Planetary candidates around the pulsating sdB star KIC 5807616 considered doubtful

Krzesiński, J.

doi:10.1051/0004-6361/201526346

Cited by 19 publications

(19 citation statements)

References 12 publications

(22 reference statements)

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“…The evidence was based on the observed periodic modulations in the light from the system, which were consistent with the illumination variations of the putative planets [101]. However, additional data showed that these periodic variations were not coherent enough to arise from orbital motion [102]. Again, the true origin of these planet-like signals has not been ascertained.…”

Section: Pseudoplanetsmentioning

confidence: 86%

Kepler-78 and the Ultra-Short-Period planets

Winn

Sanchis-Ojeda

Rappaport

2018

New Astronomy Reviews

113

121

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Compared to the Earth, the exoplanet Kepler-78b has a similar size (1.2 R ⊕ ) and an orbital period a thousand times shorter (8.5 hours). It is currently the smallest planet for which the mass, radius, and dayside brightness have all been measured. Kepler-78b is an exemplar of the ultra-short-period (USP) planets, a category defined by the simple criterion P orb < 1 day. We describe our Fourier-based search of the Kepler data that led to the discovery of Kepler-78b, and review what has since been learned about the population of USP planets. They are about as common as hot Jupiters, and they are almost always smaller than 2 R ⊕ . They are often members of compact multi-planet systems, although they tend to have relatively large period ratios and mutual inclinations. They might be the exposed rocky cores of "gas dwarfs," the planets between 2-4 R ⊕ in size that are commonly found in somewhat wider orbits.

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Section: Pseudoplanetsmentioning

confidence: 86%

Kepler-78 and the Ultra-Short-Period planets

Winn

Sanchis-Ojeda

Rappaport

2018

New Astronomy Reviews

113

121

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“…Bold highlights planets with measured densities. We exclude the putative planets orbiting KIC 05807616 (Krzesinski 2015). Results assume fractional vaporization of 20% of fractionating volume.…”

Section: Regulates Surface-interior Exchange: Density Evolution and Imentioning

confidence: 99%

Atmosphere-Interior Exchange on Hot, Rocky Exoplanets

Kite

Fegley

Schaefer

et al. 2016

ApJ

118

168

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We provide estimates of atmospheric pressure and surface composition on short-period rocky exoplanets with dayside magma pools and silicate vapor atmospheres. Atmospheric pressure tends toward vapor-pressure equilibrium with surface magma, and magma-surface composition is set by the competing effects of fractional vaporization and surface-interior exchange. We use basic models to show how surface-interior exchange is controlled by the planet's temperature, mass, and initial composition. We assume that mantle rock undergoes bulk melting to form the magma pool, and that winds flow radially away from the substellar point. With these assumptions, we find that: (1) atmosphere-interior exchange is fast when the planet's bulk-silicate FeO concentration is low, and slow when FeO concentration is high; (2) magma pools are compositionally well-mixed for substellar temperatures 2400 K, but compositionally variegated and rapidly variable for substellar temperatures 2400 K; (3) currents within the magma pool tend to cool the top of the solid mantle ("tectonic refrigeration"); (4) contrary to earlier work, many magma planets have time-variable surface compositions. Subject headings: planets and satellites: terrestrial planets -planets and satellites: physical evolution -planets and satellites: surfaces -planets and satellites: individual (Kepler-10 b, CoRoT-7 b, KIC 12557548 b, KOI-2700 b, K2-22 b, K2-19 d, WD 1145+017, 55 Cnc e, HD 219134 b, Kepler-36 b, Kepler-78 b, Kepler-93 b, WASP-47 e). arXiv:1606.06740v1 [astro-ph.EP] 21 Jun 2016 2. SETTING THE SCENE: CURRENTS VERSUS WINDS.Magma pool surface composition, X s , is regulated by magma currents ( §2.2), silicate-vapor winds ( §2.3), and the development of compositionally distinct surface zones ( §2.4). If currents transport much more mass than winds, then X s will be the same as pool-averaged composition X p . However, X s and X p may differ if winds outpace

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“…But this can not be confirmed with a second measurement, due to larger uncertainties. Additionally, more studies question the presence of already proposed companions, for example, Krzesinski (2015); Hutchens et al (2017). Our unique sample of long-term observations shows A108, page 14 of 19 F. Mackebrandt et al: EXOTIME: signals in the O-C-diagrams of rapid pulsating subdwarfs Fig.…”

Section: Discussionmentioning

confidence: 83%

“…They question the interpretation of the low-frequency variations for KIC 05807616 and KIC 10001893 (e.g. Krzesinski 2015;Blokesz et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The EXOTIME project: signals in the O–C diagrams of the rapidly pulsating subdwarfs DW Lyn, V1636 Ori, QQ Vir, and V541 Hya

Mackebrandt

Schuh

Silvotti

et al. 2020

A&A

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Aims. We aim to investigate variations in the arrival time of coherent stellar pulsations due to the light-travel time effect to test for the presence of sub-stellar companions. Those companions are the key to one possible formation scenario of apparently single sub-dwarf B stars. Methods. We made use of an extensive set of ground-based observations of the four large amplitude p-mode pulsators DW Lyn, V1636 Ori, QQ Vir, and V541 Hya. Observations of the TESS space telescope are available on two of the targets. The timing method compares the phase of sinusoidal fits to the full multi-epoch light curves with phases from the fit of a number of subsets of the original time series. Results. Observations of the TESS mission do not sample the pulsations well enough to be useful due to the (currently) fixed two-minute cadence. From the ground-based observations, we infer evolutionary parameters from the arrival times. The residual signals show many statistically significant periodic signals, but no clear evidence for changes in arrival time induced by sub-stellar companions. The signals can be explained partly by mode beating effects. We derive upper limits on companion masses set by the observational campaign.

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Planetary candidates around the pulsating sdB star KIC 5807616 considered doubtful

Cited by 19 publications

References 12 publications

Kepler-78 and the Ultra-Short-Period planets

Kepler-78 and the Ultra-Short-Period planets

Atmosphere-Interior Exchange on Hot, Rocky Exoplanets

The EXOTIME project: signals in the O–C diagrams of the rapidly pulsating subdwarfs DW Lyn, V1636 Ori, QQ Vir, and V541 Hya

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