Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties
and habitability. Combining radial velocity (RV) and transit data provides additional information
on ...exoplanet physical properties. We detect a transiting rocky planet with an orbital period
of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is
2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data
and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet’s short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy.
The Musa x paradisiaca L. inflorescence, known as banana blossom or banana heart, is used in traditional medicine for the treatment of diabetes mellitus.
Aim of the study: The aim of the study was to ...investigate the antidiabetic activity of aqueous extracts and fractions prepared from the bracts and flowers of Musa x paradisiaca in streptozotocin (STZ)-induced diabetic rats and to chemically characterize the extracts.
Standard aqueous extracts of the flowers, bracts, and their fractions were prepared and their chemical composition was determined tentatively by high-performance liquid chromatography coupled to diode-array detection and mass spectrometry (HPLC-DAD-MS). Changes in fasting glycemia and oral glucose tolerance were evaluated in STZ-induced diabetic rats (n = 8) treated with aqueous extracts of Musa x paradisiaca (200 mg/kg) for 20 days.
Chemical analyses detected 21 compounds and 17 metabolites were identified, among which were glycosylated and acetylated phenylpropanoids of p-coumaric acid and caffeic acid, as well as a glycosylated flavonol and anthocyanins. Following 15 days of treatment, the bract aqueous extracts and the methanolic fraction of the flower had significant effects on the glycemic profile after glucose load in diabetic rats as compared with the untreated diabetic group.
The results of the present study show the antidiabetic potential of extracts of the flowers and bracts of M. x paradisiaca.
Display omitted
Context.
Exoplanets with orbital periods of less than one day are known as ultra-short period (USP) planets. They are relatively rare products of planetary formation and evolution processes, but ...especially favourable for characterisation with current planet detection methods. At the time of writing, 125 USP planets have already been confirmed.
Aims.
Our aim is to validate the planetary nature of two new transiting planet candidates around M dwarfs announced by the NASA Transiting Exoplanet Survey Satellite (TESS), registered as TESS Objects of Interest (TOIs) TOI-1442.01 and TOI-2445.01.
Methods.
We used TESS data, ground-based photometric light curves, and Subaru/IRD spectrograph radial velocity (RV) measurements to validate both planetary candidates and to establish their physical properties.
Results.
TOI-1442 bis a validated exoplanet with an orbital period of
P
= 0.4090682 ± 0.0000004 day, a radius of
R
p
= 1.15 ± 0.06
R
⊕
, and equilibrium temperature of
T
p,eq
= 1357
−42
+49
K. TOI-2445 b is also validated with an orbital period of
P
= 0.3711286 ± 0.0000004 day, a radius of
R
p
= 1.33 ± 0.09
R
⊕
, and equilibrium temperature of
T
p,eq
= 1330
−56
+61
K. Their physical properties align with current empirical trends and formation theories of USP planets. Based on the RV measurements, we set 3
σ
upper mass limits of 8
M
⊕
and 20
M
⊕
, thus confirming the non-stellar, sub-Jovian nature of both transiting objects. More RV measurements will be needed to constrain the planetary masses and mean densities, and the predicted presence of outer planetary companions. These targets extend the small sample of USP planets orbiting around M dwarfs up to 21 members. They are also among the 20 most suitable terrestrial planets for atmospheric characterisation via secondary eclipse with the
James Webb
Space Telescope, according to a widespread emission spectroscopy metric.
Objective
Frailty is a common geriatric syndrome, characterized by a decrease in energy reserve and stress resistance, resulting in an accumulated decline of multiple physiological systems and ...greater vulnerability. Frailty syndrome has a multifactorial etiology involving a biological basis associated with sociobehavioral factors. We verify the association of frailty syndrome with family functionality level, nutritional status and medication adherence in older adults.
Design
Observational and analytical study.
Setting and Participants
Conducted at ambulatory the university hospital, with patients aged 60 years or older.
Measurements
Cognitive function was measured using the Mini-Mental State Examination (MMSE); nutritional status was evaluated using the Mini Nutritional Assessment (MNA) and Body Mass Index, BMI; the 5-item FRAIL scale was used for frailty screening; family functioning was assessed using the Family APGAR Index, which evaluates Adaptability, Partnership, Growth, Affection, and Resolve; Self-reported medication adherence was measured by the eight-item Morisky Medication Adherence Scale (MMAS-8).
Results
The study involved 308 older adults, with a mean age of 70.40 years, There was an association between frailty and highly dysfunctional family with an OR of 5.9 (95% CI 1.9–18.5)(p<0.05), nutritional risk assessed by BMI, where low weight presented an OR of 2.5 (95% CI 1.1–5.8) and obesity an OR of 2.8 (95% CI 1.1–7.0)(P <0.05) and a nutritional risk assessed by MNA with an OR 6.3(95% CI 1.9–20.4) and low medication adherence with an OR of 8.9 (95% CI, 3.6–21.6)(P = 0.01).
Conclusion
Frailty syndrome is associated with high levels of family dysfunction, nutritional risk and poor medication adherence amongst older people.
We report the discovery and characterization of two small transiting planets orbiting the bright M3.0V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time ...series in three sectors of the TESS mission. We confirm the planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b (
P
b
= 1.88 d), has a planetary mass of
M
b
= 3.21 ± 0.24
M
⊕
and a radius of
R
b
= 1.280
−0.039
+0.038
R
⊕
, resulting in a density of
ρ
b
= 8.39
−0.92
+1.05
g cm
−3
, which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c (
P
c
= 15.53 d), we derive a mass of
M
c
= 6.64
−0.68
+0.67
M
⊕
,aradius of
R
c
= 2.06 ± 0.04
R
⊕
,
and a bulk density of
ρ
c
=
2.00
−0.19
+0.21
g cm
−3
, which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.
Portal vein thrombosis (PVT) may occur at any time following liver transplantation. We describe our experience with portal vein recanalization in cases of thrombosis after liver transplantation. ...Twenty‐eight children (5%) out of 566 liver transplant recipients underwent portal vein recanalization using a transmesenteric approach. All children received left hepatic segments, developed PVT, and had symptoms or signs of portal hypertension. Portal vein recanalization was performed via the transmesenteric route in all cases. Twenty‐two (78.6%) patients underwent successful recanalization and stent placement. They received oral anticoagulants after the procedure, and clinical symptoms subsided. Symptoms recurred due to portal vein restenosis/thrombosis in seven patients. On an intention‐to‐treat basis, the success rate of the proposed treatment was 60.7%. Only 17 out of 28 children with posttransplant chronic PVT retained stent patency (primary + assisted) at the end of the study period. In cases of portal vein obstruction, the transmesenteric approach via minilaparotomy is technically feasible with good clinical and hemodynamic results. It is an alternative procedure to reestablish the portal flow to the liver graft that can be performed in selected cases and a therapeutic addition to other treatment strategies currently used to treat chronic PVT.
The authors demonstrate the long‐term outcomes of portal vein recanalization with stent placement using a transmesenteric approach in cases of chronic portal vein thrombosis after pediatric liver transplantation.
We present the discovery and characterisation of two transiting planets observed by the Transiting Exoplanet Survey Satellite (TESS) orbiting the nearby (d⋆ ≈ 22 pc), bright (J ≈ 9 mag) M3.5 dwarf ...LTT 3780 (TOI–732). We confirm both planets and their association with LTT 3780 via ground-based photometry and determine their masses using precise radial velocities measured with the CARMENES spectrograph. Precise stellar parameters determined from CARMENES high-resolution spectra confirm that LTT 3780 is a mid-M dwarf with an effective temperature of T(eff) = 3360 ± 51 K, a surface gravity of log g⋆ = 4.81 ± 0.04 (cgs), and an iron abundance of Fe/H = 0.09 ± 0.16 dex, with an inferred mass of M⋆ = 0.379 ± 0.016M⊙ and a radius of R⋆ = 0.382 ± 0.012R⊙. The ultra-short-period planet LTT 3780 b (P(b) = 0.77 d) with a radius of 1.35(−0.06,+0.06) R⊕, a mass of 2.34(−0.23,+0.24) M⊕, and a bulk density of 5.24(−0.81,+0.94) g/cu.cm joins the population of Earth-size planets with rocky, terrestrial composition. The outer planet, LTT 3780 c, with an orbital period of 12.25 d, radius of 2.42(−0.10,+0.10) R⊕, mass of 6.29(−0.61,+0.63) M⊕, and mean density of 2.45(−0.37,+0.44) g/cu.cm belongs to the population of dense sub-Neptunes. With the two planets located on opposite sides of the radius gap, this planetary system is an excellent target for testing planetary formation, evolution, and atmospheric models. In particular, LTT 3780 c is an ideal object for atmospheric studies with the James Webb Space Telescope (JWST).
BRAF V600E is the most common mutation in cutaneous melanomas, and has been described in 30-72% of such cases. This mutation results in the substitution of valine for glutamic acid at position 600 of ...the BRAF protein, which consequently becomes constitutively activated. The present study investigated the BRAF V600E mutation frequency and its clinical implications in a group of 77 primary cutaneous melanoma patients treated in a cancer reference center in Brazil. Mutation analysis was accomplished by polymerase chain reaction, restriction fragment length polymorphism, and automated DNA sequencing. The chi-squared and Fischer exact tests were used for comparative analyses. The BRAF V600E mutation was detected in 54/77 (70.1%) melanoma subjects. However, no statistically significant association was found between the presence of the mutation and clinical or prognostic parameters. Our results demonstrated that the BRAF V600E mutation is a common event in melanomas, representing an important molecular target for novel therapeutic approaches in such tumors.
We report the discovery of a Neptune-like planet (LP 714-47 b,
P
= 4.05204 d,
m
b
= 30.8 ± 1.5
M
⊕
,
R
b
= 4.7 ± 0.3
R
⊕
) located in the “hot Neptune desert”. Confirmation of the TESS Object of ...Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS,
Spitzer
, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TÜBİTAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (
T
eff
= 3950 ± 51 K) with a mass of 0.59 ± 0.02
M
⊙
and a radius of 0.58 ± 0.02
R
⊙
. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained.
We validate the Transiting Exoplanet Survey Satellite (TESS) object of interest TOI-2266.01 (TIC 8348911) as a small transiting planet (most likely a super-Earth) orbiting a faint M5 dwarf ( V = ...16.54) on a 2.33 d orbit. The validation is based on an approach where multicolour transit light curves are used to robustly estimate the upper limit of the transiting object's radius. Our analysis uses SPOC-pipeline TESS light curves from Sectors 24, 25, 51, and 52, simultaneous multicolour transit photometry observed with MuSCAT2, MuSCAT3' and HiPERCAM, and additional transit photometry observed with the LCOGT telescopes. TOI-2266 b is found to be a planet with a radius of 1.54 ± 0.09 R ⊕ , which locates it at the edge of the transition zone between rocky planets, water-rich planets, and sub-Neptunes (the so-called M dwarf radius valley). The planet is amenable to ground-based radial velocity mass measurement with red-sensitive spectrographs installed in large telescopes, such as MAROON-X and Keck Planet Finder (KPF), which makes it a valuable addition to a relatively small population of planets that can be used to probe the physics of the transition zone. Further, the planet's orbital period of 2.33 days places it inside a ‘keystone planet’ wedge in the period-radius plane where competing planet formation scenarios make conflicting predictions on how the radius valley depends on the orbital period. This makes the planet also a welcome addition to the small population of planets that can be used to test small-planet formation scenarios around M dwarfs.
PDF
