Low-metallicity massive single stars with rotation II.
Predicting spectra and spectral classes of chemically
homogeneously evolving stars

J 2019

Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars

KUBATOVA, B.; D. SZECSI; A. A. C. SANDER; J. KUBAT; F. TRAMPER et al.

Základní údaje

Originální název

Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars

Autoři

KUBATOVA, B.; D. SZECSI; A. A. C. SANDER; J. KUBAT; F. TRAMPER; Jiří KRTIČKA; C. KEHRIG; W. R. HAMANN; R. HAINICH a T. SHENAR

Vydání

Astronomy and Astrophysics, LES ULIS CEDEX A, EDP SCIENCES S A, 2019, 1432-0746

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

Označené pro přenos do RIV

Ano

Kód RIV

RIV/00216224:14310/19:00107949

Organizační jednotka

Přírodovědecká fakulta

Klíčová slova anglicky

stars: massive; stars: winds outflows; stars: rotation; galaxies: dwarf; radiative transfer

Štítky

rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 28. 3. 2020 13:14, Mgr. Marie Novosadová Šípková, DiS.

Anotace

ORIG CZ

V originále

Context. Metal-poor massive stars are assumed to be progenitors of certain supernovae, gamma-ray bursts, and compact object mergers that might contribute to the early epochs of the Universe with their strong ionizing radiation. However, this assumption remains mainly theoretical because individual spectroscopic observations of such objects have rarely been carried out below the metallicity of the Small Magellanic Cloud. Aims. Here we explore the predictions of the state-of-the-art theories of stellar evolution combined with those of stellar atmospheres about a certain type of metal-poor (0.02 Z(circle dot)) hot massive stars, the chemically homogeneously evolving stars that we call Transparent Wind Ultraviolet INtense (TWUIN) stars. Methods. We computed synthetic spectra corresponding to a broad range in masses (20 130 M-circle dot) and covering several evolutionary phases from the zero-age main-sequence up to the core helium-burning stage. We investigated the influence of mass loss and wind clumping on spectral appearance and classified the spectra according to the Morgan-Keenan (MK) system. Results. We find that TWUIN stars show almost no emission lines during most of their core hydrogen-burning lifetimes. Most metal lines are completely absent, including nitrogen. During their core helium-burning stage, lines switch to emission, and even some metal lines (oxygen and carbon, but still almost no nitrogen) are detected. Mass loss and clumping play a significant role in line formation in later evolutionary phases, particularly during core helium-burning. Most of our spectra are classified as an early-O type giant or supergiant, and we find Wolf-Rayet stars of type WO in the core helium-burning phase. Conclusions. An extremely hot, early-O type star observed in a low-metallicity galaxy could be the result of chemically homogeneous evolution and might therefore be the progenitor of a long-duration gamma-ray burst or a type Ic supernova. TWUIN stars may play an important role in reionizing the Universe because they are hot without showing prominent emission lines during most of their lifetime.

Česky

Spočetli jsme syntetická spektra hvězd pro široký interval počátečních hmotností odpovídající různým vývojovým stadiím hvězd od hlavní posloupnosti až po fázi hoření helia v jádře. Extrémně horké rané hvězdy pozorované v galaxiích s nízkým obsahem těžších prvků mohou být důsledkem chemicky homogenního vývoje a předchůdcem supernov typu Ic a dlouhotrvajících záblasků záření gama.

Návaznosti

GA16-01116S, projekt VaV

Název: Atmosféry a okolohvězdné prostředí magnetických horkých hvězd

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

Citovat

KUBATOVA, B.; D. SZECSI; A. A. C. SANDER; J. KUBAT; F. TRAMPER; Jiří KRTIČKA; C. KEHRIG; W. R. HAMANN; R. HAINICH a T. SHENAR. Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars. Astronomy and Astrophysics. LES ULIS CEDEX A: EDP SCIENCES S A, 2019, roč. 623, FEB 25 2019, s. "A8-1"-"A8-32", 32 s. ISSN 1432-0746. Dostupné z: https://doi.org/10.1051/0004-6361/201834360.

@article{1599998,
   author = {Kubatova, B. and Szecsi, D. and Sander, A. A. C. and Kubat, J. and Tramper, F. and Krtička, Jiří and Kehrig, C. and Hamann, W. R. and Hainich, R. and Shenar, T.},
   article_location = {LES ULIS CEDEX A},
   article_number = {FEB 25 2019},
   doi = {https://doi.org/10.1051/0004-6361/201834360},
   keywords = {stars: massive; stars: winds outflows; stars: rotation; galaxies: dwarf; radiative transfer},
   language = {eng},
   issn = {1432-0746},
   journal = {Astronomy and Astrophysics},
   title = {Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars},
   url = {https://www.aanda.org/articles/aa/pdf/2019/03/aa34360-18.pdf},
   volume = {623},
   year = {2019}
}

TY  - JOUR
ID  - 1599998
AU  - Kubatova, B. - Szecsi, D. - Sander, A. A. C. - Kubat, J. - Tramper, F. - Krtička, Jiří - Kehrig, C. - Hamann, W. R. - Hainich, R. - Shenar, T.
PY  - 2019
TI  - Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars
JF  - Astronomy and Astrophysics
VL  - 623
IS  - FEB 25 2019
SP  - "A8-1"-"A8-32"
EP  - "A8-1"-"A8-32"
PB  - EDP SCIENCES S A
SN  - 14320746
KW  - stars: massive
KW  - stars: winds outflows
KW  - stars: rotation
KW  - galaxies: dwarf
KW  - radiative transfer
UR  - https://www.aanda.org/articles/aa/pdf/2019/03/aa34360-18.pdf
L2  - https://www.aanda.org/articles/aa/pdf/2019/03/aa34360-18.pdf
N2  - Context. Metal-poor massive stars are assumed to be progenitors of certain supernovae, gamma-ray bursts, and compact object mergers that might contribute to the early epochs of the Universe with their strong ionizing radiation. However, this assumption remains mainly theoretical because individual spectroscopic observations of such objects have rarely been carried out below the metallicity of the Small Magellanic Cloud. Aims. Here we explore the predictions of the state-of-the-art theories of stellar evolution combined with those of stellar atmospheres about a certain type of metal-poor (0.02 Z(circle dot)) hot massive stars, the chemically homogeneously evolving stars that we call Transparent Wind Ultraviolet INtense (TWUIN) stars. Methods. We computed synthetic spectra corresponding to a broad range in masses (20 130 M-circle dot) and covering several evolutionary phases from the zero-age main-sequence up to the core helium-burning stage. We investigated the influence of mass loss and wind clumping on spectral appearance and classified the spectra according to the Morgan-Keenan (MK) system. Results. We find that TWUIN stars show almost no emission lines during most of their core hydrogen-burning lifetimes. Most metal lines are completely absent, including nitrogen. During their core helium-burning stage, lines switch to emission, and even some metal lines (oxygen and carbon, but still almost no nitrogen) are detected. Mass loss and clumping play a significant role in line formation in later evolutionary phases, particularly during core helium-burning. Most of our spectra are classified as an early-O type giant or supergiant, and we find Wolf-Rayet stars of type WO in the core helium-burning phase. Conclusions. An extremely hot, early-O type star observed in a low-metallicity galaxy could be the result of chemically homogeneous evolution and might therefore be the progenitor of a long-duration gamma-ray burst or a type Ic supernova. TWUIN stars may play an important role in reionizing the Universe because they are hot without showing prominent emission lines during most of their lifetime.
ER  -

KUBATOVA, B.; D. SZECSI; A. A. C. SANDER; J. KUBAT; F. TRAMPER; Jiří KRTIČKA; C. KEHRIG; W. R. HAMANN; R. HAINICH a T. SHENAR. Low-metallicity massive single stars with rotation II. Predicting spectra and spectral classes of chemically homogeneously evolving stars. \textit{Astronomy and Astrophysics}. LES ULIS CEDEX A: EDP SCIENCES S A, 2019, roč.~623, FEB 25 2019, s.~''A8-1''-''A8-32'', 32 s. ISSN~1432-0746. Dostupné z: https://doi.org/10.1051/0004-6361/201834360.

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