There are several treatment proposals for the obstetric patient with pre-eclampsia, but there is limited evidence on the adequacy of standard treatment. International healthcare organisations ...recommend that hospitals or anaesthesia departments have written guidelines, protocols or recommendations for dealing with common or severe situations. We propose evidence-based recommendations for the treatment of pre-eclampsia.
A literature review was performed using several sources, bibliography databases, recommendations made by specialist societies, and reviews. Four anaesthesiologists reviewed the references selected, in order to design clinical questions (these were obtained from recent pre-eclampsia review articles). Consensus of at least 3 out of 4 experts was required. The Oxford criteria for evidence were chosen to classify the scientific articles, and the Jadad score was applied to the final articles selected.
A total of 50 clinical questions were designed and answered. These were classified into: general questions, influence of the type of delivery, pre-anaesthesia evaluation, peripartum treatment (including analgesia and anaesthesia), eclampsia, post-delivery period, and intensive care and transport. Most of the responses showed low scientific evidence.
Evidence-based recommendations for severe pre-eclampsia treatment were provided with special emphasis on the anaesthesiologist point of view.
A&A 636, A89 (2020) We report the discovery of a new planetary system with three transiting
planets, one super-Earth and two sub-Neptunes, that orbit EPIC\,249893012, a
G8\,IV-V evolved star ...($M_\star$\,=\,1.05\,$\pm$\,0.05\,$M_\odot$,
$R_\star$\,=\,1.71\,$\pm$\,0.04\,$R_\odot$,
$T_\mathrm{eff}$\,=5430\,$\pm$\,85\,K). The star is just leaving the main
sequence. We combined \ktwo \ photometry with IRCS adaptive-optics imaging and
HARPS, HARPS-N, and CARMENES high-precision radial velocity measurements to
confirm the planetary system, determine the stellar parameters, and measure
radii, masses, and densities of the three planets. With an orbital period of
$3.5949^{+0.0007}_{-0.0007}$ days, a mass of $8.75^{+1.09}_{-1.08}\ M_{\oplus}$
, and a radius of $1.95^{+0.09}_{-0.08}\ R_{\oplus}$, the inner planet b is
compatible with nickel-iron core and a silicate mantle ($\rho_b=
6.39^{+1.19}_{-1.04}$ g cm$^{-3}$). Planets c and d with orbital periods of
$15.624^{+0.001}_{-0.001}$ and $35.747^{+0.005}_{-0.005}$ days, respectively,
have masses and radii of $14.67^{+1,84}_{-1.89}\ M_{\oplus}$ and
$3.67^{+0.17}_{-0.14}\ R_{\oplus}$ and $10.18^{+2.46}_{-2.42}\ M_{\oplus}$ and
$3.94^{+0.13}_{-0.12}\ R_{\oplus}$, respectively, yielding a mean density of
$1.62^{+0.30}_{-0.29}$ and $0.91^{+0.25}_{-0.23}$ g cm$^{-3}$, respectively.
The radius of planet b lies in the transition region between rocky and gaseous
planets, but its density is consistent with a rocky composition. Its semimajor
axis and the corresponding photoevaporation levels to which the planet has been
exposed might explain its measured density today. In contrast, the densities
and semimajor axes of planets c and d suggest a very thick atmosphere. The
singularity of this system, which orbits a slightly evolved star that is just
leaving the main sequence, makes it a good candidate for a deeper study from a
dynamical point of view.
The Kepler extended mission, also known as K2, has provided the community with a wealth of planetary candidates that orbit stars typically much brighter than the targets of the original mission. ...These planet candidates are suitable for further spectroscopic follow-up and precise mass determinations, leading ultimately to the construction of empirical mass-radius diagrams. Particularly interesting is to constrain the properties of planets between the Earth and Neptune in size, the most abundant type of planets orbiting Sun-like stars with periods less than a few years. Among many other K2 candidates, we discovered a multi-planetary system around EPIC246471491, with four planets ranging in size from twice the size of Earth, to nearly the size of Neptune. We measure the mass of the planets of the EPIC246471491 system by means of precise radial velocity measurements using the CARMENES spectrograph and the HARPS-N spectrograph. With our data we are able to determine the mass of the two inner planets of the system with a precision better than 15%, and place upper limits on the masses of the two outer planets. We find that EPIC246471491b has a mass of 9.68 Me, and a radius of 2.59 Re, yielding a mean density of 3.07 g/cm3, while EPIC246471491c has a mass of 15.68 Me, radius of 3.53 Re, and a mean density of 19.5 g/cm3. For EPIC246471491d (R=2.48Re) and EPIC246471491e (R=1.95Re) the upper limits for the masses are 6.5 and 10.7 Me, respectively. The system is thus composed of a nearly Neptune-twin planet (in mass and radius), two sub-Neptunes with very different densities and presumably bulk composition, and a fourth planet in the outermost orbit that resides right in the middle of the super-Earth/sub-Neptune radius gap. Future comparative planetology studies of this system can provide useful insights into planetary formation, and also a good test of atmospheric escape and evolution theories.
We report the discovery of a new planetary system with three transiting planets, one super-Earth and two sub-Neptunes, that orbit EPIC\,249893012, a G8\,IV-V evolved star ...(\(M_\star\)\,=\,1.05\,\(\pm\)\,0.05\,\(M_\odot\), \(R_\star\)\,=\,1.71\,\(\pm\)\,0.04\,\(R_\odot\), \(T_\mathrm{eff}\)\,=5430\,\(\pm\)\,85\,K). The star is just leaving the main sequence. We combined \ktwo \ photometry with IRCS adaptive-optics imaging and HARPS, HARPS-N, and CARMENES high-precision radial velocity measurements to confirm the planetary system, determine the stellar parameters, and measure radii, masses, and densities of the three planets. With an orbital period of \(3.5949^{+0.0007}_{-0.0007}\) days, a mass of \(8.75^{+1.09}_{-1.08}\ M_{\oplus}\) , and a radius of \(1.95^{+0.09}_{-0.08}\ R_{\oplus}\), the inner planet b is compatible with nickel-iron core and a silicate mantle (\(\rho_b= 6.39^{+1.19}_{-1.04}\) g cm\(^{-3}\)). Planets c and d with orbital periods of \(15.624^{+0.001}_{-0.001}\) and \(35.747^{+0.005}_{-0.005}\) days, respectively, have masses and radii of \(14.67^{+1,84}_{-1.89}\ M_{\oplus}\) and \(3.67^{+0.17}_{-0.14}\ R_{\oplus}\) and \(10.18^{+2.46}_{-2.42}\ M_{\oplus}\) and \(3.94^{+0.13}_{-0.12}\ R_{\oplus}\), respectively, yielding a mean density of \(1.62^{+0.30}_{-0.29}\) and \(0.91^{+0.25}_{-0.23}\) g cm\(^{-3}\), respectively. The radius of planet b lies in the transition region between rocky and gaseous planets, but its density is consistent with a rocky composition. Its semimajor axis and the corresponding photoevaporation levels to which the planet has been exposed might explain its measured density today. In contrast, the densities and semimajor axes of planets c and d suggest a very thick atmosphere. The singularity of this system, which orbits a slightly evolved star that is just leaving the main sequence, makes it a good candidate for a deeper study from a dynamical point of view.
We present the discovery and characterization of a new transiting planet from Campaign 17 of the Kepler extended mission K2. HD 119130 b is a warm sub-Neptune on a 17-d orbit around a bright (V = 9.9 ...mag) solar-like G3 V star with a mass and radius of \(M_\star = 1.00\pm0.03\,\mathrm{M_\odot}\) and \(R_\star = 1.09\pm0.03\,\mathrm{R_\odot}\), respectively. We model simultaneously the K2 photometry and CARMENES spectroscopic data and derive a radius of \(R_\mathrm{p} = 2.63_{-0.10}^{+0.12}\,\mathrm{R_\oplus}\) and mass of \(M_\mathrm{p} = 24.5_{-4.4}^{+4.4}\,\mathrm{M_\oplus}\), yielding a mean density of \(\rho_\mathrm{p} = 7.4_{-1.5}^{+1.6}\,\mathrm{g\,cm^{-3}}\), which makes it one of the densest sub-Neptune planets known to date. We also detect a linear trend in radial velocities of HD 119130 (\(\dot{\gamma}_{\rm RV}= -0.40^{+0.07}_{-0.07}\,\mathrm{m\,s^{-1}\,d^{-1}}\)) that suggests a long-period companion with a minimum mass on the order of \(33\,\mathrm{M_\oplus}\). If confirmed, it would support a formation scenario of HD 119130 b by migration caused by Kozai-Lidov oscillations.
We report the detection of a transiting Earth-size planet around GJ 357, a nearby M2.5V star, using data from the Transiting Exoplanet Survey Satellite (TESS). GJ 357 b (TOI-562.01) is a transiting, ...hot, Earth-sized planet (Teq=525+-11 K) with a radius of Rb=1.217+-0.084 Re and an orbital period of Pb=3.93 d. Precise stellar radial velocities from CARMENES and PFS, as well as archival data from HIRES, UVES, and HARPS also display a 3.93-day periodicity, confirming the planetary nature and leading to a planetary mass of Mb=1.84+-0.31 Me. In addition to the radial velocity signal for GJ 357 b, more periodicities are present in the data indicating the presence of two further planets in the system: GJ 357 c, with a minimum mass of Mc=3.40+-0.46 Me in a 9.12 d orbit, and GJ 357 d, with a minimum mass of Md=6.1+-1.0 Me in a 55.7 d orbit inside the habitable zone. The host is relatively inactive and exhibits a photometric rotation period of Prot=78+-2 d. GJ 357 b is to date the second closest transiting planet to the Sun, making it a prime target for further investigations such as transmission spectroscopy. Therefore, GJ 357 b represents one of the best terrestrial planets suitable for atmospheric characterization with the upcoming JWST and ground-based ELTs.
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_star = 0.379 +/- 0.016 M_sun and a radius of R_star = 0.382 +/- 0.012 R_sun. The ultra-short-period planet LTT 3780 b (P_b = 0.77 d) with a radius of 1.35^{+0.06}_{-0.06} R_earth, a mass of 2.34^{+0.24}_{-0.23} M_earth, and a bulk density of 5.24^{+0.94}_{-0.81} g cm^{-3} 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_earth, mass of 6.29^{+0.63}_{-0.61} M_earth, and mean density of 2.45^{+0.44}_{-0.37} g cm^{-3} 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.
