J/A+A/627/A153 NSVS 10653195 light and velocity curves (Iglesias-Marzoa+, 2019)
Absolute dimensions of the low-mass eclipsing binary system NSVS 10653195.
Iglesias-Marzoa R., Arevalo M.J., Lopez-Morales M., Torres G., Lazaro C.,
Coughlin J.L.
<Astron. Astrophys. 627, A153 (2019)>
=2019A&A...627A.153I 2019A&A...627A.153I (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Radial velocities ; Photometry
Keywords: stars: fundamental parameters - stars: low-mass -
binaries: eclipsing - binaries: spectroscopic -
stars: individual: NSVS 10653195
Abstract:
Low-mass stars in eclipsing binary systems show radii larger and
effective temperatures lower than theoretical stellar models predict
for isolated stars with the same masses. Eclipsing binaries with
low-mass components are hard to find due to their low luminosity. As a
consequence, the analysis of the known low-mass eclipsing systems is
key to understand this behavior.
We aim to investigate the mass-radius relation for low-mass stars
and the cause of the deviation of the observed radii in low-mass
detached eclipsing binary stars (LMDEB) from theoretical stellar
models.
We developed a physical model of the LMDEB system NSVS 10653195 to
accurately measure the masses and radii of the components. We obtained
several high-resolution spectra in order to fit a spectroscopic orbit.
Standardized absolute photometry was obtained to measure reliable
color indices and to measure the mean Teff of the system in
out-of-eclipse phases. We observed and analyzed optical VRI and
infrared JK band differential light-curves which were fitted using
PHOEBE. A Markov-Chain Monte Carlo (MCMC) simulation near the solution
found provides robust uncertainties for the fitted parameters.
NSVS 10653195 is a detached eclipsing binary composed of two similar
stars with masses of M1=0.6402±0.0052M☉ and
M2=0.6511±0.0052M☉ and radii of
R1=0.687+0.017-0.024R☉ and R2=0.672+0.018-0.022R☉.
Spectral types were estimated to be K6V and K7V. These stars rotate in
a circular orbit with an orbital inclination of i=86.22±0.61 degrees
and a period of P=0.5607222(2)d. The distance to the system is
estimated to be d=135.2+7.6-7.9pc, in excellent agreement with the
value from Gaia. If solar metallicity were assumed, the age of the
system would be older than log(age)∼8 based on the Mbol-logTeff
diagram.
NSVS 10653195 is composed of two oversized and active K stars. While
their radii is above model predictions their Teff are in better
agreement with models.
Description:
We generated an accurate physical model of the low-mass eclipsing
binary NSVS 10653195 with the goal of measure the physical parameters
of its components and to compare them with the prediction of
theoretical stellar evolution models. We analyzed the Kepler mission
light curve of T-Cyg1-12664 to accurately measure the times and phases
of the primary and secondary eclipse. In addition, we measured the
rotational period of the primary component by analyzing the
out-of-eclipse oscillations in the light curve due to spots. We
accurately constrained the effective temperature of the system using
ground-based absolute photometry in B, V, R_C, and I_C. We also
obtained and analyzed V R_C I_C differential light curves to measure
the eccentricity and the system's orbital inclination, and a precise
Teff ratio. From the joint analysis of new radial velocities and those
in the literature we measured the individual masses of the stars.
Finally, the PHOEBE code was used to build a physical model of the
system.
Objects:
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RA (2000) DE Designation(s)
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16 07 27.86 +12 13 59.1 NSVS 10653195 = 2MASS J16072787+1213590
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 29 723 VRI differential photometry from SARA 0.9m
table2.dat 35 1643 JK differential photometry from TCS
table3.dat 45 38 Radial velocity measurements from TRES
table7.dat 26 54 Eclipse times from literature and IR photometry
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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- 14 F14.6 d HJD Heliocentric Julian Date
16- 21 F6.3 mag dmag Differential magnitude
23- 27 F5.3 mag e_dmag Uncertainty in differential magnitude
29 A1 --- Filter [VRI] Filter
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 14 F14.6 d HJD Heliocentric Julian Date
16- 21 F6.3 mag dmag Differential magnitude
23- 27 F5.3 mag e_dmag Uncertainty in differential magnitude
29- 33 F5.3 --- Airmass Airmass
35 A1 --- Filter [JK] Filter
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 12 F12.4 d HJD Heliocentric Julian Date
14- 20 F7.2 km/s RV1 Primary radial velocity
22- 25 F4.2 km/s e_RV1 Uncertainty in primary radial velocity
27- 33 F7.2 km/s RV2 Secondary radial velocity
35- 38 F4.2 km/s e_RV2 Uncertainty in secondary radial velocity
40- 45 F6.4 --- Phase Photometric phase
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d HJD Heliocentric Julian Date of minimum
15- 21 F7.5 d e_HJD Uncertainty in HJD
23 A1 --- Type [P/S] Type of minimum
(Primary, P, or Secondary, S)
25- 26 I2 --- Ref [1/10] Reference (1)
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Note (1): References as follows:
1 = Kazarovets et al. (NSV, 1998IBVS.4655....1K 1998IBVS.4655....1K, Cat. II/219)
2 = Pojmanski (ASAS, 1998, Cat. J/AcA/48/35)
3 = Wolf et al. (2010, ASP Conf. Ser. 435, 441)
4 = Coughlin & Shaw (2007, Journal of the Southeastern Association for
Research in Astronomy, 1, 7)
5 = Zhang et al. (2014, Cat. J/MNRAS/442/2620)
6 = Zhang et al. (2015NewA...41...37Z 2015NewA...41...37Z)
7 = Honkova et al. (2015, Open European Journal on Variable Stars, 168, 1)
In the paper, the minimum at 2456824.37893 appears as P but it must be S.
It is corrected in this table.
8 = Jurysek et al. (2017, Open European Journal on Variable Stars, 179, 1)
9 = Smelcer (2019, BRNO database, available at
http://var2.astro.cz/EN/brno/index.php?lang=en)
10 = this work, from IR photometry
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References:
Coughlin and Shaw (2007JSARA...1....7C 2007JSARA...1....7C), discovery paper, first analysis
Wolf et al. (2010ASPC..435..441W 2010ASPC..435..441W), LC analysis
Zhang et al. (2014MNRAS.442.2620Z 2014MNRAS.442.2620Z), LC analysis
Zhang et al. (2015NewA...41...37Z 2015NewA...41...37Z), LC analysis, period change discovery
Acknowledgements:
Ramon Iglesias-Marzoa, rimarzoa(at)yahoo.es
(End) Ramon Iglesias-Marzoa [ULL, CEFCA], Patricia Vannier [CDS] 01-Jul-2019