No abstract available

[en] Although the Transiting Exoplanet Survey Satellite (TESS) primary mission observed the northern and southern ecliptic hemispheres, generally avoiding the ecliptic, and the Kepler space telescope during the K2 mission could only observe near the ecliptic, many of the K2 fields extend far enough from the ecliptic plane that sections overlap with TESS fields. Using photometric observations from both K2 and TESS, combined with archival spectroscopic observations, we globally modeled four known planetary systems discovered by K2 that were observed in the first year of the primary TESS mission. Specifically, we provide updated ephemerides and system parameters for K2-114 b, K2-167 b, K2-237 b, and K2-261 b. These were some of the first K2 planets to be observed by TESS in the first year and include three Jovian sized planets and a sub-Neptune with orbital periods less than 12 days. In each case, the updated ephemeris significantly reduces the uncertainty in prediction of future times of transit, which is valuable for planning observations with the James Webb Space Telescope and other future facilities. The TESS extended mission is expected to observe about half of the K2 fields, providing the opportunity to perform this type of analysis on a larger number of systems.

[en] The rapid release of accurate sky localization for gravitational-wave (GW) candidates is crucial for multi-messenger observations. During the third observing run of Advanced LIGO and Advanced Virgo, automated GW alerts were publicly released within minutes of detection. Subsequent inspection and analysis resulted in the eventual retraction of a fraction of the candidates. Updates could be delayed by up to several days, sometimes issued during or after exhaustive multi-messenger follow-up campaigns. We introduce GWSkyNet, a real-time framework to distinguish between astrophysical events and instrumental artifacts using only publicly available information from the LIGO-Virgo open public alerts. This framework consists of a non-sequential convolutional neural network involving sky maps and metadata. GWSkyNet achieves a prediction accuracy of 93.5% on a testing data set.

[en] Aiming to solve the problems of low accuracy of multi-step prediction and difficulty in determining the maximum number of prediction steps of chaotic time series, a multi-step time series prediction model based on the dilated convolution network and long short-term memory (LSTM), named the dilated convolution-long short-term memory (DC-LSTM), is proposed. The dilated convolution operation is used to extract the correlation between the predicted variable and correlational variables. The features extracted by dilated convolution operation and historical data of predicted variable are input into LSTM to obtain the desired multi-step prediction result. Furthermore, cross-correlation analyses (CCA) are applied to calculate the reasonable maximum prediction steps of chaotic time series. Actual applications of multi-step prediction were studied to demonstrate the effectiveness of the proposed model which has superiorities in RMSE, MAE and prediction accuracy because of the extraction of correlation between the predicted variable and correlational variables. Moreover, the proposed DC-LSTM model provides a new method for prediction of chaotic time series and lays a foundation for scientific data analysis of chaotic time series monitoring systems.

[en] The Chinese 13. five-year plan that covers the 2016-2020 years expects a progressive capping of the global energy consumption and the deployment of efficient carbon-free technologies among which nuclear power. Since the mid 1980's China has been developing an ambitious program for the construction of second-generation pressurized water reactor. The Fukushima accident made China turn to third-generation reactors. China has developed its own third-generation PWR-type reactor: the Hualong-1. China wants to reach a 10% nuclear share in power production by 2030 instead of 4.8% end 2019. The construction of 6 to 8 new reactors will be launched each year. This growth will require more and more uranium while only one third of today's needs is covered by its own mines. Chinese authorities are negotiating with the Orano company the purchase of a turnkey reprocessing plant for the recycling of spent fuels. In China nuclear projects deal not only with power production but also with industrial heat production, hydrogen production or seawater desalting. (A.C.)

[en] Highlights: • Radiomics models of MK and MD were imaging biomarkers for predicting IDH and MGMTmet genotypes. • Combined model improved to predict IDH, which showed the incremental value of radiomics features. • Combined model did not improve predictive performance of MGMTmet. - Abstract: Purpose: To test whether the whole-tumor radiomics analysis of DKI and DTI images could predict IDH and MGMTmet genotypes of astrocytomas.

[en] Multilayer systems are coupled networks characterized by different contexts (layers) of interaction and have gained much attention recently due to their suitability to describe a broad spectrum of empirical complex systems. They are very fragile to percolation and first-neighbor failure propagation, but little is known about how they respond to non-local disruptions, as it occurs in failures induced by flow redistribution, for example. Acknowledging that many socio-technical and biological systems sustain a flow of some physical quantity, such as energy or information, across the their components, it becomes crucial to understand when the flow redistribution can cause global cascades of failures in order to design robust systems, to increase their resilience or to learn how to efficiently dismantle them. In this paper we study the impact that different multiplex topological features have on the robustness of the system when subjected to non-local cascade propagation. We first numerically demonstrate that this dynamics has a critical value at which a small initial perturbation effectively dismantles the entire network, and that the transition appears abruptly. Then we identify that the excess of flow caused by a failure is, in general, more homogeneously distributed the networks in which the average distance between nodes is small. Using this information we find that aggregated versions of multiplex networks tend to overestimate robustness, even though to make the system more robust can be achieved by increasing the number of layers. Our predictions are confirmed by simulated cascading failures in a real multilayer system. (paper)

[en] We present spectroscopy and orbital periods P _orb for 30 apparently nonmagnetic cataclysmic binaries with periods below ∼3 hr, nearly all of which are dwarf novae, mostly of the SU Ursae Majoris subclass. We then turn to the evidence supporting the prediction that short-period dwarf novae evolve toward longer periods after passing through a minimum period—the “period bounce” phenomenon. Plotting data from the literature reveals that for superhump period excess ϵ = (P _sh − P _orb)/P _orb below ∼0.015, the period appears to increase with decreasing ϵ, agreeing at least qualitatively with the predicted behavior. Next, motivated by the long (decadal) outburst intervals of the WZ Sagittae subclass of short-period dwarf novae, we ask whether there could be a sizable population of “lurkers”—systems that resemble dwarf novae at minimum light, but which do not outburst over accessible timescales (or at all) and therefore do not draw attention to themselves. By examining the outburst history of the Sloan Digital Sky Survey sample of CVs, which were selected by color and not by outburst, we find that a large majority of the color-selected dwarf-nova-like objects have been observed to outburst, and we conclude that “lurkers,” if they exist, are a relatively minor part of the CV population.

[en] Supernovae (SNe) drive multiphase galactic outflows, impacting galaxy formation; however, cosmological simulations mostly use ad hoc feedback models for outflows, making outflow-related predictions from first principles problematic. Recent small-box simulations resolve individual SNe remnants in the interstellar medium (ISM), naturally driving outflows and permitting a determination of the wind loading factors of energy η _E, mass ${\mathrm{\eta <!--\; ??\; -->}}_m$, and metals ${\mathrm{\eta <!--\; ??\; -->}}_Z$. In this Letter, we compile small-box results, and find consensus that the hot outflows are much more powerful than the cool outflows: (i) hot outflows generally dominate the energy flux, and (ii) their specific energy e _s,h is 10–1000 times higher than cool outflows. Moreover, the properties of hot outflows are remarkably simple: $e_{s,h}\propto <!--\; ???\; -->{\mathrm{\eta <!--\; ??\; -->}}_{E,h}/{\mathrm{\eta <!--\; ??\; -->}}_{m,h}$ is almost invariant over four orders of magnitude of star formation surface density. Also, we find tentatively that ${\mathrm{\eta <!--\; ??\; -->}}_{E,h}/{\mathrm{\eta <!--\; ??\; -->}}_{Z,h}\sim <!--\; ???\; -->$ 0.5. If corroborated by more simulation data, these correlations reduce the three hot phase loading factors into one. Finally, this one parameter is closely related to whether the ISM has a “breakout” condition. The narrow range of $e_{s,h}$ indicates that hot outflows cannot escape dark matter halos with log $M_{\mathrm{h}\mathrm{a}\mathrm{l}\mathrm{o}}[M_{\odot <!--\; ???\; -->}]\gtrsim <!--\; ???\; -->12$. This mass is also where the galaxy mass–metallicity relation reaches its plateau, implying a deep connection between hot outflows and galaxy formation. We argue that hot outflows should be included explicitly in cosmological simulations and (semi-)analytic modeling of galaxy formation.

[en] Models for black hole (BH) formation from stellar evolution robustly predict the existence of a pair-instability supernova (PISN) mass gap in the range ∼50 to ∼120 solar masses. This theoretical prediction is supported by the binary black holes (BBHs) of LIGO/Virgo’s first two observing runs, whose component masses are well fit by a power law with a maximum mass cutoff at $m_{max}={40.8}_{-<!--\; ???\; -->4.4}^{+11.8}{M}_{\odot <!--\; ???\; -->}$. Meanwhile, the BBH event GW190521 has a reported primary mass of $m_1={85}_{-<!--\; ???\; -->14}^{+21}{M}_{\odot <!--\; ???\; -->}$, firmly above the inferred $m_{max}$, and secondary mass $m_2={66}_{-<!--\; ???\; -->18}^{+17}{M}_{\odot <!--\; ???\; -->}$. Rather than concluding that both components of GW190521 belong to a new population of mass-gap BHs, we explore the conservative scenario in which GW190521's secondary mass belongs to the previously observed population of BHs. We replace the default priors on m ₁ and m ₂, which assume that BH detector-frame masses are uniformly distributed, with this population-informed prior on m ₂, finding $m_2<<!--\; <\; -->48M_{\odot <!--\; ???\; -->}$ at 90% credibility. Moreover, because the total mass of the system is better constrained than the individual masses, the population prior on m ₂ automatically increases the inferred m ₁ to sit above the gap (39% for m ₁ > 120 $M_{\odot <!--\; ???\; -->}$, or 25% probability for m ₁ > 130 $M_{\odot <!--\; ???\; -->}$). As long as the prior odds for a double-mass-gap BBH are smaller than $\sim <!--\; ???\; -->1:15$, it is more likely that GW190521 straddles the pair-instability gap. We argue that GW190521 may be the first example of a straddling binary black hole, composed of a conventional stellar mass BH and a BH from the “far side” of the PISN mass gap.