J/A+A/691/A115 Time of minima of NSVS 14256825 (Zervas+, 2024)
NSVS 14256825: Period variation and orbital stability analysis of two possible
substellar companions.
Zervas K., Christopoulou P.-E.
<Astron. Astrophys. 691, A115 (2024)>
=2024A&A...691A.115Z 2024A&A...691A.115Z (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Optical
Keywords: binaries: eclipsing - planetary systems -
stars: individual: NSVS 14256825
Abstract:
Recent period investigations of the post-common envelop binary (PCEB)
NSVS 14256825 suggest that two circumbinary companions are necessary
to explain the observed eclipse timing variations (ETVs).
Our objective in this work was to search for the best-fitting curve of
two LTTE terms of the ETV diagram by implementing a grid search
optimization scheme of Keplerian (kinematic) and Newtonian (N-body)
fits alongside a dynamical stability analysis of N-body simulations.
We compiled two datasets of archival photometric data covering
different timelines and updated them with new observations and with
three new times of minima calculated from the Transiting Exoplanet
Survey Satellite (TESS). A grid search optimization process was
implemented, and the resulting solutions that fell within the 90%
confidence interval of the best-fitting curve of the ETV diagram were
tested for orbital stability using N-body simulations and the MEGNO
chaos indicator.
The Keplerian and Netwonian fits are in close agreement, and hundreds
of stable configurations were identified for both datasets reaching a
lifetime of 1Myr. Our results suggest that the ETV data can be
explained by the presence of a circumbinary planet with mass
mb=11MJup in a nearly circular inner orbit of period Pb=7yr. The
outer orbit is unconstrained with a period range Pc=20-50yr (from 3:1
to 7:1 MMR) for a circumbinary body of substellar mass
(mc=11-70MJup). The stable solutions of the minimum- and
maximum-reduced chi-square value were integrated for 100Myr and
confirmed a non-chaotic behavior. Their residuals in the ETV data
could be explained by a spin-orbit coupling model (Applegate-Lanza).
However, continuous monitoring of the system is required in order to
refine and constrain the proposed solutions.
Description:
We compiled 305 eclipse minimum times from the literature for
NSVS 14256825. In addition, we updated the TOMs with our own
observations carried out in 2017 using the 14-inch Schmidt-Cassegrain
telescope at the Patras University "Mythodea" Observatory.
Objects:
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RA (2000) DE Designation(s)
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20 20 00.45 +04 37 56.5 NSVS 14256825 = V* V1828 Aql
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 23 350 Times of minima (1999-2024) of NSVS 14256825
(literature and new)
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See also:
J/AJ/153/137 : New NSVS 14256825 eclipse times (Nasiroglu+, 2017)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 11 F11.5 d BJD Time of minima (BJD-2400000)
12 A1 --- n_BJD [*] * for minima that are not included in
dataset B
14- 20 F7.5 d e_BJD Time of minima error
22- 23 I2 --- Ref ? Reference (1)
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Note (1): References as follows:
1 = Wils et al. (2007IBVS.5800....1W 2007IBVS.5800....1W)
2 = Beuermann et al. (2012A&A...543A.138B 2012A&A...543A.138B)
3 = Kilkenny & Koen (2012MNRAS.421.3238K 2012MNRAS.421.3238K)
4 = Almeida et al. (2013ApJ...766...11A 2013ApJ...766...11A)
5 = Nasiroglu et al. (2017AJ....153..137N 2017AJ....153..137N, Cat. J/AJ/153/137)
6 = Zhu et al. (2019RAA....19..134Z 2019RAA....19..134Z)
7 = Wolf et al. (2021A&A...647A..65W 2021A&A...647A..65W)
8 = Nehir & Bulut (2022NewA...92j1703N 2022NewA...92j1703N)
9 = Pulley et al. (2022MNRAS.514.5725P 2022MNRAS.514.5725P)
10 = This work (Table 1)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Apr-2025