CDS] 03-May-2022