Search for exoplanet around northern circumpolar stars

Lee, B.-C.; Park, M.-G.; Lee, S.-M.; Jeong, Gi Seok; Oh, Hyun-Mee; Han, Inwoo; Lee, J. W.; Lee, C.-U.; Kim, S.-L.; Kim, K.-M.

doi:10.1051/0004-6361/201527076

Cited by 21 publications

(18 citation statements)

References 42 publications

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“…Regarding Kepler-91 6.6 6.7 6.8 6.9 7.0 7.1 7.2 7. Giant hosts of close-in planets Lee et al (2015), and Naef et al (2003), respectively. The blue dashed line indicates the planet mass that would produce a RV amplitude equal to the standard deviation of the RV data (once the signal of the inner planet has been removed).…”

Section: Resultsmentioning

confidence: 99%

“…We have used the RV data published in the discovery papers of HD 102956 (22 epochs in a 1164-days timespan; Johnson et al 2010), 8 Ursa Minor (21 measurements in a 1888-day timespan; Lee et al 2015), and 70 Vir (Naef et al 2003) to check for the limitations of these observations for detecting additional planets in the system. We used these data and the derived parameters in the discovery works to remove the contribution of the known planet and look for a second planet in the residuals.…”

Section: Resultsmentioning

confidence: 99%

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Close-in planets around giant stars

Lillo-Box

Barrado

Correia

2016

A&A

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Extrasolar planets abound in almost any possible configuration. However, until five years ago, there was a lack of planets orbiting closer than 0.5 au to giant or subgiant stars. Since then, recent detections have started to populated this regime by confirming 13 planetary systems. We discuss the properties of these systems in terms of their formation and evolution off the main sequence. Interestingly, we find that 70.0 ± 6.6% of the planets in this regime are inner components of multiplanetary systems. This value is 4.2σ higher than for main-sequence hosts, which we find to be 42.4 ± 0.1%. The properties of the known planets seem to indicate that the closest-in planets (a < 0.06 au) to main-sequence stars are massive (i.e., hot Jupiters) and isolated and that they are subsequently engulfed by their host as it evolves to the red giant branch, leaving only the predominant population of multiplanetary systems in orbits 0.06 < a < 0.5 au. We discuss the implications of this emerging observational trend in the context of formation and evolution of hot Jupiters.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Close-in planets around giant stars

Lillo-Box

Barrado

Correia

2016

A&A

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“…First, they are two of the very few massive planets orbiting around stars close to the mass of the Sun to be found at very low metallicity. At lower metallicities than BD+03 2562, only two other planets have been reported in the literature orbiting the stars BD +20 2457 (Niedzielski et al 2009) and HD 11755 (Lee et al 2015). The similarities among these systems are striking: giant, close to solar mass evolved stars with radii close to 30 R and with ≈7 M J minimum mass planets and in ≈1 au orbits.…”

Section: Discussionmentioning

confidence: 96%

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Villaver

Niedzielski

Wolszczan

et al. 2017

A&A

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Context. Evolved stars with planets are crucial to understanding the dependency of the planet formation mechanism on the mass and metallicity of the parent star and to studying star-planet interactions. Aims. We present two evolved stars (HD 103485 and BD+03 2562) from the Tracking Advanced PlAnetary Systems (TAPAS) with HARPS-N project devoted to RV precision measurements of identified candidates within the PennState-Toruń Centre for Astronomy Planet Search. Methods. The paper is based on precise radial velocity (RV) measurements. For HD 103485 we collected 57 epochs over 3317 days with the Hobby-Eberly Telescope (HET) and its high-resolution spectrograph and 18 ultra-precise HARPS-N data over 919 days. For BD+03 2562 we collected 46 epochs of HET data over 3380 days and 19 epochs of HARPS-N data over 919 days. Results. We present the analysis of the data and the search for correlations between the RV signal and stellar activity, stellar rotation, and photometric variability. Based on the available data, we interpret the RV variations measured in both stars as Keplerian motion. Both stars have masses close to Solar (1.11 M HD 103485 and 1.14 M BD+03 2562), very low metallicities ([Fe/H] = −0.50 and −0.71 for HD 103485 and BD+03 2562), and both have Jupiter planetary mass companions (m 2 sin i = 7 and 6.4 M J for HD 103485 and BD+03 2562 resp.) in close to terrestrial orbits (1.4 au HD 103485 and 1.3 au BD+03 2562) with moderate eccentricities (e = 0.34 and 0.2 for HD 103485 and BD+03 2562). However, we cannot totally rule-out the possibility that the signal in the case of HD 103485 is due to rotational modulation of active regions. Conclusions. Based on the current data, we conclude that BD+03 2562 has a bona fide planetary companion while for HD 103485 we cannot totally exclude the possibility that the best explanation for the RV signal modulations is not the existence of a planet but stellar activity. If the interpretation remains that both stars have planetary companions, they represent systems orbiting very evolved stars with very low metallicities, a challenge to the conditions required for the formation of massive giant gas planets.

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“…The only planetary systems discovered using RV method that bear a resemblance to TYC 3667-1280-1 are HIP 67851 b (Jones et al 2015), HD 102956 b (Johnson et al 2010), and 8 U Mi b (Lee et al 2015). However, while the host star of HIP 67851 b has a similar mass of 1.63 ± 0.22 M and is at the similar stage of stellar evolution (log g = 3.2 ± 0.2), the planet itself resides on a much wider orbit with a = 0.459 ± 0.021 au and is much lighter (1.38 ± 0.15 M J ).…”

Section: Discussionmentioning

confidence: 99%

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Niedzielski

Villaver

Nowak

et al. 2016

A&A

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Context. We present the latest result of the TAPAS project that is devoted to intense monitoring of planetary candidates that are identified within the PennState-Toruń planet search. Aims. We aim to detect planetary systems around evolved stars to be able to build sound statistics on the frequency and intrinsic nature of these systems, and to deliver in-depth studies of selected planetary systems with evidence of star-planet interaction processes. Methods. The paper is based on precise radial velocity measurements: 13 epochs collected over 1920 days with the Hobby-Eberly Telescope and its High-Resolution Spectrograph, and 22 epochs of ultra-precise HARPS-N data collected over 961 days.Results. We present a warm-Jupiter ( T eq = 1350 K, m 2 sin i = 5.4 ± 0.4 M J ) companion with an orbital period of 26.468 days in a circular (e = 0.036) orbit around a giant evolved (log g = 3.11 ± 0.09, R = 6.26 ± 0.86 R ) star with M = 1.87 ± 0.17 M . This is the most massive and oldest star found to be hosting a close-in giant planet. Its proximity to its host (a = 0.21 au) means that the planet has a 13.9 ± 2.0% probability of transits; this calls for photometric follow-up study. Conclusions. This massive warm Jupiter with a near circular orbit around an evolved massive star can help set constraints on general migration mechanisms for warm Jupiters and, given its high equilibrium temperature, can help test energy deposition models in hot Jupiters.

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Search for exoplanet around northern circumpolar stars

Cited by 21 publications

References 42 publications

Close-in planets around giant stars

Close-in planets around giant stars

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

Tracking Advanced Planetary Systems (TAPAS) with HARPS-N

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