DOCSLIB.ORG

The VLT-FLAMES Tarantula Survey. XVII

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The VLT-FLAMES Tarantula Survey. XVII UvA-DARE (Digital Academic Repository) The VLT-FLAMES Tarantula Survey. XVII Physical and wind properties of massive stars at the top of the main sequence Bestenlehner, J.M.; Gräfener, G.; Vink, J.S.; Najarro, F.; de Koter, A.; Sana, H.; Evans, C.J.; Crowther, P.A.; Hénault-Brunet, V.; Herrero, A.; Langer, N.; Schneider, F.R.N.; Simón-Díaz, S.; Taylor, W.D.; Walborn, N.R. DOI 10.1051/0004-6361/201423643 Publication date 2014 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Bestenlehner, J. M., Gräfener, G., Vink, J. S., Najarro, F., de Koter, A., Sana, H., Evans, C. J., Crowther, P. A., Hénault-Brunet, V., Herrero, A., Langer, N., Schneider, F. R. N., Simón- Díaz, S., Taylor, W. D., & Walborn, N. R. (2014). The VLT-FLAMES Tarantula Survey. XVII: Physical and wind properties of massive stars at the top of the main sequence. Astronomy & Astrophysics, 570, [A38]. https://doi.org/10.1051/0004-6361/201423643 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:06 Oct 2021 A&A 570, A38 (2014) Astronomy DOI: 10.1051/0004-6361/201423643 & c ESO 2014 Astrophysics The VLT-FLAMES Tarantula Survey XVII. Physical and wind properties of massive stars at the top of the main sequence? J. M. Bestenlehner1, G. Gräfener1, J. S. Vink1, F. Najarro2, A. de Koter3;4, H. Sana5, C. J. Evans6, P. A. Crowther7, V. Hénault-Brunet8, A. Herrero9;10, N. Langer11, F. R. N. Schneider11, S. Simón-Díaz9;10, W. D. Taylor6, and N. R. Walborn12 1 Armagh Observatory, College Hill, Armagh BT61 9DG, UK e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), Ctra. de Torrejón a Ajalvir km-4, 28850 Torrejón de Ardoz, Madrid, Spain 3 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH, Amsterdam, The Netherlands 4 Instituut voor Sterrenkunde, Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium 5 ESA/STScI, 3700 San Martin Drive, Baltimore, MD21210, USA 6 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 7 Dept. of Physics & Astronomy, Hounsfield Road, University of Sheffield, S3 7RH, UK 8 Department of Physics, Faculty of Engineering and Physical Sciences, University of Surrey, Guildford, GU2 7XH, UK 9 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain 10 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 11 Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany 12 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA Received 14 February 2014 / Accepted 4 July 2014 ABSTRACT The evolution and fate of very massive stars (VMS) is tightly connected to their mass-loss properties. Their initial and final masses differ significantly as a result of mass loss. VMS have strong stellar winds and extremely high ionising fluxes, which are thought to be critical sources of both mechanical and radiative feedback in giant H ii regions. However, how VMS mass-loss properties change during stellar evolution is poorly understood. In the framework of the VLT-Flames Tarantula Survey (VFTS), we explore the mass-loss transition region from optically thin O star winds to denser WNh Wolf-Rayet star winds, thereby testing theoretical predictions. To this purpose we select 62 O, Of, Of/WN, and WNh stars, an unprecedented sample of stars with the highest masses and luminosities known. We perform a spectral analysis of optical VFTS as well as near-infrared VLT/SINFONI data using the non-LTE radiative transfer code CMFGEN to obtain both stellar and wind parameters. For the first time, we observationally resolve the transition between optically thin O star winds and optically thick hydrogen-rich WNh Wolf-Rayet winds. Our results suggest the existence of a “kink” between both mass-loss regimes, in agreement with recent Monte Carlo simulations. For the optically thick regime, we confirm the steep dependence on the classical Eddington factor Γe from previous theoretical and observational studies. The transition occurs on the main sequence near a luminosity of 106:1 L , or a mass of 80 ::: 90 M . Above this limit, we find that – even when accounting for moderate wind clumping (with fv = 0:1) – wind mass-loss rates are enhanced with respect to standard prescriptions currently adopted in stellar evolution calculations. We also show that this results in substantial helium surface enrichment. Finally, based on our spectroscopic analyses, we are able to provide the most accurate ionising fluxes for VMS known to date, confirming the pivotal role of VMS in ionising and shaping their environments. Key words. stars: Wolf-Rayet – stars: early-type – stars: atmospheres – stars: mass-loss – stars: fundamental parameters 1. Introduction existence of a number of highly luminous Galactic objects (up to 107 L ). Crowther et al.(2010) confirmed this finding, report- Very massive stars (VMS) are defined to be initially more mas- ing the existence of VMS up to 320 M for the R136 core stars sive than 100 M (cf. Vink et al. 2013). Whilst a lot of attention in the Tarantula nebula of the Large Magellanic Cloud (LMC). has been devoted to the role of VMS at extremely low metal- Given the clustered nature of these objects it was important that licity in the very early Universe (e.g. Bromm et al. 1999; Abel Bestenlehner et al.(2011) identified an almost identical twin of et al. 2002), the role of VMS in our local Universe has largely R136a3, VFTS 682, in the context of the VFTS. Its isolated been ignored until recently. Hamann et al.(2006) found the nature increased confidence that VMS really exist above the “canonical” upper limit of about 150 M (Figer 2005). ? Appendices are available in electronic form at http://www.aanda.org Article published by EDP Sciences A38, page 1 of 92 A&A 570, A38 (2014) Interestingly, the presence of VMS of up to 320 M data used (in Sects. 2.1 and 2.2), and describe the target selection would bring them into the predicted initial mass range of process (Sect. 2.3). pair-instability supernovae of 140–260 M (Heger & Woosley 2002; Langer et al. 2007). As such explosions would disrupt the entire star, all metals would be returned to the interstellar 2.1. Spectroscopic observations medium (ISM). One such object at the top of the mass func- Within the VFTS project the entire 30 Doradus region, centred tion of a massive-star cluster would produce more metals than on the dense cluster R136, has been covered with optical fibre all the other lower mass stars together (Langer 2009). It could spectroscopy using the MEDUSA-GIRAFFE (λ4000–7000 Å) significantly affect chemical evolution modelling of galaxies. mode of the FLAMES instrument. Roughly 70% of the However, the evolution and fate of VMS are highly uncer- stars with V < 17 mag have been observed in this pro- tain. The main culprit is the unknown rate of wind mass loss, gramme. For the densely populated region near R 136 additional given that VMS are thought to evolve close to chemically ho- integral-field observations were obtained using FLAMES/UVES mogeneously (e.g. Gräfener et al. 2011). Whilst recent evolution λ / λ models have been published by e.g. Yungelson et al.(2008) and ( 4200–6100 Å) and ARGUS GIRAFFE ( 4000–4600 Å). Yusof et al.(2013), the way mass loss has been implemented Specifically for the analysis of VMS in the central re- in these models is entirely different and it is not known a priori gion of 30 Dor, K-band data were obtained with SINFONI which way is more appropriate. The key issue to decide whether the Spectrograph for INtegral Field Observations in the Near pair-instability supernovae are likely to exist in the present day Infrared on the VLT (Program ID 084.D-0980, PI: Gräfener). universe is that of stellar mass loss. The spectra cover the central arcsec around R 136 with a see- Fortunately, there has recently been significant progress in ing constraint 0.8 arcsec and a spectral resolution of R = 4000 over the wavelength≤ range of λ2:0 2:4 µm. Due to the increased our theoretical understanding of mass loss at the top of the − Hertzsprung-Russell diagram (HRD). In particular, Vink et al. IR wind-emission of VMS compared to lower-mass stars with (2011) computed mass-loss rates for VMS up to 300 M and weaker winds, these data provide a homogeneous set of wind discovered a “kink” in the mass loss versus Γ dependence, and abundance diagnostics for these objects that is less prone to involving a relatively shallow slope for optically thin O star crowding issues than e.g. optical data. The data were reduced us- winds, but changing into a steeper slope for optically thick WNh ing the standard ESO pipeline.
Load more

Recommended publications
  • The VLT-FLAMES Tarantula Survey III
    A&A 530, L14 (2011) Astronomy DOI: 10.1051/0004-6361/201117043 & c ESO 2011 Astrophysics Letter to the Editor The VLT-FLAMES Tarantula Survey III. A very massive star in apparent isolation from the massive cluster R136 J. M. Bestenlehner1,J.S.Vink1, G. Gräfener1, F. Najarro2,C.J.Evans3, N. Bastian4,5, A. Z. Bonanos6, E. Bressert5,7,8, P.A. Crowther9,E.Doran9, K. Friedrich10, V.Hénault-Brunet11, A. Herrero12,13,A.deKoter14,15, N. Langer10, D. J. Lennon16, J. Maíz Apellániz17,H.Sana14, I. Soszynski18, and W. D. Taylor11 1 Armagh Observatory, College Hill, Armagh BT61 9DG, UK e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), Ctra. de Torrejón a Ajalvir km-4, 28850 Torrejón de Ardoz, Madrid, Spain 3 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 4 Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching, Germany 5 School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK 6 Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & Vas. Pavlou Street, P. Penteli 15236, Greece 7 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 87548 Garching bei München, Germany 8 Harvard-Smithsonian CfA, 60 Garden Street, Cambridge, MA 02138, USA 9 Dept. of Physics & Astronomy, Hounsfield Road, University of Sheffield, S3 7RH, UK 10 Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany 11 SUPA, IfA, University of Edinburgh, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 12 Departamento
    [Show full text]
  • Gaia TGAS Search for Large Magellanic Cloud Runaway Supergiant Stars: Candidate Hypervelocity Star Discovery, and the Nature Of
    Astronomy & Astrophysics manuscript no. lennon˙gaia˙v2˙arx c ESO 2017 March 14, 2017 Gaia TGAS search for Large Magellanic Cloud runaway supergiant stars Candidate hypervelocity star discovery, and the nature of R 71 Daniel J. Lennon1, Roeland P. van der Marel2, Mercedes Ramos Lerate3, William O’Mullane1, and Johannes Sahlmann1;2 1 ESA, European Space Astronomy Centre, Apdo. de Correos 78, E-28691 Villanueva de la Canada,˜ Madrid, Spain 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 3 VitrocisetBelgium for ESA, European Space Astronomy Centre, Apdo. de Correos 78, E-28691 Villanueva de la Canada,˜ Madrid, Spain Received ; accepted ABSTRACT Aims. To search for runaway stars in the Large Magellanic Cloud (LMC) among the bright Hipparcos supergiant stars included in the Gaia DR1 TGAS catalog. Methods. We compute the space velocities of the visually brightest stars in the Large Magellanic Cloud that are included in the Gaia TGAS proper motion catalog. This sample of 31 stars contains a Luminous Blue Variable (LBV), emission line stars, blue and yellow supergiants and a SgB[e] star. We combine these results with published radial velocities to derive their space velocities, and by comparing with predictions from stellar dynamical models we obtain their (peculiar) velocities relative to their local stellar environment. Results. Two of the 31 stars have unusually high proper motions. Of the remaining 29 stars we find that most objects in this sample have velocities that are inconsistent with a runaway nature, being in very good agreement with model predictions of a circularly rotating disk model.
    [Show full text]
  • The VLT-FLAMES Tarantula Survey
    Astronomy & Astrophysics manuscript no. msOrevfinalcorr c ESO 2019 May 8, 2019 The VLT-FLAMES Tarantula Survey XIV. The O-Type Stellar Content of 30 Doradus N. R. Walborn1, H. Sana1,2, S. Sim´on-D´ıaz3,4, J. Ma´ız Apell´aniz5, W. D. Taylor6,7, C. J. Evans7, N. Markova8, D. J. Lennon9, and A. de Koter2,10 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands 3 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 4 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 5 Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18008 Granada, Spain 6 Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 7 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 8 Institute of Astronomy, National Astronomical Observatory, Bulgarian Academy of Sciences, PO Box 136, 4700 Smoljan, Bulgaria 9 European Space Agency, European Space Astronomy Centre, Camino Bajo del Castillo s/n, Urbanizaci´on Villafranca del Castillo, E-28691 Villanueva de la Ca˜nada, Madrid, Spain 10 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium ABSTRACT Detailed spectral classifications are presented for 352 O–B0 stars in the VLT-FLAMES Tarantula Survey ESO Large Programme, of which 213 O-type are judged of sufficiently high quality for further morphological analysis.
    [Show full text]
  • The Tarantula Nebula As a Template for Extragalactic Star Forming Regions from VLT/MUSE and HST/STIS
    This is a repository copy of The Tarantula Nebula as a template for extragalactic star forming regions from VLT/MUSE and HST/STIS. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/112327/ Version: Accepted Version Proceedings Paper: Crowther, P.A., Caballero-Nieves, S.M., Castro, N. et al. (1 more author) (2016) The Tarantula Nebula as a template for extragalactic star forming regions from VLT/MUSE and HST/STIS. In: Proceedings of the International Astronomical Union. IAUS 329: The Lives and Death-Throes of Massive Stars, 28 Nov - 02 Dec 2016, Auckland, New Zealand. Cambridge University Press , pp. 292-296. https://doi.org/10.1017/S1743921317002484 Reuse Unless indicated otherwise, fulltext items are protected by copyright with all rights reserved. The copyright exception in section 29 of the Copyright, Designs and Patents Act 1988 allows the making of a single copy solely for the purpose of non-commercial research or private study within the limits of fair dealing. The publisher or other rights-holder may allow further reproduction and re-use of this version - refer to the White Rose Research Online record for this item. Where records identify the publisher as the copyright holder, users can verify any specific terms of use on the publisher’s website. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ The lives and death-throes of massive stars Proceedings IAU Symposium No.
    [Show full text]
  • The VLT-FLAMES Tarantula Survey? XXIX
    A&A 618, A73 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833433 & c ESO 2018 Astrophysics The VLT-FLAMES Tarantula Survey? XXIX. Massive star formation in the local 30 Doradus starburst F. R. N. Schneider1, O. H. Ramírez-Agudelo2, F. Tramper3, J. M. Bestenlehner4,5, N. Castro6, H. Sana7, C. J. Evans2, C. Sabín-Sanjulián8, S. Simón-Díaz9,10, N. Langer11, L. Fossati12, G. Gräfener11, P. A. Crowther5, S. E. de Mink13, A. de Koter13,7, M. Gieles14, A. Herrero9,10, R. G. Izzard14,15, V. Kalari16, R. S. Klessen17, D. J. Lennon3, L. Mahy7, J. Maíz Apellániz18, N. Markova19, J. Th. van Loon20, J. S. Vink21, and N. R. Walborn22,?? 1 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK e-mail: [email protected] 2 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 3 European Space Astronomy Centre, Mission Operations Division, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 4 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 5 Department of Physics and Astronomy, Hicks Building, Hounsfield Road, University of Sheffield, Sheffield S3 7RH, UK 6 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA 7 Institute of Astrophysics, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 8 Departamento de Física y Astronomía, Universidad de La Serena, Avda. Juan Cisternas 1200, Norte, La Serena, Chile 9 Instituto de Astrofísica de Canarias, 38205 La Laguna,
    [Show full text]
  • The R136 Star Cluster Dissected with Hubble Space Telescope/STIS. II
    This is a repository copy of The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/166782/ Version: Accepted Version Article: Bestenlehner, J.M. orcid.org/0000-0002-0859-5139, Crowther, P.A., Caballero-Nieves, S.M. et al. (11 more authors) (2020) The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136. Monthly Notices of the Royal Astronomical Society. ISSN 0035-8711 https://doi.org/10.1093/mnras/staa2801 This is a pre-copyedited, author-produced version of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record [Joachim M Bestenlehner, Paul A Crowther, Saida M Caballero-Nieves, Fabian R N Schneider, Sergio Simón-Díaz, Sarah A Brands, Alex de Koter, Götz Gräfener, Artemio Herrero, Norbert Langer, Daniel J Lennon, Jesus Maíz Apellániz, Joachim Puls, Jorick S Vink, The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136, Monthly Notices of the Royal Astronomical Society, , staa2801] is available online at: https://doi.org/10.1093/mnras/staa2801 Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version.
    [Show full text]
  • 2Df-Aaomega Spectroscopy of Massive Stars in the Magellanic Clouds the North-Eastern Region of the Large Magellanic Cloud?,??
    A&A 584, A5 (2015) Astronomy DOI: 10.1051/0004-6361/201525882 & c ESO 2015 Astrophysics 2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds The north-eastern region of the Large Magellanic Cloud?;?? C. J. Evans1, J. Th. van Loon2, R. Hainich3, and M. Bailey4;2 1 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK e-mail: [email protected] 2 Astrophysics Group, School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, ST5 5BG, UK 3 Institute for Physics and Astronomy, University of Potsdam, 14476 Potsdam, Germany 4 Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park ic2, 146 Brownlow Hill, Liverpool L3 5RF, UK Received 13 February 2015 / Accepted 5 August 2015 ABSTRACT We present spectral classifications from optical spectroscopy of 263 massive stars in the north-eastern region of the Large Magellanic Cloud. The observed two-degree field includes the massive 30 Doradus star-forming region, the environs of SN1987A, and a number of star-forming complexes to the south of 30 Dor. These are the first classifications for the majority (203) of the stars and include eleven double-lined spectroscopic binaries. The sample also includes the first examples of early OC-type spectra (AAΩ 30 Dor 248 and 280), distinguished by the weakness of their nitrogen spectra and by C IV λ4658 emission. We propose that these stars have relatively unprocessed CNO abundances compared to morphologically normal O-type stars, indicative of an earlier evolutionary phase. From analysis of observations obtained on two consecutive nights, we present radial-velocity estimates for 233 stars, finding one apparent single-lined binary and nine (>3σ) outliers compared to the systemic velocity; the latter objects could be runaway stars or large-amplitude binary systems and further spectroscopy is required to investigate their nature.
    [Show full text]
  • Massive Runaway Stars in the Large Magellanic Cloud Sive (O2-Type) Stars Is Located at 100 200 Pc in Projection Table 1
    Astronomy & Astrophysics manuscript no. LMC2 c ESO 2018 October 14, 2018 Massive runaway stars in the Large Magellanic Cloud V.V. Gvaramadze1,2,3, P. Kroupa1, and J. Pflamm-Altenburg1 1 Argelander-Institut f¨ur Astronomie, Universit¨at Bonn, Auf dem H¨ugel 73, 53121 Bonn, Germany e-mail: [email protected] (PK); [email protected] (JP-A) 2 Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia e-mail: [email protected] (VVG) 3 Isaac Newton Institute of Chile, Moscow Branch, Universitetskij Pr. 13, Moscow 119992, Russia Received 27 April 2010/ Accepted 26 May 2010 ABSTRACT The origin of massive field stars in the Large Magellanic Cloud (LMC) has long been an enigma. The recent measurements of large 1 offsets ( 100 km s− ) between the heliocentric radial velocities of some very massive (O2-type) field stars and the systemic LMC velocity∼ provides a possible explanation of this enigma and suggests that the field stars are runaway stars ejected from their birthplaces at the very beginning of their parent cluster’s dynamical evolution. A straightforward way to prove this explanation is to measure the proper motions of the field stars and to show that they are moving away from one of the nearby star clusters or OB associations. This approach is, however, complicated by the long distance to the LMC, which makes accurate proper motion measurements difficult. We used an alternative approach for solving the problem (first applied for Galactic field stars), based on the search for bow shocks produced by runaway stars.
    [Show full text]
  • The R136 Star Cluster Dissected with Hubble Space Telescope/STIS
    MNRAS 000, 1–39 (2015) Preprint 29 January 2016 Compiled using MNRAS LATEXstylefilev3.0 The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He ii λ1640 in young star clusters Paul A. Crowther1⋆, S.M. Caballero-Nieves1, K.A. Bostroem2,3,J.Ma´ız Apell´aniz4, F.R.N. Schneider5,6,N.R.Walborn2,C.R.Angus1,7,I.Brott8,A.Bonanos9, A. de Koter10,11,S.E.deMink10,C.J.Evans12,G.Gr¨afener13,A.Herrero14,15, I.D. Howarth16, N. Langer6,D.J.Lennon17,J.Puls18,H.Sana2,11,J.S.Vink13 1Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA 3Department of Physics, University of California, Davis, 1 Shields Ave, Davis CA 95616, USA 4Centro de Astrobiologi´a, CSIC/INTA, Campus ESAC, Apartado Postal 78, E-28 691 Villanueva de la Ca˜nada, Madrid, Spain 5 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK 6 Argelanger-Institut fur¨ Astronomie der Universit¨at Bonn, Auf dem Hugel¨ 71, D-53121 Bonn, Germany 7 Department of Physics, University of Warwick, Gibbet Hill Rd, Coventry CV4 7AL, UK 8 Institute for Astrophysics, Tuerkenschanzstr. 17, AT-1180 Vienna, Austria 9 Institute of Astronomy & Astrophysics, National Observatory of Athens, I. Metaxa & Vas. Pavlou St, P. Penteli 15236, Greece 10 Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, Netherlands 11 Institute of Astronomy, KU Leuven, Celestijnenlaan
    [Show full text]
  • VLT-FLAMES Tarantula Survey
    VLT-FLAMES Tarantula Survey Alex de Koter University of Amsterdam & KU Leuven C.J. Evans (PI), W.D. Taylor, V. Hénault-Brunet, H. Sana, A. de Koter (O-star coordinator), S. Simón- Díaz, G. Carraro, T. Bagnoli, N. Bastian, J.M. Bestenlehner, A.Z. Bonanos, E. Bressert, I. Brott, M.A. Campbell, M. Cantiello, J.S. Clark, E. Costa, P.A. Crowther, S.E. de Mink, E. Doran, P.L. Dufton (B-star coordinator), P.R. Dunstall, K. Friedrich, M. Garcia, M. Gieles, G. Gräfener, A. Herrero, I.D. Howarth, R. G. Izzard, N. Langer, D.J. Lennon, J. Maíz Apellániz, N. Markova, F. Najarro, J. Puls, O.H. Ramirez, C. Sabín-Sanjulián, S.J. Smartt, V.E. Stroud, J.Th. van Loon, J.S. Vink, N.R. Walborn VLT-FLAMES Tarantula Survey PI: C. Evans Main catalogues Dynamics of the central region 1. Observing campaign and YSOs (Evans+2011) 11. Evidence for cluster rotation 2. Spectral typing & special categories (Walborn+2014) (Hénault-Brunet+ 2012a) 20XX) 12. R136 is virialized (Hénault-Brunet+ 2012b) 20XX) Individual objects Population properties 3. VFTS 016: most massive runaway star (Evans+2010) 13-14. Spin of the single O & B stars 4. R139: most massive evolved O-star pair (Taylor+2011) (Dufton+ 2013, Ramírez-Agudelo+2013) 4. VFTS 102: fastest spinning O star (Dufton+2011) 15. Spin of O star primaries (Ramírez-Agudelo+ in prep) 4. VFTS 698: peculiar B[e] supergiant (Dunstall+2012) 16-17. Multiplicity of the O & B stars (Sana+2013, Dunstall+2015) 5. VFTS 682: a 150 M star in appartent isolation (Bestenlehner+2011) 18.
    [Show full text]
  • The Electric Sun Hypothesis
    Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33
    [Show full text]
  • Uva-DARE (Digital Academic Repository)
    UvA-DARE (Digital Academic Repository) An empirical isochrone of very massive stars in R136a de Koter, A.; Heap, S.R.; Hubeny, I. DOI 10.1086/306503 Publication date 1998 Published in Astrophysical Journal Link to publication Citation for published version (APA): de Koter, A., Heap, S. R., & Hubeny, I. (1998). An empirical isochrone of very massive stars in R136a. Astrophysical Journal, 509, 879-896. https://doi.org/10.1086/306503 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:25 Sep 2021 THE ASTROPHYSICAL JOURNAL, 509:879È896, 1998 December 20 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. AN EMPIRICAL ISOCHRONE OF VERY MASSIVE STARS IN R136a1 ALEX DE KOTER,2,3 SARA R.
    [Show full text]