Appearance of innermost stable circular orbits of accretion discs around rotating neutron stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19240%2F14%3A%230005075" target="_blank" >RIV/47813059:19240/14:#0005075 - isvavai.cz</a>

Výsledek na webu

<a href="http://www.aanda.org/articles/aa/abs/2014/04/aa23541-14/aa23541-14.html" target="_blank" >http://www.aanda.org/articles/aa/abs/2014/04/aa23541-14/aa23541-14.html</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201423541" target="_blank" >10.1051/0004-6361/201423541</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Appearance of innermost stable circular orbits of accretion discs around rotating neutron stars

Popis výsledku v původním jazyce

The innermost stable cicular orbit (IS(X)) of an accretion disc that orbits a neutron star (NS) is often assumed to be a unique prediction of general relativity. However, it has been argued that ISCO also appears around highly elliptic bodies described by Newtonian theory. In this sense, the behaviour of an ISCO around a rotating oblate neutron star is formed by the interplay between relativistic and Newtonian effects. Here we briefly explore the consequences of this interplay using a straightforward analytic approach as well as numerical models that involve modern NS equations of state. We examine the ratio K between the ISCO radius and the radius of the neutron star. We find that, with growing NS spin, the ratio K first decreases, but then starts toincrease. This non-monotonic behaviour of K can give rise to a neutron star spin interval in which ISCO appears for two very different ranges of NS mass. This may strongly affect the distribution of neutron stars that have an ISCO (ISCO-N

Název v anglickém jazyce

Appearance of innermost stable circular orbits of accretion discs around rotating neutron stars

Popis výsledku anglicky

The innermost stable cicular orbit (IS(X)) of an accretion disc that orbits a neutron star (NS) is often assumed to be a unique prediction of general relativity. However, it has been argued that ISCO also appears around highly elliptic bodies described by Newtonian theory. In this sense, the behaviour of an ISCO around a rotating oblate neutron star is formed by the interplay between relativistic and Newtonian effects. Here we briefly explore the consequences of this interplay using a straightforward analytic approach as well as numerical models that involve modern NS equations of state. We examine the ratio K between the ISCO radius and the radius of the neutron star. We find that, with growing NS spin, the ratio K first decreases, but then starts toincrease. This non-monotonic behaviour of K can give rise to a neutron star spin interval in which ISCO appears for two very different ranges of NS mass. This may strongly affect the distribution of neutron stars that have an ISCO (ISCO-N

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2014

Kód důvěrnosti údajů

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

Název periodika

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

—

Svazek periodika

564

Číslo periodika v rámci svazku

April

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

4

Strana od-do

"L5 - 1"-"L5 - 4"

Kód UT WoS článku

000334671000144

EID výsledku v databázi Scopus

—