×

Serwis używa ciasteczek ("cookies") i podobnych technologii m.in. do utrzymania sesji i w celach statystycznych. • Ustawienia przeglądarki dotyczące obsługi ciasteczek można swobodnie zmieniać. • Całkowite zablokowanie zapisu ciasteczek na dysku komputera uniemożliwi logowanie się do serwisu. • Więcej informacji: Polityka cookies OPI PIB

×

Regulamin korzystania z serwisu PBN znajduję się pod adresem: Regulamin serwisu

Szukaj wśród:
Dane publikacji

Multi-messenger Observations of a Binary Neutron Star Merger

Artykuł
Czasopismo : Astrophysical Journal Letters   Tom: 848, Zeszyt: 2, Strony: 1-59
Lech Mankiewicz [1] , Aleksander Żarnecki [2] , Rafał Opiela [1] , Arkadiusz Ćwiek , Mikołaj Ćwiok [2] , Henryk Czyrkowski [2] , Ryszard Dąbrowski [2] , G Kasprowicz , K Nawrocki , Lech Piotrowski , G Wrochna , Marcin Zaremba [2] , Tomasz Bulik [3] , Mariusz Gromadzki [3] , Łukasz Wyrzykowski [3] , Aleksandra Hamanowicz [3] , Krzysztof Rybicki [3] , Krzysztof Piotr Ulaczyk [3] , Michał Michałowski [4] , pozostałych autorów 3524 , Zbigniew Szadkowski [5]
2017-10-20 angielski
Liczba arkuszy: 1
Link do publicznie dostępnego pełnego tekstu
Identyfikatory
-
Cechy publikacji
-
  • Oryginalny artykuł naukowy
  • Zrecenzowana naukowo
Dyscypliny naukowe
-
Astronomia , Fizyka
Słowa kluczowe
-
Abstrakty ( angielski )
-
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 $\sim 1.7\,{\rm{s}}$ 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 $\,{M}_{\odot }$. 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 $\sim 40\,{\rm{Mpc}}$) 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 $\sim 9$ and $\sim 16$ 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 NGC 4993 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.
Pełny tekst
-
  1. Rodzaj tekstu: Ostateczna wersja wydawcy
  2. Licencja: Dozwolony użytek osobisty
  3. Pliki
    1. ligo17.pdf, 3 267 kB Pobierz plik
Zacytuj dokument
-