WC Stars In 30 Doradus

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Evolução de estrelas massivas

S Doradus na Grande Nuvem de Magalhães e ~ 15 000 30 000 K L ~ 106 L Sol Massas > 85 M Wolf Rayet: WN, WC, WO

arXiv:1210.0062v1 [astro-ph.SR] 29 Sep 2012

While observing OB stars within the most crowded regions of the Large Mag-ellanic Cloud, we happened upon a new Wolf-Rayet star in Lucke-Hodge 41, the rich OB association that contains S Doradus and numerous other massive stars. At first glance the spectrum resembled that of a WC4 star, but closer examina-

General Disclaimer One or more of the Following Statements

(5) The W-R stars can be divided into two subtypes: These are the WN types, in which the ions of nitrogen dominate, and the WC types, in which the ions of carbon (and oxygen) dominate. Both sub-types have * Visiting Astronomer at KPNO and CHO.

Massiva stjärnors utveckling (M > 8 stjärnmassor) Nebulosor

Tarantulanebulosan (30 Doradus) är ett gigantiskt,1000 ljusår stort, HII-område C+O+He WC C+O WO De massiva stjärnorna förlorar en because the stars

Glossary - Wiley

GDOR 𝛾Doradus(stars) WC Carbon-richWolf-Rayetstar WD WhiteDwarf WDM WhiteDwarfMerger WET WholeEarthTelescope 8/18/2015 3:30:44 PM

Wolf-RayetStarsin M33II: Optical Spectroscopyof emission

starbursts: individual stars can be counted and spectroscop-ically classified, allowing a direct comparison with the mod-elisation of the spatially integrated properties of their ion-izing cluster (see Vacca et al. 1995 for such a comparison in 30 Doradus, or Bruhweiler, Miskey & Smith Neubig 2003 in NGC 604).

Formation and Evolution of Massive Stars: Current Surveys

Multi-epoch spectroscopy of over 800 massive stars in 30 Doradus Bigger context of Massive Stars Formation Dark Cloud G19.30+0.07 (VLA) No WC stars

Astronomy c ESO 2011 Astrophysics

massive stars remain unanswered, particularly in the context of results that point to the majority of high-mass stars being in bi-nary/multiple systems (e.g. Sana & Evans 2011). The Tarantula Nebula (NGC2070, 30 Doradus hereafter 30 Dor ) in the Large Magellanic Cloud (LMC) is the bright-ii region in the Local Group.

L/L® = 6 X 107 , the values of log WC(S) and Alog 'W' = log

predicted values, when these objects are not single stars but are composed of a dense cluster of similar stars has been discussed. Key words: mass loss - massive stars - H II regions The recent discovery of R 136a in the giant H il region 30 Doradus, in the Large Magellanic Cloud (LMC), as a very luminous and supermassive star (Feitzinger et al.

Open Research Online

stars. We are able to infer a high binary fraction for both WN (10 /16) and WC stars (7 /8), resulting in a combined Wolf Rayet binary fraction of > 70%. These represent the most stringent limits currently placed on the binary fraction of very massive ( > 45 M ) stars.

arXiv:1404.0166v2 [astro-ph.SR] 18 Jun 2014

Many of the stars with masses claimed to be higher than 100 M⊙ are located in the Magellanic Clouds. The most striking example is certainly that of R136, the core of the 30 Doradus giant HII region in the Large Magellanic Clouc (LMC) where the metallicity is about half the solar metallicity. Using photographic plates,

Wolf-Rayet stars: extremely hot, luminous and massive

Wolf-Rayet stars are named after Charles Wolf (1827 - 1918) and George Rayet (1839 - 1906), French astronomers who discovered these unusual stars at the Paris Observatory in 1867, using the 40-cm Foucault telescope. 150 years later, we know of only 580 in the Milky Way galaxy, and a few hundred in

Millennium Essay - JSTOR

R136/30 Doradus in the LMC is an optically visible and relatively nearby example of a giant H II (GHII) region. The central nonstellar object R136 is No. 43 in the WR catalog, having a composite spectrum of broad emission lines and stellar absorption features. This is due to a superposition of a number of early O-type stars and WN types, which have

Four Decades of Research on Massive Stars: A Scientific

11h50 Hugues Sana The Multiplicity Properties of Massive Stars in 30 Doradus 12h10 Alceste Bonanos Fundamental Parameters of 4 Massive Eclipsing Binaries in Westerlund 1 12h30-14h00 Lunch (Picnic boxes or hotel restaurant) Excursion or Activities

A newand unusualLBV-likeoutburstfromaWolf-Rayet star

Ofpe/WN9 stars were first recognised as a class based on about ten objects in the Large Magellanic Cloud (LMC), but have also been found in a number of nearby galax-ies. Ofpe/WN9 stars are luminous, typically log(L/L⊙) = 5.5 6.5, implying high initial masses; also, they have hot temperatures of roughly 29 30 kK, and wind speeds of

Cap. 15 Evolução de estrelas massivas

S Doradus na Grande Nuvem de Magalhães e ~ 15 000 30 000 K L ~ 106 L Sol Massas > 85 M Sol Wolf Rayet: WN, WC, WO


6.5 Dust formation in WC stars 149 7 Birth of massive stars and star clusters 154 7.1 Natal precursors of OB stars 155 9.2 30 Doradus the Rosetta Stone 200


ratio N(WC)/N(WN) is ˘ 1 in the solar neighbor-hood (Conti & Vacca 1990), and ˘ 0.1{0.2 within a 1000 radius of the 30 Doradus nebula (Mo at et al. 1987). In starbursting galaxies with 1/5 Z/Z 1 ˘ 30% of WR stars are of WC subtype (Schaerer & Vacca 1996; Schaerer et al. 1997). The rst detec-tions of the C IV 5808 emission line (hereafter called

arXiv:astro-ph/9910432v1 23 Oct 1999

10′′ radius of the 30 Doradus nebula (Moffat et al. 1987). In starbursting galaxies with 1/5 ≤Z/Z⊙ ≤ 1 ∼ 30% of WR stars are of WC subtype (Schaerer & Vacca 1996; Schaerer et al. 1997). The first detec-tions of the C IV λ5808 emission line (hereafter called the red bump ) in integrated galaxy spectra were re-


by IUE observations of the 30 Doradus nebula (Koornneef and Mathis, 1.980) and of local galactic 11 It regions. Thus, we presume in the following that the observed far-UV is either direct star1ight or starlight scattered by oust in close proximity to the stars. As discussed in more detail


the giant H ii region 30 Doradus in the Large Magellanic Cloud. The spectra represent spatial integrations over areas 20 00 ×20 00 , 1 0 ×1 0 , and 3 0 ×3 0 , all of which are approximately centered on R136.

The Wolf Rayet Content of the Galaxies of the Local Group and

of stars. In all except the most crowded of regions (such as 30 Doradus in the Large Magellanic Cloud), stars can be individually resolved by ground-based telescopes and instruments. Such photometric studies have been done previously (such as the Local Group Galaxy Survey [LGGS] [10]), but photometry alone can t be used to detect Wolf Rayet

The Most Massive Stars

Second stop: 30 Doradus Giant HII region in the LMC Closest starburst cluster in Local Group Central cluster of 30 Dor is R136 (usually the WFPC2 field) Contains 100's of O stars, including the hottest known O3V stars (Massey & Hunter 1998) Core of R136 is R136a (central arcsecond): was thought to be a single star with 1000's of Msol

The detectability of Wolf Rayet stars in M33-like spirals up

WC stars, with the star Tarantula Survey data to carry out a census of the 30 Doradus star-forming region in the LMC, including R136 star cluster, and found

A massive nebula around the luminous blue variable star RMC

The luminous blue variable (LBV) RMC143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3˙sub-millimetre detection of its circumstellar nebula with ALMA.

The fourth catalogue of Population I Wolf-Rayet stars in the

maining 4% of the stars - six members of the R 136 cluster at the heart of the 30 Doradus nebula - we adopted the coordinates published by Malumuth & Heap (1994). For the stars appearing on di erent plates or CCD frames, the astrometric measurements were repeated. This resulted in 30% and 10% of the stars having their coordi-

Starburst clusters with E-ELT - the harvest beyond the Milky Way

The birth place of high-mass stars 1. Starburst clusters in the Milky Way not YSO, not late-type AGB/WC Moneti et al. 2001 R136 30 Doradus Γ = -1.1


only to 30 Doradus in its massive star population. This young association contains a rich collection of stars including two of the seven known luminous blue variables (LBVs) in the LMC (one being the well-known S Doradus), a Wolf Rayet (WR) star/B supergiant pair, and two A-type supergiants, as well as


hydrogen-rich very massive stars (VMSs; masses > 100Me). Crowther et al. (2010) found that four stars in R136, the central ionizing cluster of the 30 Doradus region in the Large Magellanic Cloud (LMC), have masses that exceeded the then standard upper mass limit of 150Me (Figer 2005). The four stars they find have initial masses between 165

The History Goes On: Century Long Study of Romano's Star

Massey and Johnson [17] found a couple of carbon-rich Wolf-Rayet (WC) stars in these associations, J013458.89+304129.0 (WC4) in OB88 and J013505.37+304114.9 (WC4-5) in OB89. Moreover, the OB88 association contains the star J013500.30+304150.9 classified as an LBV candidate by Massey et al. [18],

Recent studies of planetary nebulae and BCDs with VLT FLAMES

At low Z primary Nitrogen is produced with Oxygen from massive stars (M > 9 Msol) As the starburst ages, secondary N from stars of all masses and primary N from AGBs is produced: resulting scatter. Outlying galaxies with ~solar N/O are rare and require an explanation. They contain Wolf-Rayet stars and/or show evidence of mergers.

Dissecting the Core of the Tarantula Nebula with MUSE

The Tarantula Nebula (30 Doradus) in the Large Magellanic Cloud (LMC) is intrinsically the brightest star-forming region in the Local Group and has been the subject of numerous studies across the electromagnetic spectrum. Its low (half-solar) metallicity and high star for-mation intensity are more typical of knots