A fast spinning magnetic white dwarf in the double degenerate, super-Chandrasekhar system NLTT 12758

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00479176" target="_blank" >RIV/67985815:_____/17:00479176 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/17:00099896

Výsledek na webu

<a href="http://dx.doi.org/10.1093/mnras/stw3149" target="_blank" >http://dx.doi.org/10.1093/mnras/stw3149</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stw3149" target="_blank" >10.1093/mnras/stw3149</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A fast spinning magnetic white dwarf in the double degenerate, super-Chandrasekhar system NLTT 12758

Popis výsledku v původním jazyce

We present an analysis of the close double degenerate NLTT 12758, which is comprised of a magnetic white dwarf with a field of about 3.1 MG and an apparently non-magnetic white dwarf. We measured an orbital period of 1.154 d and found that the magnetic white dwarf is spinning around its axis with a period of 23 min. An analysis of the atmospheric parameters has revealed that the cooling ages of the two white dwarfs are comparable, suggesting that they formed within a short period of time from each other. Our modelling indicates that the non-magnetic white dwarf is more massive (M = 0.83M(circle dot)) than its magnetic companion (M = 0.69M(circle dot)) and that the total mass of the system is higher than the Chandrasekhar mass. Although the stars will not come into contact over a Hubble time, when they do come into contact, dynamically unstable mass transfer will take place leading to either an accretion induced collapse into a rapidly spinning neutron star or a Type Ia supernova.

Název v anglickém jazyce

A fast spinning magnetic white dwarf in the double degenerate, super-Chandrasekhar system NLTT 12758

Popis výsledku anglicky

We present an analysis of the close double degenerate NLTT 12758, which is comprised of a magnetic white dwarf with a field of about 3.1 MG and an apparently non-magnetic white dwarf. We measured an orbital period of 1.154 d and found that the magnetic white dwarf is spinning around its axis with a period of 23 min. An analysis of the atmospheric parameters has revealed that the cooling ages of the two white dwarfs are comparable, suggesting that they formed within a short period of time from each other. Our modelling indicates that the non-magnetic white dwarf is more massive (M = 0.83M(circle dot)) than its magnetic companion (M = 0.69M(circle dot)) and that the total mass of the system is higher than the Chandrasekhar mass. Although the stars will not come into contact over a Hubble time, when they do come into contact, dynamically unstable mass transfer will take place leading to either an accretion induced collapse into a rapidly spinning neutron star or a Type Ia supernova.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

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)

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Svazek periodika

466

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

13

Strana od-do

1127-1139

Kód UT WoS článku

000398112400078

EID výsledku v databázi Scopus

2-s2.0-85018239838