Collisions of Neutron Stars with Primordial Black Holes as Fast Radio Bursts Engines

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19240%2F18%3AA0000283" target="_blank" >RIV/47813059:19240/18:A0000283 - isvavai.cz</a>

Výsledek na webu

<a href="https://iopscience.iop.org/article/10.3847/1538-4357/aae64a/meta" target="_blank" >https://iopscience.iop.org/article/10.3847/1538-4357/aae64a/meta</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/aae64a" target="_blank" >10.3847/1538-4357/aae64a</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Collisions of Neutron Stars with Primordial Black Holes as Fast Radio Bursts Engines

Popis výsledku v původním jazyce

If primordial black holes (PBH) with masses of 10^{25} g greater than or similar to m greater than or similar to 10^{17} g constitute a non-negligible fraction of galactic dark-matter halos, their existence should have observable consequences: they necessarily collide with galactic neutron stars (NS), nest in their centers, and accrete the dense matter, eventually converting them to NS-mass black holes while releasing the NS magnetic field energy. Such processes may explain the fast radio bursts (FRB) phenomenology, in particular their millisecond durations, large luminosities similar to 10^{43} erg s^{-1}, high rate of occurrence greater than or similar to 1000 day^{-1}, as well as high brightness temperatures, polarized emission, and Faraday rotation. Longer than the dynamical timescale of the Bondi-like accretion for light PBH allows for the repeating of FRB. This explanation follows naturally from the (assumed) existence of the dark-matter PBH and requires no additional unusual phenomena, in particular no unacceptably large magnetic fields of NS. In our model, the observed rate of FRB throughout the universe follows from the presently known number of NS in the Galaxy.

Název v anglickém jazyce

Collisions of Neutron Stars with Primordial Black Holes as Fast Radio Bursts Engines

Popis výsledku anglicky

If primordial black holes (PBH) with masses of 10^{25} g greater than or similar to m greater than or similar to 10^{17} g constitute a non-negligible fraction of galactic dark-matter halos, their existence should have observable consequences: they necessarily collide with galactic neutron stars (NS), nest in their centers, and accrete the dense matter, eventually converting them to NS-mass black holes while releasing the NS magnetic field energy. Such processes may explain the fast radio bursts (FRB) phenomenology, in particular their millisecond durations, large luminosities similar to 10^{43} erg s^{-1}, high rate of occurrence greater than or similar to 1000 day^{-1}, as well as high brightness temperatures, polarized emission, and Faraday rotation. Longer than the dynamical timescale of the Bondi-like accretion for light PBH allows for the repeating of FRB. This explanation follows naturally from the (assumed) existence of the dark-matter PBH and requires no additional unusual phenomena, in particular no unacceptably large magnetic fields of NS. In our model, the observed rate of FRB throughout the universe follows from the presently known number of NS in the Galaxy.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA17-16287S" target="_blank" >GA17-16287S: Oscilace a koherentní jevy v akrečních discích kolem kompaktních objektů a jejich observační podpisy</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2018

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

868

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

7

Strana od-do

„17-1“-„17-7“

Kód UT WoS článku

000450221800017

EID výsledku v databázi Scopus

2-s2.0-85057199875