Modeling sgB[e] Circumstellar Disks

D 2017

Modeling sgB[e] Circumstellar Disks

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA

Základní údaje

Originální název

Modeling sgB[e] Circumstellar Disks

Autoři

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

Vydání

508. vyd. San Francisco, USA, The B[e] Phenomenom: Forty Years of Studies, od s. 17-22, 6 s. 2017

Nakladatel

Astronomical Society of the Pacific

Další údaje

Jazyk

angličtina

Typ výsledku

Stať ve sborníku

Obor

10308 Astronomy

Stát vydavatele

Spojené státy

Utajení

není předmětem státního či obchodního tajemství

Forma vydání

elektronická verze "online"

Kód RIV

RIV/00216224:14310/17:00094655

Organizační jednotka

Přírodovědecká fakulta

ISBN

978-1-58381-900-5

UT WoS

000401591600003

Klíčová slova anglicky

dense disks or rings; viscous heating; neutral hydrogen layers

Štítky

NZ, rivok

Příznaky

Mezinárodní význam

Změněno: 22. 3. 2018 11:19, Ing. Nicole Zrilić

Anotace

V originále

During their evolution, massive stars are characterized by a significant loss of mass either via spherically symmetric stellar winds or by aspherical mass-loss mechanisms, namely outflowing equatorial disks. However, the scenario that leads to the formation of a disk or rings of gas and dust around these objects is still under debate. Is it a viscous disk or an ouftlowing disk-forming wind or some other mechanism? It is also unclear how various physical mechanisms that act on the circumstellar environment of the stars affect its shape, density, kinematic, and thermal structure. We assume that the disk-forming mechanism is a viscous transport within an equatorial outflowing disk of a rapidly or even critically rotating star. We study the hydrodynamic and thermal structure of optically thick dense parts of outflowing circumstellar disks that may form around, e.g., Be stars, sgB[e] stars, or Pop III stars. We calculate self-consistent time-dependent models of the inner dense region of the disk that is strongly affected either by irradiation from the central star and by contributions of viscous heating effects. We also simulate the dynamic effects of collision between expanding ejecta of supernovae and circumstellar disks that may be form in sgB[e] stars and, e.g., LBVs or Pop III stars.

Návaznosti

GA13-10589S, projekt VaV

Název: Ztráta hmoty horkých hmotných hvězd

Investor: Grantová agentura ČR, Ztráta hmoty horkých hmotných hvězd

Citovat

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA. Modeling sgB[e] Circumstellar Disks. Online. In Anatoly Miroshnichenko, Sergey Zharikov, Daniela Korčáková, Marek Wolf. The B[e] Phenomenom: Forty Years of Studies. 508. vyd. San Francisco, USA: Astronomical Society of the Pacific, 2017, s. 17-22. ISBN 978-1-58381-900-5.

@inproceedings{1374140,
   author = {Kurfürst, Petr and Feldmeier, Achim and Krtička, Jiří},
   address = {San Francisco, USA},
   booktitle = {The B[e] Phenomenom: Forty Years of Studies},
   edition = {508},
   editor = {Anatoly Miroshnichenko, Sergey Zharikov, Daniela Korčáková, Marek Wolf},
   keywords = {dense disks or rings; viscous heating; neutral hydrogen layers},
   howpublished = {elektronická verze "online"},
   language = {eng},
   location = {San Francisco, USA},
   isbn = {978-1-58381-900-5},
   pages = {17-22},
   publisher = {Astronomical Society of the Pacific},
   title = {Modeling sgB[e] Circumstellar Disks},
   year = {2017}
}

TY  - JOUR
ID  - 1374140
AU  - Kurfürst, Petr - Feldmeier, Achim - Krtička, Jiří
PY  - 2017
TI  - Modeling sgB[e] Circumstellar Disks
PB  - Astronomical Society of the Pacific
CY  - San Francisco, USA
SN  - 9781583819005
KW  - dense disks or rings
KW  - viscous heating
KW  - neutral hydrogen layers
N2  - During their evolution, massive stars are characterized by a significant loss of mass either via spherically symmetric stellar winds or by aspherical mass-loss mechanisms, namely outflowing equatorial disks. However, the scenario that leads to the formation of a disk or rings of gas and dust around these objects is still under debate. Is it a viscous disk or an ouftlowing disk-forming wind or some other mechanism? It is also unclear how various physical mechanisms that act on the circumstellar environment of the stars affect its shape, density, kinematic, and thermal structure. We assume that the disk-forming mechanism is a viscous transport within an equatorial outflowing disk of a rapidly or even critically rotating star. We study the hydrodynamic and thermal structure of optically thick dense parts of outflowing circumstellar disks that may form around, e.g., Be stars, sgB[e] stars, or Pop III stars. We calculate self-consistent time-dependent models of the inner dense region of the disk that is strongly affected either by irradiation from the central star and by contributions of viscous heating effects. We also simulate the dynamic effects of collision between expanding ejecta of supernovae and circumstellar disks that may be form in sgB[e] stars and, e.g., LBVs or Pop III stars.
ER  -

KURFÜRST, Petr, Achim FELDMEIER a Jiří KRTIČKA. Modeling sgB[e] Circumstellar Disks. Online. In Anatoly Miroshnichenko, Sergey Zharikov, Daniela Korčáková, Marek Wolf. \textit{The B[e] Phenomenom: Forty Years of Studies}. 508. vyd. San Francisco, USA: Astronomical Society of the Pacific, 2017, s.~17-22. ISBN~978-1-58381-900-5.

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