J/A+A/566/A101 V893 Sco long-term photometry (Bruch, 2014)
Long-term photometry of the eclipsing dwarf nova V893 Scorpii.
Orbital period, oscillations, and a possible giant planet.
Bruch A.
<Astron. Astrophys. 566, A101 (2014)>
=2014A&A...566A.101B 2014A&A...566A.101B
ADC_Keywords: Binaries, eclipsing ; Photometry
Keywords: binaries: eclipsing - stars: dwarf novae -
stars: individual: V893 Sco - planets and satellites: detection
Abstract:
The cataclysmic variable V893 Sco is an eclipsing dwarf nova which,
apart from outbursts with comparatively low amplitudes, exhibits a
particularly strong variability during quiescence on timescales of
days to seconds.The present study aims to update the outdated orbital
ephemerides published previously, to investigate deviations from
linear ephemerides, and to characterize non-random brightness
variations in a range of timescales. Light curves of V893 Sco were
observed on 39 nights, spanning a total time base of about 14 years.
They contain 114 eclipses which were used to significantly improve the
precision of the orbital period and to study long-term variations of
the time of revolution. Oscillations and similar brightness variations
were studied with Fourier techniques in the individual light curves.
The orbital period exhibits long-term variations with a cycle time of
10.2 years. They can be interpreted as a light travel time effect
caused by the presence of a giant planet with approximately 9.5
Jupiter masses in a 4.5AU orbit around V893 Sco. On some nights
transient semi-periodic variations on timescales of several minutes
can be seen which may be identified as quasi-periodic oscillations.
However, it is difficult to distinguish whether they are caused by
real physical mechanisms or if they are the effect of an accidental
superposition of unrelated flickering flares. Simulations to
investigate this question are presented.
Description:
The tables contain the light curves of V893 Sco listed in Table 1 of
the paper (except the light curves of 1999 Jun 21/22 and 2013 Jun
10/11 because of unreliable time stamps). The light curves are given
as differential magnitudes between the variable star V893 Sco and the
comparison star 2UCAC 19933473. They were observed in white light (no
filter), except on JD 2451341, when a CuSO(4)-filter (see Bessell,
1990PASP..102.1181B 1990PASP..102.1181B) was used.
Objects:
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RA (2000) DE Designation(s)
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16 15 15.15 -28 37 30.1 V893 Sco = SV* SVS 1772
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 55 40 Journal of observations
phot/* . 38 Individual light curves
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 "date" Date Observation date (YYYY MMM DD)
12 A1 --- --- [2]
13- 14 I2 --- D2 [1/31]? Second day of observation, if any
15 A1 --- Rem [a] a : Light curve already used in Paper I,
Bruch et al., 2000PASP..112..237B 2000PASP..112..237B
17- 20 I4 --- JD [1307/6457] Julian date (JD-2450000)
22- 26 A5 "h:m" Start UT start observation time
28- 32 A5 "h:m" End UT end observation time
34- 36 F3.1 s TimeRes [3/6] Time resolution
38- 41 I4 --- Int [314/8682] Number of integrations
43- 53 A11 --- FileName Name of the light curve file in subdirectory
phot
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Byte-by-byte Description of file: phot/*
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Bytes Format Units Label Explanations
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1- 15 F15.7 d HJD Heliocentric Julian Date in Barycentric
Dynamical Time (BDT)
17- 23 F7.4 mag Dmag Differential magnitude V893 Sco - 2UCAC 19933473
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Acknowledgements:
Albert Bruch, albert(at)lna.br
(End) Patricia Vannier [CDS] 14-Apr-2014