Exoplanet Orbit Database. II. Updates to Exoplanets.org

Han, Eunkyu; Wang, Sharon X.; Wright, Jason T.; Feng, Y. Katherina; Zhao, M.; Fakhouri, Onsi; Brown, Jacob I.; Hancock, Colin

doi:10.1086/678447

Cited by 289 publications

(253 citation statements)

References 33 publications

(72 reference statements)

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“…Using the Exoplanet Orbit Database (Han et al 2014, exoplanets.org), we analyse the currently known exoplanet population. 3 Our analysis reveals an interesting feature: the proportion of Jovian planets in single and multiple planetary systems is skewed in favour of single planet systems (see Table 1).…”

Section: Exoplanet Populationmentioning

confidence: 99%

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Stable habitable zones of single Jovian planet systems

Agnew

Maddison

Thilliez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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With continued improvement in telescope sensitivity and observational techniques, the search for rocky planets in stellar habitable zones is entering an exciting era. With so many exoplanetary systems available for follow-up observations to find potentially habitable planets, one needs to prioritise the ever-growing list of candidates. We aim to determine which of the known planetary systems are dynamically capable of hosting rocky planets in their habitable zones, with the goal of helping to focus future planet search programs. We perform an extensive suite of numerical simulations to identify regions in the habitable zones of single Jovian planet systems where Earth mass planets could maintain stable orbits, specifically focusing on the systems in the Catalog of Earth-like Exoplanet Survey Targets (CELESTA). We find that small, Earth-mass planets can maintain stable orbits in cases where the habitable zone is largely, or partially, unperturbed by a nearby Jovian, and that mutual gravitational interactions and resonant mechanisms are capable of producing stable orbits even in habitable zones that are significantly or completely disrupted by a Jovian. Our results yield a list of 13 single Jovian planet systems in CELESTA that are not only capable of supporting an Earth-mass planet on stable orbits in their habitable zone, but for which we are also able to constrain the orbits of the Earth-mass planet such that the induced radial velocity signals would be detectable with next generation instruments.

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Section: Exoplanet Populationmentioning

confidence: 99%

“…The TPs were then randomly distributed throughout the HZ, within the range of orbital parameters shown in Table 3. All simulations used stellar parameters and HZ values from CELESTA (Chandler et al 2016), and planetary properties and orbital parameters from the Exoplanet Orbit Database (Han et al 2014).…”

Section: Dynamical Simulationsmentioning

confidence: 99%

Stable habitable zones of single Jovian planet systems

Agnew

Maddison

Thilliez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…(1) Wenger et al (2000); (2) Soubiran et al (2010); (3) Han et al (2014); (4) Głȩbocki & Gnaciński (2005); (5) Tomkin & Popper (1986).…”

Section: Observations and Data Analysismentioning

confidence: 99%

On the nature of absorption features toward nearby stars

Kohl

Czesla

Schmitt

2016

A&A

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Context. Diffuse interstellar absorption bands (DIBs) of largely unknown chemical origin are regularly observed primarily in distant early-type stars. More recently, detections in nearby late-type stars have also been claimed. These stars' spectra are dominated by stellar absorption lines. Specifically, strong interstellar atomic and DIB absorption has been reported in τ Boo. Aims. We test these claims by studying the strength of interstellar absorption in high-resolution TIGRE spectra of the nearby stars τ Boo, HD 33608, and α CrB. Methods. We focus our analysis on a strong DIB located at 5780.61 Å and on the absorption of interstellar Na. First, we carry out a differential analysis by comparing the spectra of the highly similar F-stars, τ Boo and HD 33608, whose light, however, samples different lines of sight. To obtain absolute values for the DIB absorption, we compare the observed spectra of τ Boo, HD 33608, and α CrB to PHOENIX models and carry out basic spectral modeling based on Voigt line profiles. Results. The intercomparison between τ Boo and HD 33608 reveals that the difference in the line depth is 6.85 ± 1.48 mÅ at the DIB location which is, however, unlikely to be caused by DIB absorption. The comparison between PHOENIX models and observed spectra yields an upper limit of 34.0 ± 0.3 mÅ for any additional interstellar absorption in τ Boo; similar results are obtained for HD 33608 and α CrB. For all objects we derive unrealistically large values for the radial velocity of any presumed interstellar clouds. In τ Boo we find Na D absorption with an equivalent width of 0.65 ± 0.07 mÅ and 2.3 ± 0.1 mÅ in the D 2 and D 1 lines. For the other Na, absorption of the same magnitude could only be detected in the D 2 line. Our comparisons between model and data show that the interstellar absorption toward τ Boo is not abnormally high. Conclusions. We find no significant DIB absorption in any of our target stars. Any differences between modeled and observed spectra are instead attributable to inaccuracies in the stellar atmospheric modeling than to DIB absorption.

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“…We searched the Exoplanet Orbit Database (Han et al 2014) for other systems close to this commensurability. The only system we could find with a closer normalised distance to resonance (defined in Lithwick et al 2012), , was the Kepler-372cd pair (Rowe et al 2014), where is ∼0.0003, as compared to K2-19 with ∼0.0023.…”

Section: Introductionmentioning

confidence: 99%

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Armstrong

Santerne

Veras

et al. 2015

A&A

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Aims. The K2 mission has recently begun to discover new and diverse planetary systems. In December 2014, Campaign 1 data from the mission was released, providing high-precision photometry for ∼22 000 objects over an 80-day timespan. We searched these data with the aim of detecting more important new objects. Methods. Our search through two separate pipelines led to the independent discovery of K2-19b and c, a two-planet system of Neptune-sized objects (4.2 and 7.2 R ⊕ ), orbiting a K dwarf extremely close to the 3:2 mean motion resonance. The two planets each show transits, sometimes simultaneously owing to their proximity to resonance and the alignment of conjunctions. Results. We obtained further ground-based photometry of the larger planet with the NITES telescope, demonstrating the presence of large transit timing variations (TTVs), and used the observed TTVs to place mass constraints on the transiting objects under the hypothesis that the objects are near but not in resonance. We then statistically validated the planets through the PASTIS tool, independently of the TTV analysis.

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Exoplanet Orbit Database. II. Updates to Exoplanets.org

Cited by 289 publications

References 33 publications

Stable habitable zones of single Jovian planet systems

Stable habitable zones of single Jovian planet systems

On the nature of absorption features toward nearby stars

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

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