2019

DOI: 10.3847/2041-8213/ab322d

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TESS Spots a Compact System of Super-Earths around the Naked-eye Star HR 858

Andrew Vanderburg

¹

,

Chelsea X. Huang

²

,

Joseph E. Rodriguez

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et al.

Abstract: Transiting Exoplanet Survey Satellite (TESS ) observations have revealed a compact multi-planet system around the sixth-magnitude star HR 858 (TIC 178155732, TOI 396), located 32 parsecs away. Three planets, each about twice the size of Earth, transit this slightly-evolved, late F-type star, which is also a member of a visual binary. Two of the planets may be in mean motion resonance. We analyze the TESS observations, using novel methods to model and remove instrumental systematic errors, and combine these dat… Show more

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Cited by 105 publications

(77 citation statements)

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“…With redox diversity, no fine-tuning of H inventory is needed to give a H 2 rich atmosphere for planets with radii in the super-Earth range. This prediction can be tested with ARIEL (Tinetti et al 2016) and perhaps JWST (at HR 858; Vanderburg et al 2019; or at GJ 9827c; Rice et al 2019). Figure 8.…”

Section: 2mentioning

confidence: 99%

Atmosphere Origins for Exoplanet Sub-Neptunes

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et al. 2020

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Planets with 2 R ⊕ < R < 3 R ⊕ and orbital period <100 d are abundant; these sub-Neptune exoplanets are not well understood. For example, Kepler sub-Neptunes are likely to have deep magma oceans in contact with their atmospheres, but little is known about the effect of the magma on the atmosphere. Here we study this effect using a basic model, assuming that volatiles equilibrate with magma at T ∼ 3000 K. For our Fe-Mg-Si-O-H model system, we find that chemical reactions between the magma and the atmosphere and dissolution of volatiles into the magma are both important. Thus, magma matters. For H, most moles go into the magma, so the mass target for both H 2 accretion and H 2 loss models is weightier than is usually assumed. The known span of magma oxidation states can produce sub-Neptunes that have identical radius but with total volatile masses varying by 20-fold. Thus, planet radius is a proxy for atmospheric composition but not for total volatile content. This redox diversity degeneracy can be broken by measurements of atmosphere mean molecular weight. We emphasise H 2 supply by nebula gas, but also consider solid-derived H 2 O. We find that adding H 2 O to Fe probably cannot make enough H 2 to explain sub-Neptune radii because >10 3 -km thick outgassed atmospheres have high mean molecular weight. The hypothesis of magma-atmosphere equilibration links observables such as atmosphere H 2 O/H 2 ratio to magma FeO content and planet formation processes. Our model's accuracy is limited by the lack of experiments (lab and/or numerical) that are specific to sub-Neptunes; we advocate for such experiments.

“…With redox diversity, no fine-tuning of H inventory is needed to give a H 2 rich atmosphere for planets with radii in the super-Earth range. This prediction can be tested with ARIEL (Tinetti et al 2016) and perhaps JWST (at HR 858; Vanderburg et al 2019; or at GJ 9827c; Rice et al 2019). Figure 8.…”

Section: 2mentioning

confidence: 99%

Atmosphere Origins for Exoplanet Sub-Neptunes

¹

,

²

,

³

et al. 2020

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Planets with 2 R ⊕ < R < 3 R ⊕ and orbital period <100 d are abundant; these sub-Neptune exoplanets are not well understood. For example, Kepler sub-Neptunes are likely to have deep magma oceans in contact with their atmospheres, but little is known about the effect of the magma on the atmosphere. Here we study this effect using a basic model, assuming that volatiles equilibrate with magma at T ∼ 3000 K. For our Fe-Mg-Si-O-H model system, we find that chemical reactions between the magma and the atmosphere and dissolution of volatiles into the magma are both important. Thus, magma matters. For H, most moles go into the magma, so the mass target for both H 2 accretion and H 2 loss models is weightier than is usually assumed. The known span of magma oxidation states can produce sub-Neptunes that have identical radius but with total volatile masses varying by 20-fold. Thus, planet radius is a proxy for atmospheric composition but not for total volatile content. This redox diversity degeneracy can be broken by measurements of atmosphere mean molecular weight. We emphasise H 2 supply by nebula gas, but also consider solid-derived H 2 O. We find that adding H 2 O to Fe probably cannot make enough H 2 to explain sub-Neptune radii because >10 3 -km thick outgassed atmospheres have high mean molecular weight. The hypothesis of magma-atmosphere equilibration links observables such as atmosphere H 2 O/H 2 ratio to magma FeO content and planet formation processes. Our model's accuracy is limited by the lack of experiments (lab and/or numerical) that are specific to sub-Neptunes; we advocate for such experiments.

“…For these bright stars and large candidate signals, Minerva-Australis is easily able to obtain new precise RV measurements (e.g. Nielsen et al 2019;Vanderburg et al 2019) over the coming years to clarify the nature of these objects.…”

Section: Candidate Signalsmentioning

confidence: 99%

The Pan-Pacific Planet Search – VIII. Complete results and the occurrence rate of planets around low-luminosity giants

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²

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³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Our knowledge of the populations and occurrence rates of planets orbiting evolved intermediate-mass stars lags behind that for solar-type stars by at least a decade. Some radial velocity surveys have targeted these low-luminosity giant stars, providing some insights into the properties of their planetary systems. Here we present the final data release of the Pan-Pacific Planet Search, a 5-year radial velocity survey using the 3.9m Anglo-Australian Telescope. We present 1293 precise radial velocity measurements for 129 stars, and highlight six potential substellar-mass companions which require additional observations to confirm. Correcting for the substantial incompleteness in the sample, we estimate the occurrence rate of giant planets orbiting low-luminosity giant stars to be approximately 7.8 +9.1 −3.3 %. This result is consistent with the frequency of such planets found to orbit main-sequence A-type stars, from which the PPPS stars have evolved.

“…We modeled this slower variability by adding a 4th-order polynomial to the least-squares fit. Unlike Vanderburg et al (2019), we did not perform high-pass-filtering of the quaternion time series before the decorrelation. Finally, we fitted a basis spline to the light curve to highpass-filter any remaining long time scale variability (excluding transits and iteratively removing outliers, see Vanderburg & Johnson 2014).…”

Section: Introductionmentioning

confidence: 99%

TESS Spots a Hot Jupiter with an Inner Transiting Neptune

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et al. 2020

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2Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS ). The host star, TOI-1130, is an 11th magnitude K-dwarf in Gaia G band. It has two transiting planets: a Neptune-sized planet (3.65 ± 0.10 R ⊕ ) with a 4.1-day period, and a hot Jupiter (1.50 +0.27 −0.22 R J ) with an 8.4-day period. Precise radial-velocity observations show that the mass of the hot Jupiter is 0.974 +0.043 −0.044 M J . For the inner Neptune, the data provide only an upper limit on the mass of 0.17 M J (3σ). Nevertheless, we are confident the inner planet is real, based on follow-up ground-based photometry and adaptive optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.

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