J/A+A/691/A249 High-Inclination dwarf novae (Saez-Carvajal+, 2024)
New orbital periods of high-Inclination dwarf novae based on Gaia Alerts
photometry.
Saez-Carvajal C., Vogt N., Zorotovic M., Garcia-Veas J., Aravena-Rojas G.,
Dumond L., Figueroa-Tapia F., Lopez-Bonilla Y., Rodriguez-Jimenez A.,
Vega-Manubens I., Grawe B.
<Astron. Astrophys. 691, A249 (2024)>
=2024A&A...691A.249S 2024A&A...691A.249S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Binaries, cataclysmic; Binaries, eclipsing
Keywords: ephemerides - binaries: eclipsing - stars: dwarf novae - novae -
cataclysmic variables
Abstract:
The orbital period of a cataclysmic variable stands as a crucial
parameter for investigating the structure and physics of these binary
systems, as well as understanding their evolution. We use photometric
Gaia data of dwarf novae (DNe) in the quiescent state, available over
various years, to determine new orbital periods and improve or modify
previously suggested period values. Two approaches are implemented for
selecting high-inclination targets, either eclipsing or with
ellipsoidal variations. We determine new orbital periods for 75 DNe
and improve ephemerides for 27 more (three of which change
significantly), contributing to 9.4% of the known DNe periods between
0.05 and 2.0 days, and doubling those with periods exceeding 0.44
days. Their phase-folded light curves, available on Zenodo, are
presented and arranged by their orbital period, illustrating the
transition from short-period systems, dominated by radiation from the
accretion disk and the hot spot, to longer-period DNe, where the
Roche-lobe filling secondary star is the primary visual flux source.
This transition, which occurs around the well-known period gap
(between ∼ 2 and 3 hours), is expected since DNe with larger orbital
periods typically harbour more massive donors contributing to the
visible flux. However, this transition is not abrupt. Within the same
range of periods, we observe systems dominated by ellipsoidal
variations, where the companion star is clearly visible, as well as
others dominated by the disk and the hot spot. The presence of some
DNe with ellipsoidal variations near the lower edge of the period gap
is striking, as the companions in these systems are expected to be
cool low-mass M-dwarfs not visible in the light curve. This could
indicate that we are observing systems where the donor star was
originally much more massive and underwent significant nuclear
evolution before mass transfer began, as has been suggested previously
for QZ Ser.
Description:
This dataset contains the individual Gaia alerts eclipse (or
brightness minima) epochs for DNe systems. The table includes four
columns: the first lists the Gaia name identification of each system,
the second provides the number of detected eclipses (N), the third
shows the cycle number (E), and the fourth column presents the
corresponding Heliocentric Julian Date (HJD). These data were used to
fit Eq. 2 in the associated publication and are crucial for the
accurate determination of orbital periods.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sources.dat 53 101 List of studied sources
table1.dat 36 1052 Individual Gaia alerts eclipse (or brightness
minima) epochs for DNe systems
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Byte-by-byte Description of file: sources.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- GaiaID Gaia name identification, Gaia NNaaa
12- 31 A20 --- Name Other name
34- 35 I2 h RAh Right ascension (J2000)
37- 38 I2 min RAm Right ascension (J2000)
40- 43 F4.1 s RAs Right ascension (J2000)
45 A1 --- DE- Declination sign (J2000)
46- 47 I2 deg DEd Declination (J2000)
49- 50 I2 arcmin DEm Declination (J2000)
52- 53 I2 arcsec DEs Declination (J2000)
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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- 10 A10 --- GaiaID Gaia name identification, Gaia NNaaa
12- 15 F4.1 --- N Number of detected eclipses
17- 23 F7.1 --- E Total number of eclipse observations
25- 36 F12.2 d HJD Heliocentric Julian Date minus 2450000
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Acknowledgements:
Catalina Saez-Carvajal, catalina.saezc(at)alumnos.uv.cl
History:
19-Nov-2024: on-line version
19-Mar-2025: 2 positions corrected in sources.dat
(End) Patricia Vannier [CDS] 09-Oct-2024