Фізіологічна активність оздоровлювального напою "Трускавецька кришталева, збагачена алоє". Повідомлення 2: Холеретично-абсорбційний, екскреторно-депураційний та адаптогенний ефекти

Показано, что влияние напитка “Трускавецька кришталева, збагачена алоє“ на холерез, салурез, обмен уратов и состояние адаптации имеет место, но уступает таковому эталона - биоактивной воды "Нафтуся".In rats experiments by comparativ investigations it is shown that tonic drink "Трускавецька кришталева, збагачена алоє" causes effects on cholerese, salurese, exchange of urates and adaptation less than thouse of bioactiv water Naftussya

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Shortest Path Problems on a Polyhedral Surface

We develop algorithms to compute edge sequences, Voronoi diagrams, shortest path maps, the Fréchet distance, and the diameter for a polyhedral surface. Distances on the surface are measured either by the length of a Euclidean shortest path or by link distance

Geodesic Fréchet Distance Inside a Simple Polygon

We present the first algorithm for the geodesic Fréchet distance between two polygonal curves A and B inside a simple polygon P. If A and B have total complexity N and P has complexity k, then the algorithm runs in O(k+N 2 log kN log N) expected time and O(k+N 2) space. This runtime is quite good as it is only a logarithmic factor larger than the non-geodesic Fréchet algorithm [2]. We also unveil an alluring alternative to parametric search that applies to both the non-geodesic and geodesic Fréchet distance algorithms. This randomized approach is based on a variant of red-blue intersections and is appealing due to its elegance and practical efficiency when compared to parametric search