Two-dimensional modeling of density and thermal structure of
dense circumstellar outflowing disks

J 2018

Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA

Základní údaje

Originální název

Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks

Autoři

KURFÜRST, Petr (203 Česká republika, garant, domácí), Achim FELDMEIER (276 Německo) a Jiří KRTIČKA (203 Česká republika, domácí)

Vydání

Astronomy and Astrophysics, Les Ulis, EDP Sciences, 2018, 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: 4.378 v roce 2014

Kód RIV

RIV/00216224:14310/18:00113946

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1051/0004-6361/201731300

UT WoS

000434420000001

Klíčová slova anglicky

stars: massive; stars: mass-loss; stars: winds-outflows; stars: evolution; stars: rotation; hydrodynamics

Štítky

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 29. 4. 2021 11:07, Mgr. Marie Šípková, DiS.

Anotace

V originále

Context. Evolution of massive stars is affected by a significant loss of mass either via (nearly) spherically symmetric stellar winds or by aspherical mass-loss mechanisms, namely the outflowing equatorial disks. However, the scenario that leads to the formation of a disk or rings of gas and dust around massive stars is still under debate. Aims. We study the hydrodynamic and thermal structure of optically thick, dense parts of outflowing circumstellar disks that may be formed around various types of critically rotating massive stars, for example, Be stars, B[e] supergiant (sgB[e]) stars or Pop III stars. Methods. We specify the optical depth of the disk along the line-of-sight from stellar poles. Within the optically thick dense region we calculate the vertical disk thermal structure using the diffusion approximation while for the optically thin outer layers we assume a local thermodynamic equilibrium with the impinging stellar irradiation. We use two of our own types of hydrodynamic codes: two-dimensional operator-split numerical code and unsplit code based on the Roe's method. Results. Our models show the geometric distribution and contribution of viscous heating that begins to dominate in the central part of the disk. In the models of dense viscous disks the viscosity increases the central temperature up to several tens of thousands of Kelvins. The high mass-loss rates and high viscosity lead to instabilities with significant waves or bumps in density and temperature in the very inner disk region. Conclusions. The two-dimensional radial-vertical models of dense outflowing disks including the full Navier-Stokes viscosity terms show very high temperatures that are however limited to only the central disk cores inside the optically thick area, while near the edge of the optically thick region the temperature may be low enough for the existence of neutral hydrogen.

Návaznosti

GA16-01116S, projekt VaV

Název: Atmosféry a okolohvězdné prostředí magnetických horkých hvězd

Investor: Grantová agentura ČR, Atmosféry a okolohvězdné prostředí magnetických horkých hvězd

LM2010005, projekt VaV

Název: Velká infrastruktura CESNET (Akronym: VI CESNET)

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

Citovat

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA. Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks. Astronomy and Astrophysics. Les Ulis: EDP Sciences, 2018, roč. 613, May 2018, s. 1-24. ISSN 0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201731300.

@article{1398835,
   author = {Kurfürst, Petr and Feldmeier, Achim and Krtička, Jiří},
   article_location = {Les Ulis},
   article_number = {May 2018},
   doi = {http://dx.doi.org/10.1051/0004-6361/201731300},
   keywords = {stars: massive; stars: mass-loss; stars: winds-outflows; stars: evolution; stars: rotation; hydrodynamics},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks},
   url = {http://adsabs.harvard.edu/abs/2017arXiv171202908K},
   volume = {613},
   year = {2018}
}

TY  - JOUR
ID  - 1398835
AU  - Kurfürst, Petr - Feldmeier, Achim - Krtička, Jiří
PY  - 2018
TI  - Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks
JF  - Astronomy and Astrophysics
VL  - 613
IS  - May 2018
SP  - 1-24
EP  - 1-24
PB  - EDP Sciences
SN  - 00046361
KW  - stars: massive
KW  - stars: mass-loss
KW  - stars: winds-outflows
KW  - stars: evolution
KW  - stars: rotation
KW  - hydrodynamics
UR  - http://adsabs.harvard.edu/abs/2017arXiv171202908K
L2  - http://adsabs.harvard.edu/abs/2017arXiv171202908K
N2  - Context. Evolution of massive stars is affected by a significant loss of mass either via (nearly) spherically symmetric stellar winds or by aspherical mass-loss mechanisms, namely the outflowing equatorial disks. However, the scenario that leads to the formation of a disk or rings of gas and dust around massive stars is still under debate. Aims. We study the hydrodynamic and thermal structure of optically thick, dense parts of outflowing circumstellar disks that may be formed around various types of critically rotating massive stars, for example, Be stars, B[e] supergiant (sgB[e]) stars or Pop III stars. Methods. We specify the optical depth of the disk along the line-of-sight from stellar poles. Within the optically thick dense region we calculate the vertical disk thermal structure using the diffusion approximation while for the optically thin outer layers we assume a local thermodynamic equilibrium with the impinging stellar irradiation. We use two of our own types of hydrodynamic codes: two-dimensional operator-split numerical code and unsplit code based on the Roe's method. Results. Our models show the geometric distribution and contribution of viscous heating that begins to dominate in the central part of the disk. In the models of dense viscous disks the viscosity increases the central temperature up to several tens of thousands of Kelvins. The high mass-loss rates and high viscosity lead to instabilities with significant waves or bumps in density and temperature in the very inner disk region. Conclusions. The two-dimensional radial-vertical models of dense outflowing disks including the full Navier-Stokes viscosity terms show very high temperatures that are however limited to only the central disk cores inside the optically thick area, while near the edge of the optically thick region the temperature may be low enough for the existence of neutral hydrogen.
ER  -

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA. Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks. \textit{Astronomy and Astrophysics}. Les Ulis: EDP Sciences, 2018, roč.~613, May 2018, s.~1-24. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201731300.

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