Predictions of the effect of clumping on the wind properties of
O-type stars

J 2011

Predictions of the effect of clumping on the wind properties of O-type stars

MUIJRES, Lianne, Alex DE KOTER, Jorick VINK, Jiří KRTIČKA, Jiří KUBÁT et. al.

Základní údaje

Originální název

Predictions of the effect of clumping on the wind properties of O-type stars

Název česky

Předpovědi vlivu chuchvalců na vlastnostnosti větru hvězd typu O

Autoři

MUIJRES, Lianne (528 Nizozemské království), Alex DE KOTER (528 Nizozemské království), Jorick VINK (528 Nizozemské království), Jiří KRTIČKA (203 Česká republika, garant, domácí), Jiří KUBÁT (203 Česká republika) a Norbert LANGER (276 Německo)

Vydání

Astronomy and Astrophysics, Les Ulis Cedex, France, EDP Sciences, 2011, 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: 4.587

Kód RIV

RIV/00216224:14310/11:00049668

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1051/0004-6361/201014290

UT WoS

000286458400044

Klíčová slova česky

přenos záření; hvězdy: rané; hvězdy: hmotné; hvězdy: ztráta hmoty; hvězdy: větry

Klíčová slova anglicky

radiative transfer; stars: early-type; stars: massive; stars: mass-loss; stars: winds; outflows

Štítky

AKR, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 20. 4. 2012 09:52, Ing. Andrea Mikešková

Anotace

ORIG CZ

V originále

Aims. Both empirical evidence and theoretical ndings indicate that the stellar winds of massive early-type stars are inhomogeneous, i.e., porous and clumpy. For relatively dense winds, empirically derived mass-loss rates might be reconciled with predictions if these empirical rates are corrected for clumping. The predictions, however, do not account for structure in the wind. To allow for a consistent comparison, we investigate and quantify the e ect of clumpiness and porosity of the out ow on the predicted wind energy and the maximal e ect on the mass-loss rate of O-type stars. Methods. Combining non-LTE model atmospheres and a Monte Carlo method to compute the transfer of momentum from the photons to the gas, the e ect of clumping and porosity on the energy transferred from the radiation eld to the wind is computed in out ows in which the clumping and porosity strati cation is parameterized by heuristic prescriptions. Results. The impact of structure in the out ow on the wind energy is complex and is a function of stellar temperature, the density of gas in the clumps, and the physical scale of the clumps. If the medium is already clumped in the photosphere, the emergent radiation eld will be softer, slightly increasing the wind energy of relatively cool O stars (30 000 K) but slightly decreasing it for relatively hot O stars (40 000 K). More important is that as a result of recombination of the gas in a clumped wind the line force increases. However, because of porosity the line force decreases, simply because photons may travel in-between the clumps, avoiding interactions with the gas. If the changes in the wind energy only a ect the mass-loss rate and not the terminal velocity of the ow, we nd that the combined e ect of clumpiness and porosity is a small reduction in the mass-loss rate if the clumps are smaller than 1/100th the local density scale height. In this case, empirical mass-loss determinations based on Halpha tting and theory match for stars with dense winds ( M > 10 7 M yr 1 ) if the overdensity of gas in the clumps, relative to the case of a smooth wind, is modest. For clumps larger than 1/10th H , the predicted mass-loss rates exhibit almost the same dependence on clumpiness as do empirical rates. We show that this implies that empirical and predicted mass-loss rates can no longer be matched. Very high overdensities of gas in clumps of such large size may cause the predicted M to decrease by a factor of from 10 to 100. This type of structure is likely not to be the cause of the weak-wind problem in early-type stars, unless a mechanism can be identi ed that causes extreme structure to develop in winds for which M < 10 7 M yr 1 (weak winds) that is not active in denser winds.

Česky

Ukazuje se, že hvězdné větry horkých hvězd jsou nehomogenní. Studujeme vliv strukturovanosti větru na předpovězenou energii větru a maximální možný vliv na rychlost ztráty hmoty hvězd typu O. Používáme NLTE modely atmosfér a metodu Monte Carlo pro výpočet přenosu hybnosti fototonů plynu. Vliv chuchvalců a porozity je parametrizován pomocí vhodného předpisu. Vliv struktury větru na předanou energii je složitý a závisí na efektivní teplotě hvězdy, hustotě plynu v chuchvalcích a stavu chuchvalců.

Návaznosti

GA205/08/0003, projekt VaV

Název: Předpovědi rychlosti ztráty hmoty horkých hvězd

Investor: Grantová agentura ČR, Předpovědi rychlosti ztráty hmoty horkých hvězd

Citovat

MUIJRES, Lianne, Alex DE KOTER, Jorick VINK, Jiří KRTIČKA, Jiří KUBÁT a Norbert LANGER. Predictions of the effect of clumping on the wind properties of O-type stars. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, 2011, roč. 526, zima, s. "A32-1"-"A32-11", 11 s. ISSN 0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201014290.

@article{916260,
   author = {Muijres, Lianne and de Koter, Alex and Vink, Jorick and Krtička, Jiří and Kubát, Jiří and Langer, Norbert},
   article_location = {Les Ulis Cedex, France},
   article_number = {zima},
   doi = {http://dx.doi.org/10.1051/0004-6361/201014290},
   keywords = {radiative transfer; stars: early-type; stars: massive; stars: mass-loss; stars: winds; outflows},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Predictions of the effect of clumping on the wind properties of O-type stars},
   url = {http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014290&Itemid=129},
   volume = {526},
   year = {2011}
}

TY  - JOUR
ID  - 916260
AU  - Muijres, Lianne - de Koter, Alex - Vink, Jorick - Krtička, Jiří - Kubát, Jiří - Langer, Norbert
PY  - 2011
TI  - Predictions of the effect of clumping on the wind properties of O-type stars
JF  - Astronomy and Astrophysics
VL  - 526
IS  - zima
SP  - "A32-1"-"A32-11"
EP  - "A32-1"-"A32-11"
PB  - EDP Sciences
SN  - 00046361
KW  - radiative transfer
KW  - stars: early-type
KW  - stars: massive
KW  - stars: mass-loss
KW  - stars: winds
KW  - outflows
UR  - http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014290&Itemid=129
L2  - http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014290&Itemid=129
N2  - Aims. Both empirical evidence and theoretical ndings indicate that the stellar winds of massive early-type stars are inhomogeneous, i.e., porous and clumpy. For relatively dense winds, empirically derived mass-loss rates might be reconciled with predictions if these empirical rates are corrected for clumping. The predictions, however, do not account for structure in the wind. To allow for a consistent comparison, we investigate and quantify the e ect of clumpiness and porosity of the out ow on the predicted wind energy and the maximal e ect on the mass-loss rate of O-type stars. Methods. Combining non-LTE model atmospheres and a Monte Carlo method to compute the transfer of momentum from the photons to the gas, the e ect of clumping and porosity on the energy transferred from the radiation eld to the wind is computed in out ows in which the clumping and porosity strati cation is parameterized by heuristic prescriptions. Results. The impact of structure in the out ow on the wind energy is complex and is a function of stellar temperature, the density of gas in the clumps, and the physical scale of the clumps. If the medium is already clumped in the photosphere, the emergent radiation eld will be softer, slightly increasing the wind energy of relatively cool O stars (30 000 K) but slightly decreasing it for relatively hot O stars (40 000 K). More important is that as a result of recombination of the gas in a clumped wind the line force increases. However, because of porosity the line force decreases, simply because photons may travel in-between the clumps, avoiding interactions with the gas. If the changes in the wind energy only a ect the mass-loss rate and not the terminal velocity of the ow, we nd that the combined e ect of clumpiness and porosity is a small reduction in the mass-loss rate if the clumps are smaller than 1/100th the local density scale height. In this case, empirical mass-loss determinations based on Halpha tting and theory match for stars with dense winds ( M > 10 7 M yr 1 ) if the overdensity of gas in the clumps, relative to the case of a smooth wind, is modest. For clumps larger than 1/10th H , the predicted mass-loss rates exhibit almost the same dependence on clumpiness as do empirical rates. We show that this implies that empirical and predicted mass-loss rates can no longer be matched. Very high overdensities of gas in clumps of such large size may cause the predicted M to decrease by a factor of from 10 to 100. This type of structure is likely not to be the cause of the weak-wind problem in early-type stars, unless a mechanism can be identi ed that causes extreme structure to develop in winds for which M < 10 7 M yr 1 (weak winds) that is not active in denser winds.
ER  -

MUIJRES, Lianne, Alex DE KOTER, Jorick VINK, Jiří KRTIČKA, Jiří KUBÁT a Norbert LANGER. Predictions of the effect of clumping on the wind properties of O-type stars. \textit{Astronomy and Astrophysics}. Les Ulis Cedex, France: EDP Sciences, 2011, roč.~526, zima, s.~''A32-1''-''A32-11'', 11 s. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201014290.

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