The Transiting Multi-planet System HD 3167: A 5.7 M<sub>⊕</sub> Super-Earth and an 8.3 M<sub>⊕</sub> Mini-Neptune

Gandolfi, D.; Barragán, Oscar; Hatzes, A. P.; Fridlund, M.; Fossati, L.; Donati, P.; Johnson, Marshall C.; Nowak, G.; Prieto-Arranz, J.; Albrecht, S.; Dai, Fei; Deeg, H. J.; Endl, Michael; Grziwa, S.; Hjorth, María; Korth, J.; Nespral, D.; Saario, J.; Smith, A. M. S.; Antoniciello, G.; Alarcon, Javier; Bedell, Megan; Blay, P.; Brems, Stefan S.; Cabrera, J.; Csizmadia, Szilárd; Cusano, F.; Cochran, William D.; Eigmüller, Philipp; Erikson, A.; Hernández, J. I. González; Guenther, E. W.; Hirano, Teruyuki; Mascareño, A. Suárez; Narita, Norio; Πάλλη, Ε.; Parviainen, H.; Pätzold, M.; Persson, C. M.; Rauer, H.; Saviane, I.; Schmidtobreick, L.; Eylen, Vincent Van; Winn, Joshua N.; Zakhozhay, O. V.

doi:10.3847/1538-3881/aa832a

Cited by 79 publications

(59 citation statements)

References 89 publications

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“…Notably, the three complementary methods all yielded the same conclusions, resulting in a mass measurement for the innermost planet that is not only precise but also robust. Demory et al 2011Demory et al , 2016Winn et al 2011;Nelson et al 2014), CoRoT-7b (Léger et al 2009;Queloz et al 2009;Haywood et al 2014), WASP-47e (Becker et al 2015;Dai et al 2015;Sinukoff et al 2017b;Vanderburg et al 2017), Kepler-78b (Howard et al 2013;Pepe et al 2013;Sanchis-Ojeda et al 2013;Hatzes 2014;Grunblatt et al 2015), Kepler-10b (Batalha et al 2011;Dumusque et al 2014;Weiss et al 2016;Rajpaul et al 2017), K2-131b , HD 3167b (Vanderburg et al 2016a;Christiansen et al 2017;Gandolfi et al 2017, respectively labeled as C17 and G17 in the plot), K2-106b (Guenther et al 2017;Sinukoff et al 2017a, G17 and S17 respectively). Notably, the last two planets have two independent density measurements that are not consistent with each other, resulting in a disagreement in the interpretation of the internal composition.…”

Section: Discussionmentioning

confidence: 99%

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

et al. 2018

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Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51±0.05R Å and a mass of 5.08±0.41M Å , consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

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Section: Discussionmentioning

confidence: 99%

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

et al. 2018

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“…These planets have the advantage that due to their short periods, their masses and radii can be determined with high accuracy. Currently known transiting ultrashort-period planets (USPs) include CoRoT-7b (Léger et al 2009), 55 Cnc e (Winn et al 2011), Kepler-10b (Batalha et al 2011), Kepler-78b (Sanchis-Ojeda et al 2013, WASP-47e (Dai et al 2015;Sinukoff et al 2017a), KOI 1843.03 ), K2-106 (Guenther et al 2017), and HD3167b (discovery: Vanderburg (2016), characterization: Gandolfi et al (2017)).…”

Section: Introductionmentioning

confidence: 99%

“…Other potentially interesting objects to search for the signatures of volcanism and an exosphere using optical transmission spectroscopy are K2-106 (Guenther et al 2017) and HD3167 b (Vanderburg 2016;Gandolfi et al 2017;Christiansen et al 2017). What makes these objects interesting is that their densities are higher than that of 55 Cnc e. K2-106 b and HD3167 b have a density of 13.1 −3.6 +5.4 and 8.00 +1.10 −0.98 g cm −3 , respectively.…”

Section: Introductionmentioning

confidence: 99%

Searching for volcanic activity and a mercury-like exosphere of the super-Earth HD3167 b

Guenther

Kislyakova

2019

Monthly Notices of the Royal Astronomical Society

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HD3167 b is a transiting super-Earth that has a density which is consistent with a rocky composition. The planet is exposed to strong radiation, intense stellar wind, and likely strong tidal forces and induction heating. According to theory, planets that are so close to the star should have an atmosphere like Mercury but much more extended and denser. Other theories predict that such planets have a lava lake on their surfaces and exhibit an enormous volcanic activity. We have calculated the heating by electromagnetic induction to estimate if it can drive significant volcanic activity at HD3167 b and shown that for some magnetic fields the heating can be substantial. HD3167 is an ideal target to search for the exosphere of a planet, and signs of volcanic activity. We observed the planet in-and out-of transit with UVES in order to search for presence of lines originating from the exosphere of the planet such as the Na D 1,2 and CaII H&K lines as well as numerous [S II], [S III], and [O III] lines that are tracers of volcanic activity. We derived upper limits for the ratios of the line fluxes to the stellar flux. The upper limits that we derived are I p,λ /I * ,λ = 1.5 10 −3 for the CaII H&K lines, and I p,λ /I * ,λ = 7.2 10 −4 and I p,λ /I * ,λ = 3.3 10 −4 for the NaD 1,2 lines, respectively. The fact that our upper limits correspond to previous detections in 55 Cnc e shows that not all super-Earth show these lines all the time and that they might be variable.

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“…We used the coadded FIES spectrum, which has an SNR ratio of ∼150 per pixel at 5500 Å, to derive the fundamental parameters of GJ9827. The analysis was performed following the procedures already adopted for other K2 host stars (Johnson et al 2016;Barragán et al 2017b;Fridlund et al 2017;Gandolfi et al 2017;Guenther et al 2017). We took advantage of four different spectral analysis packages applied independently by different subgroups within our team.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

“…Sinukoff et al (2016) reported the detection of 11 multiplanetary systems from K2 Campaigns 1 and 2. However, there are few such systems around nearby stars (Armstrong et al 2015;Crossfield et al 2015;Gandolfi et al 2017), and only a handful around brighter stars that are suitable for spectroscopic characterization.…”

Section: Introductionmentioning

confidence: 99%

Three Super-Earths Transiting the Nearby Star GJ 9827

Niraula

Redfield

Dai

et al. 2017

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We report on the discovery of three transiting planets around GJ9827. The planets have radii of 1.75±0.18, 1.36±0.14, and 2.11 0.21 0.22 -+ R ⊕ , and periods of 1.20896, 3.6480, and 6.2014 days, respectively. The detection was made in Campaign 12 observations as part of our K2 survey of nearby stars. GJ9827 is a V=10.39 mag K6V star at a distance of 30.3±1.6 parsecs and the nearest star to be found hosting planets by Kepler and K2. The radial velocity follow-up, high-resolution imaging, and detection of multiple transiting objects near commensurability drastically reduce the false positive probability. The orbital periods of GJ9827b, c, and d planets are very close to the 1:3:5 mean motion resonance. Our preliminary analysis shows that GJ9827 planets are excellent candidates for atmospheric observations. Besides, the planetary radii span both sides of the rocky and gaseous divide, hence the system will be an asset in expanding our understanding of the threshold.

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The Transiting Multi-planet System HD 3167: A 5.7 M_⊕ Super-Earth and an 8.3 M_⊕ Mini-Neptune

Cited by 79 publications

References 89 publications

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Searching for volcanic activity and a mercury-like exosphere of the super-Earth HD3167 b

Three Super-Earths Transiting the Nearby Star GJ 9827

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The Transiting Multi-planet System HD 3167: A 5.7 M⊕ Super-Earth and an 8.3 M⊕ Mini-Neptune

Cited by 79 publications

References 89 publications

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Searching for volcanic activity and a mercury-like exosphere of the super-Earth HD3167 b

Three Super-Earths Transiting the Nearby Star GJ 9827

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The Transiting Multi-planet System HD 3167: A 5.7 M_⊕ Super-Earth and an 8.3 M_⊕ Mini-Neptune