The VLT-FLAMES Tarantula Survey

Ramírez-Agudelo, O. H.; Sana, H.; Koter, A. de; Tramper, F.; Grin, N. J.; Schneider, F. R. N.; Langer, N.; Puls, J.; Маркова, Н.; Bestenlehner, J. M.; Castro, N.; Crowther, P. A.; Evans, C. J.; García, M.; Gräfener, G.; Herrero, A.; Kempen, B. van; Lennon, D. J.; Apellániz, J. Maíz; Najarro, F.; Sabín-Sanjulián, C.; Simón‐Díaz, S.; Taylor, W. D.; Vink, J. S.

doi:10.1051/0004-6361/201628914

Cited by 79 publications

(67 citation statements)

References 110 publications

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“…Hillier 1991). This has lead to a downward revision of empirical mass-loss rates, by a factor of ∼2−3 (Moffat & Robert 1994;Puls et al 2008;Hamann et al 2008;Ramírez-Agudelo et al 2017). …”

Section: Monte Carlo Modellingmentioning

confidence: 99%

Winds from stripped low-mass helium stars and Wolf-Rayet stars

Vink

2017

A&A

102

121

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We present mass-loss predictions from Monte Carlo radiative transfer models for helium (He) stars as a function of stellar mass, down to 2 M . Our study includes both massive Wolf-Rayet (WR) stars and low-mass He stars that have lost their envelope through interaction with a companion. For these low-mass He stars we predict mass-loss rates that are an order of magnitude smaller than by extrapolation of empirical WR mass-loss rates. Our lower mass-loss rates make it harder for these elusive stripped stars to be discovered via line emission, and we should attempt to find these stars through alternative methods instead. Moreover, lower massloss rates make it less likely that low-mass He stars provide stripped-envelope supernovae (SNe) of type Ibc. We express our mass-loss predictions as a function of L and Z and not as a function of the He abundance, as we do not consider this physically astute given our earlier work. The exponent of theṀ versus Z dependence is found to be 0.61, which is less steep than relationships derived from recent empirical atmospheric modelling. Our shallower exponent will make it more challenging to produce "heavy" black holes of order 40 M , as recently discovered in the gravitational wave event GW 150914, making low metallicity for these types of events even more necessary.

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Section: Monte Carlo Modellingmentioning

confidence: 99%

Winds from stripped low-mass helium stars and Wolf-Rayet stars

Vink

2017

A&A

102

121

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“…In lower metallicity environments, such as in the LMC and the SMC galaxies, some work (Massa et al 2017) indicates that wind mass loss rates may be actually higher than typically adopted in evolutionary predictions (Vink et al 2001;Belczynski et al 2010), others seem to agree with standard calculations (Ramírez-Agudelo et al 2017), and yet others point out to much lower mass-loss rates than expected (Bouret et al 2003;Ramachandran et al 2019;Sundqvist et al 2019). In the upper stellar mass regime, Hainich et al (2013Hainich et al ( , 2019 determine mass-loss rates which are in broad agreement with the theoretical expectations.…”

Section: Introductionmentioning

confidence: 97%

The Formation of a 70 M_⊙ Black Hole at High Metallicity

Belczyński

Hirschi

Kaiser

et al. 2020

ApJ

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A 70 M black hole was discovered in Milky Way disk in a long period (P = 78.9 days) and almost circular (e = 0.03) detached binary system (LB-1) with a high (Z ∼ 0.02) metallicity 8 M B star companion. Current consensus on the formation of black holes from high metallicity stars limits the black hole mass to be below 20 M due to strong mass loss in stellar winds. So far this was supported by the population of Galactic black hole X-ray binaries with Cyg X-1 hosting the most massive ∼ 15 M black hole. Using the Hurley et al. 2000 analytic evolutionary formulae, we show that the formation of a 70 M black hole in high metallicity environment is possible if stellar wind mass loss rates, that are typically adopted in evolutionary calculations, are reduced by factor of 5.As observations indicate, a fraction of massive stars (∼ 7%) have surface magnetic fields which, as suggested by Owocki et al. 2016, may quench the wind mass-loss, independently of stellar mass and metallicity. We also computed detailed stellar evolution models and we confirm such a scenario. A non-rotating 85 M star model at Z = 0.014 with decreased winds ends up as a 71 M star prior corecollapse with a 32 M helium core and a 28 M CO core. Such star avoids pair-instability pulsation supernova mass loss that severely limits black hole mass and may form a ∼ 70 M black hole in the direct collapse. Stars that can form 70 M black holes at high Z expand to significant size with radius of R 600 R (thanks to large H-rich envelope), however, exceeding the size of LB-1 orbit (semi-major axis a 350 R ). Therefore, we can explain the formation of black holes upto 70 M at high metallicity and this result is independent from LB-1; whether it hosts or does not host a massive black hole. However, if LB-1 hosts a massive black hole we are unable to explain how such a binary star system could have formed without invoking some exotic scenarios.

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“…[53,54] which terminate at the onset of He-burning. Figure 3 presents the HR diagram of the Tarantula Nebula, comprising single star results from VFTS [47][48][49][50][51], VLT/MUSE [11], HST/STIS [52] and literature results for other stars within 160 parsec of R136, including Wolf-Rayet stars [60]. Results for binary systems have been incorporated, primarily involving VFTS B-type binaries [61], Tarantula Massive Binary Monitoring (TMBM) O-type binaries [62] and recent literature for WR stars [37,63].…”

Section: Physical Propertiesmentioning

confidence: 99%

“…The most remarkable X-ray source in the Tarantula is VFTS 399 with L X,corr ∼ 5 × 10 34 erg s −1 despite being associated with a low luminosity O9 giant, implying L X,corr /L Bol ∼ 2 × 10 −4 . Clark et al [81] conclude that VFTS 399 is a high-mass X-ray binary hosting a neutron star remnant, with the O giant known to be a rapid rotator (v e sin i = 324 km s −1 , according to [50]), as one would expect for a mass gainer in a close binary system. Two point sources in the Tarantula are even brighter in X-rays than VFTS 399.…”

Section: Binaries Rotation and Runawaysmentioning

confidence: 99%

“…Wind velocities of OB stars cannot be measured from optical spectroscopy, so usually spectral type calibrations are adopted based on measured velocities from UV P Cygni profiles of C IV, N V or Si IV [84]. Until recently, high S/N, high quality UV spectroscopy of OB stars in the Large [47,49,50], HST/STIS [52] and other surveys [37,60,63] for WR stars). Filled symbols are within NGC 2070, open symbols elsewhere in the Tarantula.…”

Section: Wind Propertiesmentioning

confidence: 99%

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Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

Crowther

2019

Galaxies

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A review of the properties of the Tarantula Nebula (30 Doradus) in the Large Magellanic Cloud is presented, primarily from the perspective of its massive star content. The proximity of the Tarantula and its accessibility to X-ray through radio observations permit it to serve as a Rosetta Stone amongst extragalactic supergiant HII regions since one can consider both its integrated characteristics and the individual properties of individual massive stars. Recent surveys of its high mass stellar content, notably the VLT FLAMES Tarantula Survey (VFTS), are reviewed, together with VLT/MUSE observations of the central ionizing region NGC 2070 and HST/STIS spectroscopy of the young dense cluster R136, provide a near complete Hertzsprung-Russell diagram of the region, and cumulative ionizing output. Several high mass binaries are highlighted, some of which have been identified from a recent X-ray survey. Brief comparisons with the stellar content of giant HII regions in the Milky Way (NGC 3372) and Small Magellanic Cloud (NGC 346) are also made, together with Green Pea galaxies and star forming knots in high−z galaxies. Finally, the prospect of studying massive stars in metal poor galaxies is evaluated.

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The VLT-FLAMES Tarantula Survey

Cited by 79 publications

References 110 publications

Winds from stripped low-mass helium stars and Wolf-Rayet stars

Winds from stripped low-mass helium stars and Wolf-Rayet stars

The Formation of a 70 M_⊙ Black Hole at High Metallicity

Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

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The VLT-FLAMES Tarantula Survey

Cited by 79 publications

References 110 publications

Winds from stripped low-mass helium stars and Wolf-Rayet stars

Winds from stripped low-mass helium stars and Wolf-Rayet stars

The Formation of a 70 M⊙ Black Hole at High Metallicity

Massive Stars in the Tarantula Nebula: A Rosetta Stone for Extragalactic Supergiant HII Regions

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Product

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The Formation of a 70 M_⊙ Black Hole at High Metallicity