Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...312..121t&link_type=abstract
Astronomy and Astrophysics, v.312, p.121-134
Astronomy and Astrophysics
Astrophysics
22
Stars: Cataclysmic Variables, Stars: Individual: Tt Ari, Stars: Oscillations
Scientific paper
Results based on the 30 best nightly runs are reported. The moments of 33 brightness maxima and 35 minima show large scatter of phases within 0.6^p^-interval. The value of the primary photometric period of P=0.132953+/-13x10^-6^d differs from the previously published ones. Periodograms for detrended nightly runs show significant peaks at different frequencies from 28 to 103c/d. The most prominent peaks correspond to periods of 23.7, 15.2, 27.5 and 51.6min. This argues for transient quasi-periodic oscillations (QPO) occurring at few preferred time scales rather than for a QPO with a time scale decreasing from 27min in 1962 to 17min in 1985 (Semeniuk et al. 1987). Such behaviour may be explained by the "beat-frequency model" (Hollander & van Paradijs 1992). It seems that in TT Ari we observe contributions of several instability mechanisms with similar time scales. At higher frequencies 90-900 c/d the periodogram for all observations obeys a power law with an index γ=1.600+/-0.008. This value coincides within error estimates with that of γ=1.51+/-0.04 obtained for a mean periodogram. Such apparent red noise may be owed to the QPOs. The variations in UBVRI are highly correlated. A method for determination of relative colours of "slow", "fast correlated" variations and an "uncorrelated noise" is proposed. Corresponding parameters are determined. Values U-B=-1.04mag, -1.24mag, -1.35mag and B-V=0.19mag, 0.05mag, 0.12mag for "mean brightness", "fast" and "slow" variations, respectively.
Andronov Ivan Leonidovich
Chinarova Lidia L.
Kumsiashvili M. I.
Luthardt R.
Pajdosz Gabriel
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