Modeling sgB[e] Circumstellar Disks

D 2017

Modeling sgB[e] Circumstellar Disks

KURFÜRST, Petr, Achim FELDMEIER and Jiří KRTIČKA

Basic information

Original name

Modeling sgB[e] Circumstellar Disks

Authors

KURFÜRST, Petr (203 Czech Republic, guarantor, belonging to the institution), Achim FELDMEIER (276 Germany) and Jiří KRTIČKA (203 Czech Republic, belonging to the institution)

Edition

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

Publisher

Astronomical Society of the Pacific

Other information

Language

English

Type of outcome

Stať ve sborníku

Field of Study

10308 Astronomy

Country of publisher

United States of America

Confidentiality degree

není předmětem státního či obchodního tajemství

Publication form

electronic version available online

RIV identification code

RIV/00216224:14310/17:00094655

Organization unit

Faculty of Science

ISBN

978-1-58381-900-5

UT WoS

000401591600003

Keywords in English

dense disks or rings; viscous heating; neutral hydrogen layers

Abstract

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.

Links

GA13-10589S, research and development project

Name: Ztráta hmoty horkých hmotných hvězd

Investor: Czech Science Foundation

Citovat

KURFÜRST, Petr, Achim FELDMEIER and 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. 508th ed. San Francisco, USA: Astronomical Society of the Pacific, 2017, p. 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 and 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}. 508th ed. San Francisco, USA: Astronomical Society of the Pacific, 2017, p.~17-22. ISBN~978-1-58381-900-5.

Detailed Information on Publication Record