Intrinsic polarization of Wolf-Rayet stars due to the
rotational modulation of the stellar wind

J 2022

Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind

ABDELLAOUI, Slah, Jiří KRTIČKA a Petr KURFÜRST

Základní údaje

Originální název

Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind

Autoři

ABDELLAOUI, Slah (788 Tunisko, garant, domácí), Jiří KRTIČKA (203 Česká republika, domácí) a Petr KURFÜRST (203 Česká republika, domácí)

Vydání

Astronomy & Astrophysics, Les Ulis, EDP Sciences, 2022, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 6.500

Kód RIV

RIV/00216224:14310/22:00125048

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1051/0004-6361/202141732

UT WoS

000747994100001

Klíčová slova anglicky

stars: Wolf-Rayet; stars: rotation; polarization; stars: winds; outflows

Štítky

rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 1. 6. 2022 15:32, Mgr. Marie Šípková, DiS.

Anotace

V originále

Fast rotating Wolf-Rayet stars are expected to be progenitors of long duration gamma-ray bursts. However, the observational test of this model is problematic. Spectral lines of Wolf-Rayet stars originate in expanding stellar wind, therefore a reliable spectroscopical determination of their rotational velocities is difficult. Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind may provide an indirect way to determine the rotational velocities of these stars. However, detailed wind models are required for this purpose. We determine the intrinsic polarization of Wolf-Rayet stars from hydrodynamical wind models as a function of rotational velocity. We used 2.5D hydrodynamical simulations to calculate the structure of rotating winds of Wolf-Rayet stars. The simulations account for the deformation of the stellar surface due to rotation, gravity darkening, and nonradial forces. From the derived models, we calculated the intrinsic stellar polarization. The mass loss rate was scaled to take realistic wind densities of Wolf-Rayet stars into account. The hydrodynamical wind models predict a prolate wind structure, which leads to a relatively low level of polarization. Even relatively large rotational velocities are allowed by observational constrains. The obtained wind structure is similiar to that obtained previously for rotating optically thin winds. Derived upper limits of rotational velocities of studied Wolf-Rayet stars are not in conflict with the model of long duration gamma-ray bursts

Návaznosti

LM2010005, projekt VaV

Název: Velká infrastruktura CESNET (Akronym: VI CESNET)

Investor: Ministerstvo školství, mládeže a tělovýchovy ČR, Velká infrastruktura CESNET

Citovat

ABDELLAOUI, Slah, Jiří KRTIČKA a Petr KURFÜRST. Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind. Astronomy & Astrophysics. Les Ulis: EDP Sciences, 2022, roč. 658, February, s. 1-7. ISSN 0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/202141732.

@article{1803637,
   author = {Abdellaoui, Slah and Krtička, Jiří and Kurfürst, Petr},
   article_location = {Les Ulis},
   article_number = {February},
   doi = {http://dx.doi.org/10.1051/0004-6361/202141732},
   keywords = {stars: Wolf-Rayet; stars: rotation; polarization; stars: winds; outflows},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy & Astrophysics},
   title = {Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind},
   url = {https://ui.adsabs.harvard.edu/abs/2022A&A...658A..46A},
   volume = {658},
   year = {2022}
}

TY  - JOUR
ID  - 1803637
AU  - Abdellaoui, Slah - Krtička, Jiří - Kurfürst, Petr
PY  - 2022
TI  - Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind
JF  - Astronomy & Astrophysics
VL  - 658
IS  - February
SP  - 1-7
EP  - 1-7
PB  - EDP Sciences
SN  - 00046361
KW  - stars: Wolf-Rayet
KW  - stars: rotation
KW  - polarization
KW  - stars: winds
KW  - outflows
UR  - https://ui.adsabs.harvard.edu/abs/2022A&A...658A..46A
N2  - Fast rotating Wolf-Rayet stars are expected to be progenitors of long duration gamma-ray bursts. However, the observational test of this model is problematic. Spectral lines of Wolf-Rayet stars originate in expanding stellar wind, therefore a reliable spectroscopical determination of their rotational velocities is difficult. Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind may provide an indirect way to determine the rotational velocities of these stars. However, detailed wind models are required for this purpose. We determine the intrinsic polarization of Wolf-Rayet stars from hydrodynamical wind models as a function of rotational velocity. We used 2.5D hydrodynamical simulations to calculate the structure of rotating winds of Wolf-Rayet stars. The simulations account for the deformation of the stellar surface due to rotation, gravity darkening, and nonradial forces. From the derived models, we calculated the intrinsic stellar polarization. The mass loss rate was scaled to take realistic wind densities of Wolf-Rayet stars into account. The hydrodynamical wind models predict a prolate wind structure, which leads to a relatively low level of polarization. Even relatively large rotational velocities are allowed by observational constrains. The obtained wind structure is similiar to that obtained previously for rotating optically thin winds. Derived upper limits of rotational velocities of studied Wolf-Rayet stars are not in conflict with the model of long duration gamma-ray bursts
ER  -

ABDELLAOUI, Slah, Jiří KRTIČKA a Petr KURFÜRST. Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind. \textit{Astronomy \&{} Astrophysics}. Les Ulis: EDP Sciences, 2022, roč.~658, February, s.~1-7. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/202141732.

Podrobný výpis o publikaci