Radiatively Driven Winds and the Shaping of Bipolar Luminous Blue Variable Nebulae

Dwarkadas, Vikram V.; Owocki, S. P.

doi:10.1086/344257

Cited by 79 publications

(110 citation statements)

References 31 publications

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“…Kep is the Keplerian velocity on the equator (i.e., the breakup angular velocity). Dwarkadas & Owocki (2002) and Smith et al (2003a), for example, take ¼ 0:9, while Maeder & Desjacques (2001) take ¼ 0:8 0:9. The model presented by Langer et al (1999) is different in that they consider the ratio of luminosity to the Eddington limit.…”

Section: Angg Ular Velocity Evv Olution Duringgthe Great Eruptionmentioning

confidence: 99%

“…In that paper I listed some arguments in favor of such a model. However, the new finding of Smith et al (2003b) of a more massive Homunculus and several new papers using a single-star model for the shaping of the wind and circumstellar matter of Car (e.g., Dwarkadas & Owocki 2002;Smith et al 2003a;González et al 2004;van Boekel et al 2003) motivate me to reconsider the single-star model. Other papers in recent years study the role of rotation and/or binary companion in Car.…”

Section: Introductionmentioning

confidence: 99%

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Why a Single‐Star Model Cannot Explain the Bipolar Nebula of η Carinae

Soker

2004

ApJ

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I examine the angular momentum evolution during the 1837-1856 Great Eruption of the massive star Carinae. I find that the new estimate of the mass blown during that eruption implies that the envelope of Car substantially spun down during the 20 yr eruption. Single-star models, most of which require the envelope to rotate at close to the break-up velocity, cannot account for the bipolar nebula-the Homunculus-formed from matter expelled in that eruption. The kinetic energy and momentum of the Homunculus further constrain singlestar models. I discuss how Car can fit into a unified model for the formation of bipolar lobes in which two oppositely ejected jets inflate two lobes (or bubbles). These jets are blown by an accretion disk, which requires stellar companions in the case of bipolar nebulae around stellar objects.

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Section: Angg Ular Velocity Evv Olution Duringgthe Great Eruptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Why a Single‐Star Model Cannot Explain the Bipolar Nebula of η Carinae

Soker

2004

ApJ

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“…Various types of mechanisms for jet formation have been proposed so far, which include magnetic collimation of outflow ejected from the accretion disk or the central star (Ogilvie & Livio 2001;Tsinganos & Bogovalov 2002), mass ejection into an asymmetric medium surrounding the object, bipolar wind from very rapid stellar rotation of blue variable nebulae (Dwarkadas & Owocki 2002), radiative collimation of winds by the disk radiation field (Fukue 2002), and thermonuclear runaway on a rotating oblate WD (Porter et al 1998;Scott 2000).…”

Section: Discussionmentioning

confidence: 99%

High-Velocity Jets in Recurrent Nova Outbursts

Kato

Hachisu

2003

The Astrophysical Journal

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Very fast bipolar mass outflows are suggested from emission-line profiles during the early stage of outbursts in the recurrent nova U Sco. The ejection velocity reaches 5000 or 6000 km s Ϫ1 at the optical peak and gradually decreases in time. Such properties have not been reproduced so far in nova theories. We propose a jet-shaped mass outflow as a mechanism of acceleration up to several thousand kilometers per second. The mass flow is accelerated where the jet is shaped, which is deep inside the region where the spherically symmetric winds would be accelerated. The terminal jet velocity depends sensitively on the white dwarf mass but weakly on other parameters.

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“…Rotation of the star can lead to enhanced mass-loss [14]. Also a star rotating close to its break-up velocity may emit a wind preferentially in the polar direction [8]. Mass-loss rates are also metallicity dependent, although rotation can lead to high rates even at low metallicity.…”

Section: Winds From Massive Starsmentioning

confidence: 99%