Recent results suggest that the two planets in the HD 82943 system are inclined to the sky plane by 20 ± 4°. Here, we show that the debris disc in this system is inclined by 27 ± 4°, thus adding ...strength to the derived planet inclinations and suggesting that the planets and debris disc are consistent with being aligned at a level similar to the Solar system. Further, the stellar equator is inferred to be inclined by 28 ± 4°, suggesting that the entire star-planet-disc system is aligned, the first time such alignment has been tested for radial velocity discovered planets on ∼au wide orbits. We show that the planet-disc alignment is primordial, and not the result of planetary secular perturbations to the disc inclination. In addition, we note three other systems with planets at 10 au discovered by direct imaging that already have good evidence of alignment, and suggest that empirical evidence of system-wide star-planet-disc alignment is therefore emerging, with the exception of systems that host hot Jupiters. While this alignment needs to be tested in a larger number of systems, and is perhaps unsurprising, it is a reminder that the system should be considered as a whole when considering the orientation of planetary orbits.
ABSTRACT
We observed the K7 class III star NO Lup in an ALMA survey of the 1–3 Myr Lupus association and detected circumstellar dust and CO gas. Here we show that the J = 3–2 CO emission is both ...spectrally and spatially resolved, with a broad velocity width ∼19 km s−1 for its resolved size ∼1 arcsec (∼130 au). We model the gas emission as a Keplerian disc, finding consistency, but only with a central mass of ∼11M⊙, which is implausible given its spectral type and X-Shooter spectrum. A good fit to the data can also be found by modelling the CO emission as outflowing gas with a radial velocity ∼22 km s−1. We interpret NO Lup’s CO emission as the first imaged class III circumstellar disc with outflowing gas. We conclude that the CO is continually replenished, but cannot say if this is from the breakup of icy planetesimals or from the last remnants of the protoplanetary disc. We suggest further work to explore the origin of this CO, and its higher than expected velocity in comparison to photoevaporative models.
ABSTRACT
Debris discs around main-sequence stars are belts of planetesimals – asteroids and comets – formed in the protoplanetary discs around young stars. Planetesimals comprise both the building ...blocks of planets around young stars and the source of dusty debris around older stars. Imaging observations of dust continuum emission and scattered light reveal the location of these planetesimal belts around their host stars. Analysis of debris discs observed at millimetre wavelengths revealed a trend between the discs’ radii and the host star luminosities. This trend was tentatively linked to the preferential formation of dust-producing planetesimals near snow lines (specifically CO) in the protoplanetary discs around the host stars. Here, we perform a homogeneous analysis of 95 debris discs observed at far-infrared wavelengths by the Herschel Space Observatory and fit the obtained distribution of radii and widths as a function of stellar luminosity with a power-law relation. We identify a trend in disc radius as a function of stellar luminosity similar to that identified at millimetre wavelengths, but cannot convincingly recover it from the available data set due to the large uncertainties on disc radius and width inherent in the marginally spatially resolved data, and the bias of smaller discs around more distant stars (which are also the more luminous) being omitted from our analysis. We see a trend in disc temperature as a function of stellar luminosity, consistent with previous findings from similar analyses.
ABSTRACT
We report the first characterization of the individual discs in the intermediate-separation binary systems KK Oph and HD 144668 at millimetre wavelengths. In both systems, the circumprimary ...and the circumsecondary discs are detected in the millimetre continuum emission, but not in 13CO nor C18O lines. Even though the disc structure is only marginally resolved, we find indications of large-scale asymmetries in the outer regions of the primary discs, most likely due to perturbation by the companion. The derived dust masses are firmly above debris disc level for all stars. The primaries have about three times more dust in their discs than the secondaries. In the case of HD 144668, the opacity spectral index of the primary and secondary differ by a large margin of 0.69, which may be a consequence of the secondary disc being more compact. Upper limits on the gas masses imply less than 0.1 Mjup in any of these discs, meaning that giant planets can no longer form in them. Considering that there have been no massive gas discs identified to date in intermediate-separation binaries (i.e. binaries at a few hundred au separation), this opens space for speculation whether their binarity causes the removal of gas, with tidal interaction truncating the discs and hence shortening the accretion time-scale. More systematic studies in this respect are sorely needed.
Alignment in star-debris disc systems seen by Herschel Greaves, J. S; Kennedy, G. M; Thureau, N ...
Monthly notices of the Royal Astronomical Society. Letters,
02/2014, Letnik:
438, Številka:
1
Journal Article, Web Resource
Recenzirano
Odprti dostop
Many nearby main-sequence stars have been searched for debris using the far-infrared Herschel satellite, within the DEBRIS, DUNES and Guaranteed-Time Key Projects. We discuss here 11 stars of ...spectral types A-M where the stellar inclination is known and can be compared to that of the spatially resolved dust belts. The discs are found to be well aligned with the stellar equators, as in the case of the Sun's Kuiper belt, and unlike many close-in planets seen in transit surveys. The ensemble of stars here can be fitted with a star-disc tilt of 10°. These results suggest that proposed mechanisms for tilting the star or disc in fact operate rarely. A few systems also host imaged planets, whose orbits at tens of au are aligned with the debris discs, contrary to what might be expected in models where external perturbers induce tilts.
Aim The National Training Programme in laparoscopic colorectal surgery was set up in 2008 to introduce laparoscopic colorectal surgery nationwide in a safe and structured way.
Method Over 150 ...consultant surgeons were enrolled; they received regular and supervised hands on training, and the operative outcome and the structured sign‐off process were monitored continuously.
Results Over 1000 training cases have been recorded with clinical outcomes comparable to established experts; 1/3 elective colorectal resections in England are performed laparoscopically.
Conclusion This successful and novel training model may be a training paradigm for other surgical and interventional specialities.
To identify baseline clinical and demographic characteristics associated with clinically important treatment responses in a randomized trial of nonsurgical therapies for fecal incontinence (FI).
...Women (N = 296) with FI were randomized to loperamide or placebo- and manometry-assisted biofeedback exercises or educational pamphlet in a 2 × 2 factorial design. Treatment response was defined in 3 ways from baseline to 24 weeks: minimal clinically important difference (MID) of -5 points in St. Mark's score, ≥50% reduction in FI episodes, and combined St. Mark's MID and ≥50% reduction FI episodes. Multivariable logistic regression models included baseline characteristics and treatment groups with and without controlling for drug and exercise adherence.
Treatment response defined by St. Mark's MID was associated with higher symptom severity (adjusted odds ratio aOR 1.20, 95% confidence interval CI 1.11-1.28) and being overweight vs normal/underweight (aOR 2.15, 95% CI 1.07-4.34); these predictors remained controlling for adherence. Fifty percent reduction in FI episodes was associated with the combined loperamide/biofeedback group compared with placebo/pamphlet (aOR 4.04, 95% CI 1.36-11.98), St. Mark's score in the placebo/pamphlet group (aOR 1.29, 95% CI 1.01-1.65), FI subtype of urge vs urge plus passive FI (aOR 2.39, 95% CI 1.09-5.25), and passive vs urge plus passive FI (aOR 3.26, 95% CI 1.48-7.17). Controlling for adherence, associations remained, except St. Mark's score.
Higher severity of FI symptoms, being overweight, drug adherence, FI subtype, and combined biofeedback and medication treatment were associated with clinically important treatment responses. This information may assist in counseling patients, regarding efficacy and expectations of nonsurgical treatments of FI.
Aim
Patient‐reported outcome (PRO) measures (PROMs) are standard measures in the assessment of colorectal cancer (CRC) treatment, but the range and complexity of available PROMs may be hindering the ...synthesis of evidence. This systematic review aimed to: (i) summarize PROMs in studies of CRC surgery and (ii) categorize PRO content to inform the future development of an agreed minimum ‘core’ outcome set to be measured in all trials.
Method
All PROMs were identified from a systematic review of prospective CRC surgical studies. The type and frequency of PROMs in each study were summarized, and the number of items documented. All items were extracted and independently categorized by content by two researchers into ‘health domains’, and discrepancies were discussed with a patient and expert. Domain popularity and the distribution of items were summarized.
Results
Fifty‐eight different PROMs were identified from the 104 included studies. There were 23 generic, four cancer‐specific, 11 disease‐specific and 16 symptom‐specific questionnaires, and three ad hoc measures. The most frequently used PROM was the EORTC QLQ‐C30 (50 studies), and most PROMs (n = 40, 69%) were used in only one study. Detailed examination of the 50 available measures identified 917 items, which were categorized into 51 domains. The domains comprising the most items were ‘anxiety’ (n = 85, 9.2%), ‘fatigue’ (n = 67, 7.3%) and ‘physical function’ (n = 63, 6.9%). No domains were included in all PROMs.
Conclusion
There is major heterogeneity of PRO measurement and a wide variation in content assessed in the PROMs available for CRC. A core outcome set will improve PRO outcome measurement and reporting in CRC trials.
ABSTRACT
Low-mass stars might offer today the best opportunities to detect and characterize planetary systems, especially those harbouring close-in low-mass temperate planets. Among those stars, ...TRAPPIST-1 is exceptional since it has seven Earth-sized planets, of which three could sustain liquid water on their surfaces. Here we present new and deep ALMA observations of TRAPPIST-1 to look for an exo-Kuiper belt which can provide clues about the formation and architecture of this system. Our observations at 0.88 mm did not detect dust emission, but can place an upper limit of 23 µJy if the belt is smaller than 4 au, and 0.15 mJy if resolved and 100 au in radius. These limits correspond to low dust masses of ∼10−5 to 10−2 M⊕, which are expected after 8 Gyr of collisional evolution unless the system was born with a >20 M⊕ belt of 100 km-sized planetesimals beyond 40 au or suffered a dynamical instability. This 20 M⊕ mass upper limit is comparable to the combined mass in TRAPPIST-1 planets, thus it is possible that most of the available solid mass in this system was used to form the known planets. A similar analysis of the ALMA data on Proxima Cen leads us to conclude that a belt born with a mass ≳1 M⊕ in 100 km-sized planetesimals could explain its putative outer belt at 30 au. We recommend that future characterizations of debris discs around low-mass stars should focus on nearby and young systems if possible.
Experimental and imaging studies in monkeys have outlined various long association fiber bundles within the temporoparietal region. In the present study the trajectory of the middle longitudinal ...fascicle (MdLF) has been delineated in 4 human subjects using diffusion tensor magnetic resonance imaging segmentation and tractography. The MdLF seems to extend from the inferior parietal lobule (IPL), specifically the angular gyrus, to the temporal pole remaining within the white matter of the superior temporal gyrus (STG). Comparison of the superior longitudinal fascicle II-arcuate fascicle (SLF II-AF) with the MdLF in the same subjects revealed that MdLF is located in a medial and caudal position relative to SLF II-AF and that it extends more rostrally. Given the location of MdLF between the IPL (angular gyrus) and the STG, it is suggested that MdLF could have a role in language and attention functions.
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