A close-in giant planet escapes engulfment by its star.

When main-sequence stars expand into red giants, they are expected to engulf close-in planets1-5. Until now, the absence of planets with short orbital periods around post-expansion, core-helium-burning red giants6-8 has been interpreted as evidence that short-period planets around Sun-like stars do not survive the giant expansion phase of their host stars9. Here we present the discovery that the giant planet 8 Ursae Minoris b10 orbits a core-helium-burning red giant. At a distance of only 0.5 AU from its host star, the planet would have been engulfed by its host star, which is predicted by standard single-star evolution to have previously expanded to a radius of 0.7 AU. Given the brief lifetime of helium-burning giants, the nearly circular orbit of the planet is challenging to reconcile with scenarios in which the planet survives by having a distant orbit initially. Instead, the planet may have avoided engulfment through a stellar merger that either altered the evolution of the host star or produced 8 Ursae Minoris b as a second-generation planet11. This system shows that core-helium-burning red giants can harbour close planets and provides evidence for the role of non-canonical stellar evolution in the extended survival of late-stage exoplanetary systems.

A temperate Earth-sized planet with tidal heating transiting an M6 star.

Temperate Earth-sized exoplanets around late-M dwarfs offer a rare opportunity to explore under which conditions planets can develop hospitable climate conditions. The small stellar radius amplifies the atmospheric transit signature, making even compact secondary atmospheres dominated by N2 or CO2 amenable to characterization with existing instrumentation1. Yet, despite large planet search efforts2, detection of low-temperature Earth-sized planets around late-M dwarfs has remained rare and the TRAPPIST-1 system, a resonance chain of rocky planets with seemingly identical compositions, has not yet shown any evidence of volatiles in the system3. Here we report the discovery of a temperate Earth-sized planet orbiting the cool M6 dwarf LP 791-18. The newly discovered planet, LP 791-18d, has a radius of 1.03 ± 0.04 R⊕ and an equilibrium temperature of 300-400 K, with the permanent night side plausibly allowing for water condensation. LP 791-18d is part of a coplanar system4 and provides a so-far unique opportunity to investigate a temperate exo-Earth in a system with a sub-Neptune that retained its gas or volatile envelope. On the basis of observations of transit timing variations, we find a mass of 7.1 ± 0.7 M⊕ for the sub-Neptune LP 791-18c and a mass of [Formula: see text] for the exo-Earth LP 791-18d. The gravitational interaction with the sub-Neptune prevents the complete circularization of LP 791-18d's orbit, resulting in continued tidal heating of LP 791-18d's interior and probably strong volcanic activity at the surface5,6.

Very regular high-frequency pulsation modes in young intermediate-mass stars.

Asteroseismology probes the internal structures of stars by using their natural pulsation frequencies1. It relies on identifying sequences of pulsation modes that can be compared with theoretical models, which has been done successfully for many classes of pulsators, including low-mass solar-type stars2, red giants3, high-mass stars4 and white dwarfs5. However, a large group of pulsating stars of intermediate mass-the so-called δ Scuti stars-have rich pulsation spectra for which systematic mode identification has not hitherto been possible6,7. This arises because only a seemingly random subset of possible modes are excited and because rapid rotation tends to spoil regular patterns8-10. Here we report the detection of remarkably regular sequences of high-frequency pulsation modes in 60 intermediate-mass main-sequence stars, which enables definitive mode identification. The space motions of some of these stars indicate that they are members of known associations of young stars, as confirmed by modelling of their pulsation spectra.

Publisher Correction: A planet within the debris disk around the pre-main-sequence star AU Microscopii.

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

A planet within the debris disk around the pre-main-sequence star AU Microscopii.

AU Microscopii (AU Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 22 million years1. AU Mic possesses a relatively rare2 and spatially resolved3 edge-on debris disk extending from about 35 to 210 astronomical units from the star4, and with clumps exhibiting non-Keplerian motion5-7. Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic 'activity' on the star8,9. Here we report observations of a planet transiting AU Mic. The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07 astronomical units, a radius of 0.4 Jupiter radii, and a mass of less than 0.18 Jupiter masses at 3σ confidence. Our observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution.

A wide star-black-hole binary system from radial-velocity measurements.

All stellar-mass black holes have hitherto been identified by X-rays emitted from gas that is accreting onto the black hole from a companion star. These systems are all binaries with a black-hole mass that is less than 30 times that of the Sun1-4. Theory predicts, however, that X-ray-emitting systems form a minority of the total population of star-black-hole binaries5,6. When the black hole is not accreting gas, it can be found through radial-velocity measurements of the motion of the companion star. Here we report radial-velocity measurements taken over two years of the Galactic B-type star, LB-1. We find that the motion of the B star and an accompanying Hα emission line require the presence of a dark companion with a mass of [Formula: see text] solar masses, which can only be a black hole. The long orbital period of 78.9 days shows that this is a wide binary system. Gravitational-wave experiments have detected black holes of similar mass, but the formation of such massive ones in a high-metallicity environment would be extremely challenging within current stellar evolution theories.

A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host.

The amount of ultraviolet irradiation and ablation experienced by a planet depends strongly on the temperature of its host star. Of the thousands of extrasolar planets now known, only six have been found that transit hot, A-type stars (with temperatures of 7,300-10,000 kelvin), and no planets are known to transit the even hotter B-type stars. For example, WASP-33 is an A-type star with a temperature of about 7,430 kelvin, which hosts the hottest known transiting planet, WASP-33b (ref. 1); the planet is itself as hot as a red dwarf star of type M (ref. 2). WASP-33b displays a large heat differential between its dayside and nightside, and is highly inflated-traits that have been linked to high insolation. However, even at the temperature of its dayside, its atmosphere probably resembles the molecule-dominated atmospheres of other planets and, given the level of ultraviolet irradiation it experiences, its atmosphere is unlikely to be substantially ablated over the lifetime of its star. Here we report observations of the bright star HD 195689 (also known as KELT-9), which reveal a close-in (orbital period of about 1.48 days) transiting giant planet, KELT-9b. At approximately 10,170 kelvin, the host star is at the dividing line between stars of type A and B, and we measure the dayside temperature of KELT-9b to be about 4,600 kelvin. This is as hot as stars of stellar type K4 (ref. 5). The molecules in K stars are entirely dissociated, and so the primary sources of opacity in the dayside atmosphere of KELT-9b are probably atomic metals. Furthermore, KELT-9b receives 700 times more extreme-ultraviolet radiation (that is, with wavelengths shorter than 91.2 nanometres) than WASP-33b, leading to a predicted range of mass-loss rates that could leave the planet largely stripped of its envelope during the main-sequence lifetime of the host star.

A Comparison of 2 Abbreviated Methods for Assessing Adolescent Bone Age: The Shorthand Bone Age Method and the SickKids/Columbia Method.

BACKGROUND: Radiographic assessment of bone age is critically important to decision-making on the type and timing of operative interventions in pediatric orthopaedics. The current widely accepted method for determining bone age is time and resource-intensive. This study sought to assess the reliability and accuracy of 2 abbreviated methods, the Shorthand Bone Age (SBA) and the SickKids/Columbia (SKC) methods, to the widely accepted Greulich and Pyle (GP) method. METHODS: Standard posteroanterior radiographs of the left hand of 125 adolescent males and 125 adolescent females were compiled, with bone ages determined by the GP method ranging from 9 to 16 years for males and 8 to 14 years for females. Blinded to the chronologic age and GP bone age of each child, the bone age for each radiograph was determined using the SBA and SKC methods by an orthopaedic surgery resident, 2 pediatric orthopaedic surgeons, and a musculoskeletal radiologist. Measurements were then repeated 2 weeks later after rerandomization of the radiographs. Intrarater and interrater reliability for the 2 abbreviated methods as well as the agreement between all 3 methods were calculated using weighted κ values. Mean absolute differences between methods were also calculated. RESULTS: Both bone age methods demonstrated substantial to almost perfect intrarater reliability, with a weighted κ ranging from 0.79 to 0.93 for the SBA method and from 0.82 to 0.96 for the SKC method. Interrater reliability was moderate to substantial (weighted κ: 0.55 to 0.84) for the SBA method and substantial to almost perfect (weighted κ: 0.67 to 0.92) for the SKC method. Agreement between the 3 methods was substantial for all raters and all comparisons. The mean absolute difference, been GP-derived and SBA-derived bone age, was 7.6±7.8 months, as compared with 8.8±7.4 months between GP-derived and SKC-derived bone ages. CONCLUSIONS: The SBA and SKC methods have comparable reliability, and both correlate well to the widely accepted GP methods and to each other. However, they have relatively large absolute differences when compared with the GP method. These methods offer simple, efficient, and affordable estimates for bone age determination, but at best provide an estimate to be used in the appropriate setting. LEVEL OF EVIDENCE: Diagnostic study-level III.

A Neptune-sized transiting planet closely orbiting a 5­10-million-year-old star.

Theories of the formation and early evolution of planetary systems postulate that planets are born in circumstellar disks, and undergo radial migration during and after dissipation of the dust and gas disk from which they formed. The precise ages of meteorites indicate that planetesimals­the building blocks of planets­are produced within the first million years of a star's life. Fully formed planets are frequently detected on short orbital periods around mature stars. Some theories suggest that the in situ formation of planets close to their host stars is unlikely and that the existence of such planets is therefore evidence of large-scale migration. Other theories posit that planet assembly at small orbital separations may be common. Here we report a newly born, transiting planet orbiting its star with a period of 5.4 days. The planet is 50 per cent larger than Neptune, and its mass is less than 3.6 times that of Jupiter (at 99.7 per cent confidence), with a true mass likely to be similar to that of Neptune. The star is 5­10 million years old and has a tenuous dust disk extending outward from about twice the Earth­Sun separation, in addition to the fully formed planet located at less than one-twentieth of the Earth­Sun separation.

Supracondylar Humerus Fractures in Older Children: Success of Closed Reduction and Percutaneous Pinning.

BACKGROUND: The incidence of supracondylar humerus (SCH) fracture declines and fracture types change as children grow. Optimal treatment method is unclear in older children. The aim of the study was to determine if fracture type and configuration of distal humerus fractures changes as patients approach skeletal maturity, and to assess the success of closed reduction and percutaneous pin (CRPP) in extra-articular SCH fractures in this transitional age group. METHODS: Inclusion criteria for this retrospective review were (1) distal humerus fractures with extension types 2 and 3, flexion type, T-type; (2) surgically managed, and (3) modified Sauvegrain score ≥1. Reviewed parameters included fracture type and configuration, grade of skeletal maturity, fixation technique, and loss of reduction. Primary analysis was to determine the distribution of fracture type and configuration with age or grade of skeletal maturity. Secondary analysis was used to determine the factors affecting treatment success of CRPP in extra-articular fractures. RESULTS: A total of 142 patients were included (58 males and 84 females). Fracture types revealed significant changes with increased age (P=0.031) and skeletal maturity grade (P<0.005). Skeletal maturity was a better predictor of changing fracture type than chronological age. T-type fractures were only seen in patients with modified Sauvegrain score ≥6 and flexion-type fractures were only seen in patients with modified Sauvegrain score ≤4. Loss of reduction rate after CRPP was 5%. The success of CRPP was not affected by age, sex, modified Sauvegrain score, fracture type, direction of displacement, coronal fracture pattern, number of pins or medial pin use. Fracture obliquity in the sagittal plane (P=0.05), suboptimal pin spread (P<0.01), and lack of bicolumnar fixation (P<0.01) were found as statistically significant factors associated with failed CRPP. CONCLUSION: The distribution of fracture type changed with increased age and skeletal maturity. CRPP of extra-articular fractures in older children is a reliable option regardless of the stage of skeletal maturity. Determinants of a good outcome include optimal pinning technique with adequate pin spread at the fracture site and bicolumnar fixation. LEVEL OF EVIDENCE: Level IV-retrospective case series.

Consumption of Cow's Milk in Early Childhood and Fracture Risk: A Prospective Cohort Study.

Cow's milk is consumed by most North American children, yet the relationships between the volume and fat content of cow's milk consumed and childhood fracture risk are unclear. Our primary objectives in this study were to evaluate whether the volume or fat content of cow's milk consumed at 1-3 years of age was associated with the risk of fracture between 3 and 10 years of age. This was a prospective cohort study of 2,466 children enrolled in Toronto, Ontario, Canada, between 2008 and 2016. The primary exposure was volume of cow's milk consumed between the ages of 1 and 3 years, and the secondary exposure was average percentage of milk fat consumed by each child during the same period. The primary outcome was a parental report of child fracture at ages 3-10 years. In the primary and secondary adjusted analyses, no association between milk volume and fracture risk (adjusted relative risk = 1.04, 95% confidence interval: 0.87, 1.26) or between milk-fat content and fracture risk (adjusted relative risk = 1.05, 95% confidence interval: 0.84, 1.31) was observed. In this study, we did not identify a protective association of early childhood cow's milk volume or fat consumption with fracture risk in later childhood. Future prospective research is needed to understand whether cow's milk is beneficial for fracture prevention through the life course.

A rocky composition for an Earth-sized exoplanet.

Planets with sizes between that of Earth (with radius R Earth symbol) and Neptune (about 4R Earth symbol) are now known to be common around Sun-like stars. Most such planets have been discovered through the transit technique, by which the planet's size can be determined from the fraction of starlight blocked by the planet as it passes in front of its star. Measuring the planet's mass--and hence its density, which is a clue to its composition--is more difficult. Planets of size 2-4R Earth symbol have proved to have a wide range of densities, implying a diversity of compositions, but these measurements did not extend to planets as small as Earth. Here we report Doppler spectroscopic measurements of the mass of the Earth-sized planet Kepler-78b, which orbits its host star every 8.5 hours (ref. 6). Given a radius of 1.20 ± 0.09 R Earth symbol and a mass of 1.69 ± 0.41 R Earth symbol, the planet's mean density of 5.3 ± 1.8 g cm(-3) is similar to Earth's, suggesting a composition of rock and iron.

A sub-Mercury-sized exoplanet.

Since the discovery of the first exoplanets, it has been known that other planetary systems can look quite unlike our own. Until fairly recently, we have been able to probe only the upper range of the planet size distribution, and, since last year, to detect planets that are the size of Earth or somewhat smaller. Hitherto, no planets have been found that are smaller than those we see in the Solar System. Here we report a planet significantly smaller than Mercury. This tiny planet is the innermost of three that orbit the Sun-like host star, which we have designated Kepler-37. Owing to its extremely small size, similar to that of the Moon, and highly irradiated surface, the planet, Kepler-37b, is probably rocky with no atmosphere or water, similar to Mercury.

Alignment of the stellar spin with the orbits of a three-planet system.

The Sun's equator and the planets' orbital planes are nearly aligned, which is presumably a consequence of their formation from a single spinning gaseous disk. For exoplanetary systems this well-aligned configuration is not guaranteed: dynamical interactions may tilt planetary orbits, or stars may be misaligned with the protoplanetary disk through chaotic accretion , magnetic interactions or torques from neighbouring stars. Indeed, isolated 'hot Jupiters' are often misaligned and even orbiting retrograde. Here we report an analysis of transits of planets over starspots on the Sun-like star Kepler-30 (ref. 8), and show that the orbits of its three planets are aligned with the stellar equator. Furthermore, the orbits are aligned with one another to within a few degrees. This configuration is similar to that of our Solar System, and contrasts with the isolated hot Jupiters. The orderly alignment seen in the Kepler-30 system suggests that high obliquities are confined to systems that experienced disruptive dynamical interactions. Should this be corroborated by observations of other coplanar multi-planet systems, then star-disk misalignments would be ruled out as the explanation for the high obliquities of hot Jupiters, and dynamical interactions would be implicated as the origin of hot Jupiters.

Transiting circumbinary planets Kepler-34 b and Kepler-35 b.

Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars (binaries). Although long anticipated, the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than ∼1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.

Supernova SN 2011fe from an exploding carbon-oxygen white dwarf star.

Type Ia supernovae have been used empirically as 'standard candles' to demonstrate the acceleration of the expansion of the Universe even though fundamental details, such as the nature of their progenitor systems and how the stars explode, remain a mystery. There is consensus that a white dwarf star explodes after accreting matter in a binary system, but the secondary body could be anything from a main-sequence star to a red giant, or even another white dwarf. This uncertainty stems from the fact that no recent type Ia supernova has been discovered close enough to Earth to detect the stars before explosion. Here we report early observations of supernova SN 2011fe in the galaxy M101 at a distance from Earth of 6.4 megaparsecs. We find that the exploding star was probably a carbon-oxygen white dwarf, and from the lack of an early shock we conclude that the companion was probably a main-sequence star. Early spectroscopy shows high-velocity oxygen that slows rapidly, on a timescale of hours, and extensive mixing of newly synthesized intermediate-mass elements in the outermost layers of the supernova. A companion paper uses pre-explosion images to rule out luminous red giants and most helium stars as companions to the progenitor.

Occurrence and core-envelope structure of 1-4× Earth-size planets around Sun-like stars.

Small planets, 1-4× the size of Earth, are extremely common around Sun-like stars, and surprisingly so, as they are missing in our solar system. Recent detections have yielded enough information about this class of exoplanets to begin characterizing their occurrence rates, orbits, masses, densities, and internal structures. The Kepler mission finds the smallest planets to be most common, as 26% of Sun-like stars have small, 1-2 R⊕ planets with orbital periods under 100 d, and 11% have 1-2 R⊕ planets that receive 1-4× the incident stellar flux that warms our Earth. These Earth-size planets are sprinkled uniformly with orbital distance (logarithmically) out to 0.4 the Earth-Sun distance, and probably beyond. Mass measurements for 33 transiting planets of 1-4 R⊕ show that the smallest of them, R < 1.5 R⊕, have the density expected for rocky planets. Their densities increase with increasing radius, likely caused by gravitational compression. Including solar system planets yields a relation: ρ = 2:32 + 3:19 R=R ⊕ [g cm(-3)]. Larger planets, in the radius range 1.5-4.0 R⊕, have densities that decline with increasing radius, revealing increasing amounts of low-density material (H and He or ices) in an envelope surrounding a rocky core, befitting the appellation ''mini-Neptunes.'' The gas giant planets occur preferentially around stars that are rich in heavy elements, while rocky planets occur around stars having a range of heavy element abundances. Defining habitable zones remains difficult, without benefit of either detections of life elsewhere or an understanding of life's biochemical origins.

Temperament and fracture in preschool-aged children.

OBJECTIVES: Approximately one-half of all children will sustain a fracture before adulthood. Understanding the factors that place a child at increased risk of fracture is necessary to inform effective injury prevention strategies. The purpose of this study was to examine the association between temperament and fracture risk in preschool-aged children. METHODS: Children aged 3 to 6 years who were diagnosed with a fracture were recruited from the Hospital for Sick Children Fracture Clinic. Using a retrospective case-control study design, the 148 cases were frequency-matched by age and sex to 426 controls from the TARGet Kids primary care paediatric cohort. The Childhood Behaviour Questionnaire, a 36-item caregiver response questionnaire was used to assess three of the following temperament factors: surgency (e.g., high activity level), negative affect (e.g., anger, fear, discomfort) and effortful control (e.g., attentional focusing). RESULTS: Unadjusted logistic models demonstrated no association between children with previous fracture and higher scores of surgency (unadjusted odds ratio [OR]=1.06, 95% confidence interval [CI]: 0.84, 1.34), negative affect (unadjusted OR=1.15, 95% CI: 0.93, 1.42) or effortful control (unadjusted OR=0.80, 95% CI: 0.63, 1.03). Further, models adjusted for covariates also demonstrated no significant association with surgency (1.00, 95% CI: 0.78, 1.29), negative affect (1.09, 95% CI: 0.86, 1.37) and effortful control (0.80, 95% CI: 0.61, 1.05). CONCLUSION: None of the three main temperament types identified by the Childhood Behaviour Questionnaire were associated with an increase in fracture risk.

Risk Factors of Acute Kidney Injury in Critically Ill Children.

OBJECTIVES: Acute kidney injury may be promoted by critical illness, preexisting medical conditions, and treatments received both before and during ICU admission. We aimed to estimate the frequency of acute kidney injury during ICU treatment and to determine factors, occurring both before and during the ICU stay, associated with the development of acute kidney injury. DESIGN: Cohort study of critically ill children. SETTING: University-affiliated PICU. PATIENTS: Eligible patients were admitted to the ICU between January 2006 and June 2009. We excluded those admitted with known primary renal failure, chronic renal failure or postrenal transplant, conditions with known renal complications, or metabolic conditions treated with dialysis. Patients were also excluded if they had a short ICU stay (< 6 hr) and those who had no creatinine or urine output measurements during their ICU stay. INTERVENTIONS: None. MEASUREMENTS AND MAIN RESULTS: Of the 3,865 pediatric patients who met the inclusion criteria, 915 (23.7%) developed acute kidney injury, as classified by the Risk, Injury, Failure, Loss of kidney function, and End-stage kidney disease criteria, during their ICU stay. Patients at high risk for development of acute kidney injury included those urgently admitted to the ICU (adjusted odds ratio, 1.88), those who developed respiratory dysfunction during their ICU care (adjusted odds ratio, 2.90), and those who treated with extracorporeal membrane oxygenation (adjusted odds ratio, 2.72). The single greatest risk factor for acute kidney injury was the administration of nephrotoxic medications during ICU admission (adjusted odds ratio, 3.37). CONCLUSIONS: This study, the largest evaluating the incidence of RIFLE-defined acute kidney injury in critically ill children, found that one-quarter of patients admitted to the ICU developed acute kidney injury. We identified a number of potentially modifiable risk factors, the largest of which was the administration of nephrotoxic medication. The results of this study may be used to inform targeted interventions to reduce acute kidney injury and improve the outcomes of critically ill children.

Prevalence of Earth-size planets orbiting Sun-like stars.

Determining whether Earth-like planets are common or rare looms as a touchstone in the question of life in the universe. We searched for Earth-size planets that cross in front of their host stars by examining the brightness measurements of 42,000 stars from National Aeronautics and Space Administration's Kepler mission. We found 603 planets, including 10 that are Earth size ( ) and receive comparable levels of stellar energy to that of Earth (1 - 2 R[Symbol: see text] ). We account for Kepler's imperfect detectability of such planets by injecting synthetic planet-caused dimmings into the Kepler brightness measurements and recording the fraction detected. We find that 11 ± 4% of Sun-like stars harbor an Earth-size planet receiving between one and four times the stellar intensity as Earth. We also find that the occurrence of Earth-size planets is constant with increasing orbital period (P), within equal intervals of logP up to ~200 d. Extrapolating, one finds 5.7(-2.2)(+1.7)% of Sun-like stars harbor an Earth-size planet with orbital periods of 200-400 d.