Pulsation frequencies were identified for three SB1 binary star systems, two of which
were confirmed Dor pulsators and the other being an elliptical variable, from both
photometric observations, from the TESS mission, and spectroscopic observations,
from the University of Canterbury Mt John Observatory (UCMJO) in New Zealand, of the
target stars. For HD 217792 pulsation frequencies of: 0.670(2), 1.025(1), 1.278(2),
1.3813(7), 1.639(2), and 1.840(3) d−1 were determined from photometric observations
and 0.661(1), 1.018(1), 1.278(2), 1.373(1), 1.625(2) and 1.838(2)d−1 were determined
from spectroscopic observations. For HD 17310 pulsation frequencies of: 0.403(4),
0.453(6), and 0.558(3) d−1 were determined from photometric observations and
0.404(1), 0.455(1) and 0.544(8) d−1 were determined from spectroscopic observations.
For HD 85964, an elliptical variable, frequencies of: 0.8008(1), 1.60200(2), 2.4029(2),
and 3.2036(4) d−1 were determined from photometric observation and 0.8008(1),
1.6081(1), 2.4041(1) and 3.2089(2) d−1 were determined from spectroscopic
observations. The results obtained from analysis of both sets of observations agree for
most results to one or two decimal places but not within the errors of the results
obtained from the photometric observations. These discrepancies in the determined
frequencies could be attributed to the procedure used to determine the binary orbital
parameters not accounting for any variations in radial velocity arising due to anything
other than binary motion. This has been identified as the greatest contributing factor to
the discrepancies identified between the two sets of results.
