Orbital Period Variation of KIC 10544976: Applegate Mechanism versus Light Travel Time Effect

Almeida, L. A.; Almeida, Leandro de; Damineli, A.; Rodrigues, C. V.; Castro, M.; Lopes, C. E. Ferreira; Jablonski, F.; Nascimento, J. D. Do; Pereira, M. G.

doi:10.3847/1538-3881/ab0963

Cited by 15 publications

(16 citation statements)

References 39 publications

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“…Such variations can be related to stellar magnetic activity or to the presence of a third body in the system (e.g. Applegate 1992;Morales et al 2010;Ferreira Lopes et al 2015b;Bours et al 2016;Almeida et al 2019). Besides that, the presence of a non-visible third body in an eccentric orbit can cause a rapid orbital precession (Soderhjelm 1975).…”

Section: Low-mass Stellar Parametersmentioning

confidence: 99%

Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey

Carmo

Lopes

Παπαγεωργίου

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The discovery and characterization of Algol eclipsing binaries (EAs) provide an opportunity to contribute for a better picture of the structure and evolution of low-mass stars. However, the cadence of most current photometric surveys hinders the detection of EAs since the separation between observations is usually larger than the eclipse(s) duration and hence few measurements are found at the eclipses. Even when those objects are detected as variable, their periods can be missed if an appropriate oversampling factor is not used in the search tools. In this paper, we apply this approach to find the periods of stars cataloged in the Catalina Real-Time Transient Survey (CRTS) as EAs having unknown period (EAup). As a result, the periods of $\sim 56\%$ of them were determined. Eight objects were identified as low-mass binary systems and modeled with the Wilson & Devinney synthesis code combined with a Monte-Carlo Markov Chain optimization procedure. The computed masses and radii are in agreement with theoretical models and show no evidence of inflated radii. This paper is the first of a series aiming to identify suspected binary systems in large surveys.

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Section: Low-mass Stellar Parametersmentioning

confidence: 99%

Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey

Carmo

Lopes

Παπαγεωργίου

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Concerning the binary case, the ETV technique allowed observers to detect a few post-CE systems with one evolved binary, comprised of a WD and a low-mass star, and a BD companion(s). Some examples of such systems are HQ Aqr, V471 Tau, HW Vir, and KIC 10544976 (Goździewski et al 2015;Vaccaro et al 2015;Beuermann et al 2012;Almeida et al 2019). No BD has been found orbiting DWDs but, similar to the case of circumbinary planets (CBPs), if such a population exists, it could be found through GW astronomy with the LISA mission (Robson et al 2018;Tamanini & Danielski 2019).…”

Section: Brown Dwarfsmentioning

confidence: 99%

Section: Brown Dwarfsmentioning

confidence: 99%

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

Danielski

Korol

Rossi

2019

A&A

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Aims. We explore the prospects for the detection of giant circumbinary exoplanets and brown dwarfs (BDs) orbiting Galactic double white dwarfs binaries (DWDs) with the Laser Interferometer Space Antenna (LISA). Methods. By assuming an occurrence rate of 50%, motivated by white dwarf pollution observations, we built a Galactic synthetic population of P-type giant exoplanets and BDs orbiting DWDs. We carried this out by injecting different sub-stellar populations, with various mass and orbital separation characteristics, into the DWD population used in the LISA mission proposal. We then performed a Fisher matrix analysis to measure how many of these three-body systems show a periodic Doppler-shifted gravitational wave perturbation detectable by LISA. Results. We report the number of circumbinary planets (CBPs) and (BDs) that can be detected by LISA for various combinations of mass and semi-major axis distributions. We identify pessimistic and optimistic scenarios corresponding, respectively, to 3 and 83 (14 and 2218) detections of CBPs (BDs), observed during the length of the nominal LISA mission. These detections are distributed all over the Galaxy following the underlying DWD distribution, and they are biased towards DWDs with higher LISA signal-to-noise ratio and shorter orbital period. Finally, we show that if LISA were to be extended for four more years, the number of systems detected will be more than doubled in both the optimistic and pessimistic scenarios. Conclusions. Our results present promising prospects for the detection of post-main sequence exoplanets and BDs, showing that gravitational waves can prove the existence of these populations over the totality of the Milky Way. Detections by LISA will deepen our knowledge on the life of exoplanets subsequent to the most extreme evolution phases of their hosts, clarifying whether new phases of planetary formation take place later in the life of the stars. Such a method is strongly complementary to electromagnetic studies within the solar region and opens a window into the investigation of planets and BDs everywhere in the entire Galaxy, and possibly even in nearby galaxies in the Local Group. Evidences for sub-stellar objects around WDs White dwarf pollutionWhite dwarfs are expected to have a pure H or He atmosphere (Schatzman 1945) and their high surface gravity (∼ 10 5 denser than the Sun) makes the sinking metals diffusion timescale several order of magnitude shorter than the evolutionary period. Yet, observations show the presence of heavy elements in the spectra of 25% to 50% of all observed WDs (Zuckerman et al. 2003(Zuckerman et al. , 2010Koester et al. 2014), indicating that a continuous supply Article number, page 1 of 16

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“…Mazeh 2008); (iii) light-time effect, due to an external perturber (e.g.,Wolf 2014).For a brief check of possibility (i) we followAlmeida et al (2019) and use the empirical studies ofOláh et al (2009), …”

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confidence: 99%

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

Kovács

Hartman

Bakos

2019

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We revisit the issue of period variation of the recently claimed red nova precursor candidate KIC 9832227. By using the data gathered during the main mission of the Kepler satellite, those collected by ground-based wide-field surveys and other monitoring programs (such as ASAS-SN), we find that the currently available timing data strongly support a model consisting of the known W UMa binary and a distant low-mass companion with an orbital period of ∼ 13.5 years. The period of the W UMa component exhibits a linear period decrease with a pace of (1.10 ± 0.05) × 10 −6 days per year, within the range of many other similar systems. This rate of decrease is several orders of magnitude lower than that of V1309 Sco, the first (and so far the only) well-established binary precursor of a nova observed a few years before the outburst. The high-fidelity fit of the timing data and the conformity of the derived minimum mass of (0.38 ± 0.02) M ⊙ of the outer companion from these data with the limit posed by the spectroscopic non-detection of this component, are in agreement with the suggested hierarchical nature of this system.

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Orbital Period Variation of KIC 10544976: Applegate Mechanism versus Light Travel Time Effect

Cited by 15 publications

References 39 publications

Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey

Recovering variable stars in large surveys: EAup Algol-type class in the Catalina Survey

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

The hierarchical triple nature of the former red nova precursor candidate KIC 9832227

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