Circumbinary Planets and the SOLARIS Project

Konacki, Maciej; Sybilski, P.; Kozłowski, S; Ratajczak, M.; Hełminiak, K. G.

doi:10.1017/s1743921311027098

Cited by 4 publications

(2 citation statements)

References 20 publications

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“…The major observational disadvantage of the system is its period, very close to 4 d, which makes the eclipses not always possible to observe from one place during a single season. Further work on this system requires continuous photometry from a global network of telescopes, such as WET (Nather et al 1990), Solaris (Konacki et al 2012) or HAT-S (Bakos et al 2009), in order to derive some of the crucial parameters, like the radii or temperatures, even more accurately.…”

Section: Discussionmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak

Brahm

Ratajczak

et al. 2014

A&A

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Aims. We present the results of the combined photometric and spectroscopic analysis of a bright (V = 9.14), close (d = 31 pc), late-type detached eclipsing binary, AK Fornacis. This P = 3.981 d system has not been previously recognised as a double-lined spectroscopic binary, and this is the first full physical model of this unique target. Methods. With the FEROS, CORALIE, and HARPS spectrographs, we collected a number of high-resolution spectra to calculate radial velocities of both components of the binary. Measurements were done with our own disentangling procedure and the TODCOR technique, and were later combined with the photometry from the ASAS and SuperWASP archives. We also performed an atmospheric analysis of the component spectra with the Spectroscopy Made Easy package. Results. Our analysis shows that AK For consists of two active, cool dwarfs having masses of M 1 = 0.6958 ± 0.0010 and M 2 = 0.6355 ± 0.0007 M and radii of R 1 = 0.687 ± 0.020 and R 2 = 0.609 ± 0.016 R , respectively, which are slightly less metal-abundant than the Sun. Parameters of both components are well reproduced by the models. Conclusions. AK For is the brightest system among the known eclipsing binaries with K-or M-type stars. Its orbital period is one of the longest, and its rotational velocities is one of the lowest, which allows us to obtain very precise radial velocity measurements. The precision in physical parameters that we obtained places AK For among the binaries with the best mass measurements in the literature. It also fills the gap in our knowledge of stars in the range of 0.5-0.8 M and between short and long-period systems. All this makes AK For a unique benchmark for understanding the properties of low-mass stars.

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Section: Discussionmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak

Brahm

Ratajczak

et al. 2014

A&A

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“…HATSouth is the first such network, although many more are planned. The Las Cumbres Observatory Global Telescope (LCOGT; Brown et al 2010), SOLARIS (Konacki et al 2011), and the Korea Micro-lensing Telescope Network (KMTNet) (Kim et al 2010) will all form global, homogeneous, and automated networks when they are completed.…”

Section: Introductionmentioning

confidence: 99%

HATSouth: A Global Network of Fully Automated Identical Wide-Field Telescopes1

Bakos¹,

Csubry²,

Penev³

et al. 2013

Publications of the Astronomical Society of the Pacific

217

133

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HATSouth is the world's first network of automated and homogeneous telescopes that is capable of year-round 24-hour monitoring of positions over an entire hemisphere of the sky. The primary scientific goal of the network is to discover and characterize a large number of transiting extrasolar planets, reaching out to long periods and down to small planetary radii. HATSouth achieves this by monitoring extended areas on the sky, deriving high precision light curves for a large number of stars, searching for the signature of planetary transits, and confirming planetary candidates with larger telescopes. HATSouth employs six telescope units spread over three prime locations with large longitude separation in the southern hemisphere (Las Campanas Observatory, Chile; HESS site, Namibia; Siding Spring Observatory, Australia). Each of the HATSouth units holds four 0.18 m diameter f/2.8 focal ratio telescope tubes on a common mount producing an 8.2 • × 8.2 • field-of-view on the sky, imaged using four 4K × 4K CCD cameras and Sloan r filters, to give a pixel scale of 3.7 ′′ pixel −1 . The HATSouth network is capable of continuously monitoring 128 square arc-degrees at celestial positions moderately close to the anti-solar direction. We present the technical details of the network, summarize operations, and present detailed weather statistics for the three sites. Robust operations have meant that on average each of the six HATSouth units has conducted observations on ∼ 500 nights over a two-year time period, yielding a total of more than 1 million science frames at four minute integration time, and observing ∼ 10.65 hours per day on average. We describe the scheme of our data transfer and reduction from raw pixel images to trend-filtered light curves and transiting planet candidates. Photometric precision reaches ∼ 6 mmag at 4 minute cadence for the brightest non-saturated stars at r ≈ 10.5. We present detailed transit recovery simulations to determine the expected yield of transiting planets from HATSouth. We highlight the advantages of networked operations, namely, a threefold increase in the expected number of detected planets, as compared to all telescopes operating from the same site.

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Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

Marcadon

Hełminiak

Marques

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a new analysis of the multiple star V1200 Centauri based on the most recent observations for this system. We used the photometric observations from the Solaris network and the TESS telescope, combined with the new radial velocities from the CHIRON spectrograph and those published in the literature. We confirmed that V1200 Cen consists of a 2.5-day eclipsing binary orbited by a third body. We derived the parameters of the eclipsing components, which are MAa = 1.393 ± 0.018 M⊙, RAa = 1.407 ± 0.014 R⊙ and Teff, Aa = 6 588 ± 58 K for the primary, and MAb = 0.863 3 ± 0.008 1 M⊙, RAb = 1.154 ± 0.014 R⊙ and Teff, Ab = 4 475 ± 68 K for the secondary. Regarding the third body, we obtained significantly different results than previously published. The period of the outer orbit is found to be 180.4 days, implying a minimum mass MB = 0.871 ± 0.020 M⊙. Thus, we argue that V1200 Cen is a quadruple system with a secondary pair composed of two low-mass stars. Finally, we determined the ages of each eclipsing component using two evolution codes, namely MESA and CESTAM. We obtained ages of 16–18.5 Myr and 5.5–7 Myr for the primary and the secondary, respectively. In particular, the secondary appears larger and hotter than predicted at the age of the primary. We concluded that dynamical and tidal interactions occurring in multiples may alter the stellar properties and explain the apparent non-coevality of V1200 Centauri.

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Circumbinary Planets and the SOLARIS Project

Cited by 4 publications

References 20 publications

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

HATSouth: A Global Network of Fully Automated Identical Wide-Field Telescopes1

Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

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