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Journal articles on the topic 'Very massive stars'

Author: Grafiati

Published: 14 March 2023

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1

Yusof, Norhasliza. "Wolf-Rayet stars from Very Massive Stars." Proceedings of the International Astronomical Union 9, S307 (June 2014): 152–53. http://dx.doi.org/10.1017/s1743921314006632.

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AbstractMany studies focused on very massive stars (VMS) within the framework of Pop. III stars, because this is where they were thought to be abundant. In this work, we focus on the evolution of VMS in the local universe following the discovery of VMS in the R136 cluster in the Large Magellanic Cloud (LMC). We computed grids of VMS evolutionary tracks in the range 120–500 M⊙ with solar, LMC and Small Magellanic Cloud metallicities. All models end their lives as Wolf-Rayet (WR) stars of the WC (or WO) type. We discuss the evolution and fate of VMS around solar metallicity with particular focus on the WR phase. For example, we show that a distinctive feature that may be used to disentangle Wolf-Rayet stars originating from VMS from those originating from lower initial masses is the enhanced abundances of Ne and Mg at the surface of WC stars.

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2

Heydari-Malayeri, M. "Multiplicity of Very Massive Stars." Symposium - International Astronomical Union 143 (1991): 645–46. http://dx.doi.org/10.1017/s0074180900046064.

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Are there very massive stars (VMSs) of mass greater than 100 M⊙? This question constitutes one of the fundamental problems of astrophysics. We present observational evidence against the existence of such stars in the Magellanic Clouds. The multiplicity of VMSs has several important consequences for astrophysics. If VMSs do not exist we need to revise our ideas about the formation and evolution of stars.

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3

Hirschi, R. "Very low-metallicity massive stars:." Astronomy & Astrophysics 461, no. 2 (October 9, 2006): 571–83. http://dx.doi.org/10.1051/0004-6361:20065356.

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4

Jørgen, Knut, and Røed Ødegaard. "Instabilities in Very Massive Stars." International Astronomical Union Colloquium 176 (2000): 391–92. http://dx.doi.org/10.1017/s0252921100058176.

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AbstractDetailed dynamical models and nucleosynthesis yields of very massive stars from early pre-MS through very late stages have been computed. The recent reduction of mass loss rates for the WR stages can have important consequences for both the evolution, surface composition and stability. Depending on mass and metallicity, in the present models instabilities occur during the accretion phase (pre-ZAMS), LBV stage and very late stages (WC).

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5

Chené, André-Nicolas, Olivier Schnurr, Paul A. Crowther, Eduardo F. Lajus, and Anthony F. J. Moffat. "Very massive binaries in R 136." Proceedings of the International Astronomical Union 6, S272 (July 2010): 497–98. http://dx.doi.org/10.1017/s174392131101115x.

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AbstractAs recent observations have shown, luminous, hydrogen-rich WN5-7h stars (and their somewhat less extreme cousins, O3f/WN6 stars) are the most massive main-sequence stars known. However, not nearly enough very massive stars have been reliably weighed to yield a clear picture of the upper initial-mass function (IMF). We therefore have carried out repeated high-quality spectroscopy of four new O3f/WN6 and WN5-7h binaries in R136 in the LMC with GMOS at Gemini-South, to derive Keplerian orbits for both components, respectively, and thus to directly determine their masses. We also monitored binary candidates and other, previously unsurveyed stars, to increase the number of very massive stars that can be directly weighed.

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6

Oh, Seungkyung, and Pavel Kroupa. "Very massive stars in not so massive clusters." Monthly Notices of the Royal Astronomical Society 481, no. 1 (August 18, 2018): 153–63. http://dx.doi.org/10.1093/mnras/sty2245.

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7

Belkus, H., J. Van Bever, and D. Vanbeveren. "The Evolution of Very Massive Stars." Astrophysical Journal 659, no. 2 (April 20, 2007): 1576–81. http://dx.doi.org/10.1086/512181.

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8

Davidson, Kris. "Giant eruptions of very massive stars." Journal of Physics: Conference Series 728 (July 2016): 022008. http://dx.doi.org/10.1088/1742-6596/728/2/022008.

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9

Bomans, Dominik J., and Kerstin Weis. "Massive variable stars at very low metallicity?" Proceedings of the International Astronomical Union 6, S272 (July 2010): 265–70. http://dx.doi.org/10.1017/s1743921311010519.

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AbstractObservational contraints on the evolution and instabilities of massive stars at very low metallicities are limited. Most of the information come from HST observations of one target, I Zw 18. Recent distance estimates of I Zw 18 put it at 17 Mpc, moving detailed studies of single stars clearly beyond the range of current ground based telescopes. Since massive stars with metallcities of 1/10 of solar and below are our best proxies for massive stars in (proto-) galaxies around the time of reionization, finding them and studying their evolution and instabilities is of premium importance for our understanding of galaxy formation, feedback, and the IGM reionization. Here we present pilot study results of variable stars in two more nearby extremely low metallicity galaxies, UGC 5340 and UGCA 292, and comment on the possibilities of more detailed studies of variable massive stars with new ground-based instrumentation.

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10

Dijkstra, M., and J. S. B. Wyithe. "Very massive stars in high-redshift galaxies." Monthly Notices of the Royal Astronomical Society 379, no. 4 (August 21, 2007): 1589–98. http://dx.doi.org/10.1111/j.1365-2966.2007.12039.x.

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11

Vink, Jorick S., Alexander Heger, Mark R. Krumholz, Joachim Puls, S. Banerjee, N. Castro, K. J. Chen, et al. "Very Massive Stars in the local Universe." Proceedings of the International Astronomical Union 10, H16 (August 2012): 51–79. http://dx.doi.org/10.1017/s1743921314004657.

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AbstractRecent studies have claimed the existence of very massive stars (VMS) up to 300M⊙in the local Universe. As this finding may represent a paradigm shift for the canonical stellar upper-mass limit of 150M⊙, it is timely to discuss the status of the data, as well as the far-reaching implications of such objects. We held a Joint Discussion at the General Assembly in Beijing to discuss (i) the determination of the current masses of the most massive stars, (ii) the formation of VMS, (iii) their mass loss, and (iv) their evolution and final fate. The prime aim was to reach broad consensus between observers and theorists on how to identify and quantify the dominant physical processes.

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12

Goodman, J., and Christopher J. White. "Stability of metal-rich very massive stars." Monthly Notices of the Royal Astronomical Society 456, no. 1 (December 16, 2015): 525–37. http://dx.doi.org/10.1093/mnras/stv2694.

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13

Negueruela, I., A. Marco, A. Herrero, and J. S. Clark. "New very massive stars in Cygnus OB2." Astronomy & Astrophysics 487, no. 2 (June 24, 2008): 575–81. http://dx.doi.org/10.1051/0004-6361:200810094.

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14

Yusof, Norhasliza, Raphael Hirschi, Georges Meynet, Paul A. Crowther, Sylvia Ekström, Urs Frischknecht, Cyril Georgy, Hasan Abu Kassim, and Olivier Schnurr. "Evolution and fate of very massive stars." Monthly Notices of the Royal Astronomical Society 433, no. 2 (June 3, 2013): 1114–32. http://dx.doi.org/10.1093/mnras/stt794.

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15

Vanbeveren, Dany. "The evolution of massive and very massive stars in clusters." New Astronomy Reviews 53, no. 1-2 (May 2009): 27–35. http://dx.doi.org/10.1016/j.newar.2009.03.001.

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16

Bagnulo, S., G. A. Wade, Y. Nazé, J. H. Grunhut, M. E. Shultz, D. J. Asher, P. A. Crowther, et al. "A search for strong magnetic fields in massive and very massive stars in the Magellanic Clouds." Astronomy & Astrophysics 635 (March 2020): A163. http://dx.doi.org/10.1051/0004-6361/201937098.

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Despite their rarity, massive stars dominate the ecology of galaxies via their strong, radiatively-driven winds throughout their lives and as supernovae in their deaths. However, their evolution and subsequent impact on their environment can be significantly affected by the presence of a magnetic field. While recent studies indicate that about 7% of OB stars in the Milky Way host strong, stable, organised (fossil) magnetic fields at their surfaces, little is known about the fields of very massive stars, nor the magnetic properties of stars outside our Galaxy. We aim to continue searching for strong magnetic fields in a diverse set of massive and very massive stars (VMS) in the Large and Small Magellanic Clouds (LMC/SMC), and we evaluate the overall capability of FORS2 to usefully search for and detect stellar magnetic fields in extra-galactic environments. We have obtained FORS2 spectropolarimetry of a sample of 41 stars, which principally consist of spectral types B, O, Of/WN, WNh, and classical WR stars in the LMC and SMC. Four of our targets are Of?p stars; one of them was just recently discovered. Each spectrum was analysed to infer the longitudinal magnetic field. No magnetic fields were formally detected in our study, although Bayesian statistical considerations suggest that the Of?p star SMC 159-2 is magnetic with a dipolar field of the order of 2.4–4.4 kG. In addition, our first constraints of magnetic fields in VMS provide interesting insights into the formation of the most massive stars in the Universe.

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17

Ekström, Sylvia, Georges Meynet, and André Maeder. "Can Very Massive Stars Avoid Pair-Instability Supernovae?" Proceedings of the International Astronomical Union 3, S250 (December 2007): 209–16. http://dx.doi.org/10.1017/s1743921308020516.

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AbstractVery massive primordial stars (140 M⊙ < M < 260 M⊙) are supposed to end their lives as PISN. Such an event can be traced by a typical chemical signature in low metallicity stars, but at the present time, this signature is lacking in the extremely metal-poor stars we are able to observe. Does it mean that those very massive objects were not formed, contrarily to the primordial star formation scenarios ? Could it be possible that they avoided this tragic fate ?We explore the effects of rotation, anisotropical mass loss and magnetic field on the core size of very massive Population III models. We find that magnetic fields provide the strong coupling that is lacking in standard evolution metal-free models and our 150 M⊙ Population III model avoids indeed the pair-instability explosion.

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18

Smith, Nathan. "Luminous blue variables and the fates of very massive stars." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2105 (September 18, 2017): 20160268. http://dx.doi.org/10.1098/rsta.2016.0268.

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Luminous blue variables (LBVs) had long been considered massive stars in transition to the Wolf–Rayet (WR) phase, so their identification as progenitors of some peculiar supernovae (SNe) was surprising. More recently, environment statistics of LBVs show that most of them cannot be in transition to the WR phase after all, because LBVs are more isolated than allowed in this scenario. Additionally, the high-mass H shells around luminous SNe IIn require that some very massive stars above 40 M ⊙ die without shedding their H envelopes, and the precursor outbursts are a challenge for understanding the final burning sequences leading to core collapse. Recent evidence suggests a clear continuum in pre-SN mass loss from super-luminous SNe IIn, to regular SNe IIn, to SNe II-L and II-P, whereas most stripped-envelope SNe seem to arise from a separate channel of lower-mass binary stars rather than massive WR stars. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.

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19

Salvadori, S., P. Bonifacio, E. Caffau, S. Korotin, S. Andreevsky, M. Spite, and Á. Skúladóttir. "Probing the existence of very massive first stars." Monthly Notices of the Royal Astronomical Society 487, no. 3 (May 31, 2019): 4261–84. http://dx.doi.org/10.1093/mnras/stz1464.

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20

Kashi, Amit, Kris Davidson, and Roberta M. Humphreys. "RECOVERY FROM GIANT ERUPTIONS IN VERY MASSIVE STARS." Astrophysical Journal 817, no. 1 (January 22, 2016): 66. http://dx.doi.org/10.3847/0004-637x/817/1/66.

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21

Gvaramadze, Vasilii V., and Alessia Gualandris. "Very massive runaway stars from three-body encounters." Monthly Notices of the Royal Astronomical Society 410, no. 1 (September 30, 2010): 304–12. http://dx.doi.org/10.1111/j.1365-2966.2010.17446.x.

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22

Heger, A., I. Baraffe, C. L. Fryer, and S. E. Woosley. "Evolution and nucleosynthesis of very massive primordial stars." Nuclear Physics A 688, no. 1-2 (May 2001): 197–200. http://dx.doi.org/10.1016/s0375-9474(01)00697-2.

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23

Schneider, R., A. Ferrara, P. Natarajan, and K. Omukai. "First Stars, Very Massive Black Holes, and Metals." Astrophysical Journal 571, no. 1 (May 20, 2002): 30–39. http://dx.doi.org/10.1086/339917.

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24

Baraffe, I., A. Heger, and S. E. Woosley. "On the Stability of Very Massive Primordial Stars." Astrophysical Journal 550, no. 2 (April 2001): 890–96. http://dx.doi.org/10.1086/319808.

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25

Eenens, Philippe, Joseph Cassinelli, Peter Conti, Catharine Garmany, Karel van der Hucht, Rolf Kudritzki, Henny Lamers, André Maeder, Anthony Moffat, and Stanley Owocki. "Working Group on Hot Massive Stars (Groupe De Travail Sur Les Etoiles Massives Chaudes)." Transactions of the International Astronomical Union 24, no. 1 (2000): 176–85. http://dx.doi.org/10.1017/s0251107x00002844.

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The Working Group on Hot Massive Stars has been officially recognized by the IAU Executive Committee during the XXIII General Assembly in August 1997. Its origins are the Hot Star Newsletter, launched in 1994, and a long tradition of interaction and collaborative research strengthened by a series of meetings on hot beaches. It gathers over 500 researchers working on OB stars, Luminous Blue Variables, Wolf-Rayet stars, and in general all topics related to the evolution of massive stars and to the physics and consequences of winds from hot stars. The very successful recent symposium on “Wolf-Rayet phenomena in massive stars and starburst galaxies” is an indicator of the increasing interest of the extragalactic community in the study of these extraordinary stars.

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26

Belkus, Houria, Joris Van Bever, and Dany Vanbeveren. "The Formation and Evolution of Very Massive Stars in Dense Stellar Systems." Proceedings of the International Astronomical Union 3, S246 (September 2007): 357–58. http://dx.doi.org/10.1017/s1743921308015925.

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AbstractThe early evolution of dense stellar systems is governed by massive single star and binary evolution. Core collapse of dense massive star clusters can lead to the formation of very massive objects through stellar collisions (M≥ 1000M⊙). Stellar wind mass loss determines the evolution and final fate of these objects, and determines whether they form black holes (with stellar or intermediate mass) or explode as pair instability supernovae, leaving no remnant. We present a computationally inexpensive evolutionary scheme for very massive stars that can readily be implemented in an N-body code. Using our new N-body code ‘Youngbody’ which includes a detailed treatment of massive stars as well as this new scheme for very massive stars, we discuss the formation of intermediate mass and stellar mass black holes in young starburst regions. A more detailed account of these results can be found in Belkus, Van Bever & Vanbeveren (2007).

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27

Volpato, Guglielmo, Paola Marigo, Guglielmo Costa, Alessandro Bressan, Michele Trabucchi, and Léo Girardi. "A Study of Primordial Very Massive Star Evolution." Astrophysical Journal 944, no. 1 (February 1, 2023): 40. http://dx.doi.org/10.3847/1538-4357/acac91.

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Abstract We present new evolutionary models of primordial very massive stars with initial masses ranging from 100 to 1000 M ⊙ that extend from the main sequence to the onset of dynamical instability caused by the creation of electron–positron pairs during core C, Ne, or O burning, depending on the star’s mass and metallicity. Mass loss accounts for radiation-driven winds, as well as pulsation-driven mass loss on the main sequence and during the red supergiant phase. After examining the evolutionary properties, we focus on the final outcome of the models and associated compact remnants. Stars that avoid the pair instability supernova channel should produce black holes with masses ranging from ≈40 to ≈1000 M ⊙. In particular, stars with initial masses of about 100 M ⊙ could leave black holes of ≃85–90 M ⊙, values consistent with the estimated primary black hole mass of the GW190521 merger event. Overall, these results may contribute to explaining future data from next-generation gravitational-wave detectors, such as the Einstein Telescope and Cosmic Explorer, which will have access to an as-yet-unexplored black hole mass range of ≈102–104 M ⊙ in the early universe.

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28

Lomax, Jamie R., Matthew Peters, John Wisniewski, Julianne Dalcanton, Benjamin Williams, Julie Lutz, Yumi Choi, and Aaron Sigut. "Massive Stars in M31." Proceedings of the International Astronomical Union 12, S329 (November 2016): 419. http://dx.doi.org/10.1017/s1743921317002599.

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AbstractMassive stars are intrinsically rare and therefore present a challenge to understand from a statistical perspective, especially within the Milky Way. We recently conducted follow-up observations to the Panchromatic Hubble Andromeda Treasury (PHAT) survey that were designed to detect more than 10,000 emission line stars, including WRs, by targeting regions in M31 previously known to host large numbers of young, massive clusters and very young stellar populations. Because of the existing PHAT data, we are able to derive an effective temperature, bolarimetric luminosity, and extinction for each of our detected stars. We report on preliminary results of the massive star population of our dataset and discuss how our results compare to previous studies of massive stars in M31.

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29

Garba, L., E. A. Chidi, and F. S. Koki. "Evaluation of thermal- nuclear effects from pair-creation in the final fate very-massive stars." Bayero Journal of Pure and Applied Sciences 14, no. 1 (December 21, 2021): 237–50. http://dx.doi.org/10.4314/bajopas.v14i1.28.

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Thermonuclear conditions found in explosive massive-stars requirethe use of not only efficient, accurate but thermodynamically consistent stellar equation of state (EOS) routines.The use of tables to describe EoS involved in stellar models is very much needed in understanding the final fate of massive stars. Many massive-low metallicity stars end their life as pair creation supernova (PCSN) through the creation of electron-positron pairs.We used thermodynamically consistent EoS tables to numerically evaluate the thermonuclear effects of the electron electron-positron pair creation in rotating 150 and 200 Massive starsat SMC and rotating and non-rotating 500 M⊙at LMC.As expected, the effect of rotationofreducing the oxygen core masshad increasedthe thermal energy within the threshold of the pair-creation instability.Similarly, lower mass loss stars with SMC model produced higher thermal energies,which can cmpletely explode the stars as PCSNe without remnant.On the other hand, the non-rotating 500 M⊙ might have only reached the instability region due to its lower metallicity (compared to solar metallicity) that iscapable of suppressing the mass loss such that the thermonuclear energy maintains certain amount of elements into the pair creation region. At the final explosion of the stars, the helium core mass educed the thermal energies in trying to avoid the pair-creation region. Many implications of these results for the evolution and explosion of massive stars are discussed.

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30

Fukushima, Hajime, Takashi Hosokawa, Gen Chiaki, Kazuyuki Omukai, Naoki Yoshida, and Rolf Kuiper. "Formation of massive stars under protostellar radiation feedback: very metal-poor stars." Monthly Notices of the Royal Astronomical Society 497, no. 1 (July 9, 2020): 829–45. http://dx.doi.org/10.1093/mnras/staa1994.

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ABSTRACT We study the formation of very metal-poor stars under protostellar radiative feedback effect. We use cosmological simulations to identify low-mass dark matter haloes and star-forming gas clouds within them. We then follow protostar formation and the subsequent long-term mass accretion phase of over one million years using two-dimensional radiation-hydrodynamics simulations. We show that the critical physical process that sets the final mass is the formation and expansion of a bipolar H ii region. The process is similar to the formation of massive primordial stars, but radiation pressure exerted on dust grains also contributes to halting the accretion flow in the low-metallicity case. We find that the net feedback effect in the case with metallicity Z = 10−2 Z⊙ is stronger than in the case with Z ∼ 1 Z⊙. With decreasing metallicity, the radiation-pressure effect becomes weaker, but photoionization heating of the circumstellar gas is more efficient owing to the reduced dust attenuation. In the case with Z = 10−2 Z⊙, the central star grows as massive as 200 solar masses, similarly to the case of primordial star formation. We conclude that metal-poor stars with a few hundred solar masses can be formed by gas accretion despite the strong radiative feedback.

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31

Leung, Kam-Ching. "Massive Contact Binary Systems." Symposium - International Astronomical Union 143 (1991): 207–12. http://dx.doi.org/10.1017/s0074180900045162.

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In recent years very massive single stars have been found to be upward of 90 M⊙. Massive contact binary systems have been found among the early-type systems, but their masses are far less than those reported for single stars. The most massive component found is about 60 M⊙.It is generally believed that no late-type very massive stars have been detected (Humphreys and Davidson). This may be due to the large amount of mass loss from stellar wind. Recently, several extremely long-period late-type binary systems have been found to be contact systems. Two systems, UU Cnc and 5 Cet, have their primary components with masses exceeding 40 M⊙, and K spectra. This result tends to suggest that close or interacting binary stars may be able to preserve the mass loss from stellar wind within the binary systems.

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32

Meyer, D. M.-A., M. Petrov, and M. Pohl. "Wind nebulae and supernova remnants of very massive stars." Monthly Notices of the Royal Astronomical Society 493, no. 3 (February 26, 2020): 3548–64. http://dx.doi.org/10.1093/mnras/staa554.

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ABSTRACT A very small fraction of (runaway) massive stars have masses exceeding $60\!-\!70\, \rm M_{\odot }$ and are predicted to evolve as luminous blue variable and Wolf–Rayet stars before ending their lives as core-collapse supernovae. Our 2D axisymmetric hydrodynamical simulations explore how a fast wind ($2000\, \rm km\, \rm s^{-1}$) and high mass-loss rate ($10^{-5}\, \rm M_{\odot }\, \rm yr^{-1}$) can impact the morphology of the circumstellar medium. It is shaped as 100 pc-scale wind nebula that can be pierced by the driving star when it supersonically moves with velocity $20\!-\!40\, \rm km\, \rm s^{-1}$ through the interstellar medium (ISM) in the Galactic plane. The motion of such runaway stars displaces the position of the supernova explosion out of their bow shock nebula, imposing asymmetries to the eventual shock wave expansion and engendering Cygnus-loop-like supernova remnants. We conclude that the size (up to more than $200\, \rm pc$) of the filamentary wind cavity in which the chemically enriched supernova ejecta expand, mixing efficiently the wind and ISM materials by at least $10{{\ \rm per\ cent}}$ in number density, can be used as a tracer of the runaway nature of the very massive progenitors of such $0.1\, \rm Myr$ old remnants. Our results motivate further observational campaigns devoted to the bow shock of the very massive stars BD+43°3654 and to the close surroundings of the synchrotron-emitting Wolf–Rayet shell G2.4+1.4.

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33

Brandl, Bernhard R., David F. Chernoff, and Anthony F. J. Moffat. "Massive Stars Ejected from R136?" Symposium - International Astronomical Union 207 (2002): 694–96. http://dx.doi.org/10.1017/s0074180900224571.

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We present the observational signature of a statistically significant number of very massive stars around the core of R136 and discuss the evidence for dynamical processes to be responsible for their apparent location. Alternative scenarios are discussed as well.

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34

Preibisch, Thomas, Gerd Weigelt, and Hans Zinnecker. "Multiplicity of Massive Stars." Symposium - International Astronomical Union 200 (2001): 69–78. http://dx.doi.org/10.1017/s0074180900225072.

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We discuss the observed multiplicity of massive stars and implications on theories of massive star formation. After a short summary of the literature on massive star multiplicity, we focus on the O-and B-type stars in the Orion Nebula Cluster, which constitute a homogenous sample of very young massive stars. 13 of these stars have recently been the targets of a bispectrum speckle interferometry survey for companions. Considering the visual and also the known spectroscopic companions of these stars, the total number of companions is at least 14. Extrapolation with correction for the unresolved systems suggests that there are at least 1.5 and perhaps as much as 4 companions per primary star on average. This number is clearly higher than the mean number of ∼ 0.5 companions per primary star found for the low-mass stars in the general field population and also in the Orion Nebula cluster. This suggests that a different mechanism is at work in the formation of high-mass multiple systems in the dense Orion Nebula cluster than for low-mass stars.

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35

Lee, H. M. "Dynamics of Galactic Nuclei Containing Massive Remnant Stars." Symposium - International Astronomical Union 174 (1996): 293–302. http://dx.doi.org/10.1017/s0074180900001637.

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We have examined the dynamical evolution of stellar system containing massive remnant stellar component. If individual mass of remnant stars is much heavier than that of normal stars which comprise most of the mass in the cluster, remnant stars quickly form a subsystem within the core of cluster of ordinary stars. The subsystem evolves on its own relaxation time scale which is very short. However, the post collapse expansion driven by the three-body binary heating becomes very slow because the expansion energy of the compact subcluster can be easily absorbed by surrounding cluster. The gravitational radiation can lead to the merger of binaries when binaries become very hard. A central seed black hole might form if repeated merger becomes very efficient. Otherwise, relatively stable two-component phase of central compact cluster of remnant stars surrounded by larger cluster of low mass stars would last for a long time.

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36

Han, Sophia, and Madappa Prakash. "On the Minimum Radius of Very Massive Neutron Stars." Astrophysical Journal 899, no. 2 (August 26, 2020): 164. http://dx.doi.org/10.3847/1538-4357/aba3c7.

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37

Aoki, W., N. Tominaga, T. C. Beers, S. Honda, and Y. S. Lee. "A chemical signature of first-generation very massive stars." Science 345, no. 6199 (August 21, 2014): 912–15. http://dx.doi.org/10.1126/science.1252633.

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38

Kalari, V. M., J. S. Vink, W. J. de Wit, N. J. Bastian, and R. A. Méndez. "The origin of very massive stars around NGC 3603." Astronomy & Astrophysics 625 (May 2019): L2. http://dx.doi.org/10.1051/0004-6361/201935107.

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The formation mechanism of the most massive stars in the Universe remains an unsolved problem. Are they able to form in relative isolation in a manner similar to the formation of solar-type stars, or do they necessarily require a clustered environment? In order to shed light on this important question, we study the origin of two very massive stars (VMS): the O2.5If*/WN6 star RFS7 (∼100 M⊙), and the O3.5If* star RFS8 (∼70 M⊙), found within ∼53 and 58 pc, respectively, of the Galactic massive young cluster NGC 3603, using Gaia data. The star RFS7 is found to exhibit motions resembling a runaway star from NGC 3603. This is now the most massive runaway star candidate known in the Milky Way. Although RFS8 also appears to move away from the cluster core, it has proper-motion values that appear inconsistent with being a runaway from NGC 3603 at the 3σ level (but with substantial uncertainties due to distance and age). Furthermore, no evidence for a bow-shock or a cluster was found surrounding RFS8 from available near-infrared photometry. In summary, whilst RFS7 is likely a runaway star from NGC 3603, making it the first VMS runaway in the Milky Way, RFS8 is an extremely young (∼2 Myr) VMS, which might also be a runaway, but this would need to be established from future spectroscopic and astrometric observations, as well as precise distances. If RFS 8 was still not found to meet the criteria for being a runaway from NGC 3603 from such future data, this would have important ramifications for current theories of massive star formation, as well as the way the stellar initial mass function is sampled.

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Chen, Ke-Jung, Alexander Heger, Stan Woosley, Ann Almgren, and Daniel J. Whalen. "PAIR INSTABILITY SUPERNOVAE OF VERY MASSIVE POPULATION III STARS." Astrophysical Journal 792, no. 1 (August 13, 2014): 44. http://dx.doi.org/10.1088/0004-637x/792/1/44.

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40

Moeckel, Nickolas, and Cathie J. Clarke. "Collisional formation of very massive stars in dense clusters." Monthly Notices of the Royal Astronomical Society 410, no. 4 (November 12, 2010): 2799–806. http://dx.doi.org/10.1111/j.1365-2966.2010.17659.x.

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41

Ohkubo, Takuya, H. Umeda, K. Maeda, K. Nomoto, S. Tsuruta, and M. J. Rees. "Population III Very-Massive Stars—Their Evolution and Explosion." Proceedings of the International Astronomical Union 1, S228 (May 2005): 167–68. http://dx.doi.org/10.1017/s1743921305005508.

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42

Dubus, Guillaume, and Benoît Cerutti. "Massive stars at (very) high energies: γ-ray binaries." Proceedings of the International Astronomical Union 6, S272 (July 2010): 581–86. http://dx.doi.org/10.1017/s174392131101146x.

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Abstractγ-ray binaries are systems that emit most of their radiative power above 1 MeV. They are associated with O or Be stars in orbit with a compact object, possibly a young pulsar. Much like colliding wind binaries, the pulsar generates a relativistic wind that interacts with the stellar wind. The result is non-thermal emission from radio to very high energy γ-rays. The wind, radiation and magnetic field of the massive star play a major role in the dynamics and radiative output of the system. They are particularly important to understand the high energy physics at work. Inversely, γ-ray binaries offer novel probes of stellar winds and insights into the fate of O/B binaries.

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43

de Koter, Alex, Sara R. Heap, and Ivan Hubeny. "An Empirical Isochrone of Very Massive Stars in R136a." Astrophysical Journal 509, no. 2 (December 20, 1998): 879–96. http://dx.doi.org/10.1086/306503.

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44

G�rtler, J., and Th Henning. "Circumstellar dust shells around very young and massive stars." Astrophysics and Space Science 128, no. 1 (1986): 163–77. http://dx.doi.org/10.1007/bf00656028.

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45

Wise, John H., and Tom Abel. "How Very Massive Metal‐Free Stars Start Cosmological Reionization." Astrophysical Journal 684, no. 1 (September 2008): 1–17. http://dx.doi.org/10.1086/590050.

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46

Oh, S. Peng, Kenneth M. Nollett, Piero Madau, and G. J. Wasserburg. "Did Very Massive Stars Preenrich and Reionize the Universe?" Astrophysical Journal 562, no. 1 (November 20, 2001): L1—L4. http://dx.doi.org/10.1086/337996.

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47

Tsuruta, Sachiko, Takuya Ohkubo, Hideyuki Umeda, Keiichi Maeda, Ken'ichi Nomoto, Tomoharu Suzuki, and Martin J. Rees. "Explosion of very massive stars and the origin of intermediate mass black holes." Proceedings of the International Astronomical Union 2, S238 (August 2006): 241–46. http://dx.doi.org/10.1017/s1743921307005054.

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AbstractWe calculate evolution, collapse, explosion, and nucleosynthesis of Population III very massive stars with 500 M⊙ and 1000 M⊙. It was found that both 500 M⊙ and 1000 M⊙ models enter the region of pair-instability but continue to undergo core collapse to black holes. For moderately aspherical explosions, the patterns of nucleosynthesis match the observational data of intergalactic and intercluster medium and hot gases in M82, better than models involving hypernovae and pair instability supernovae.Our results suggest that explosions of Population III core-collapse very massive stars contribute significantly to the chemical evolution of gases in clusters of galaxies. The final black hole masses are about 500 M⊙ for our most massive 1000 M⊙ models. This result may support the view that Population III very massive stars are responsible for the origin of intermediate mass black holes which were recently reported to be discovered.

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48

Hanson, Margaret M., Lex Kaper, Arjan Bik, Fernando Comerón, Joachim Puls, Alexander Jokuthy, and Rolf-Peter Kudritzki. "Stellar content of obscured compact H II regions." Symposium - International Astronomical Union 212 (2003): 467–73. http://dx.doi.org/10.1017/s0074180900212655.

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Near-infrared, spectroscopic studies of central ionizing sources of very young H ii regions is presented in conjunction with a recently available, sophisticated atmospheric code to constrain the physical conditions and environment of very massive stars at very early stages of evolution. Combining high quality near-infrared spectroscopy of very young massive stars with model atmosphere calculations should allow for the most accurate quantitative determination of Teff, rotation, L, and log g, and to search for binaries and possible disk or in-fall signatures in forming or recently formed massive stars. These characteristics make up a vital boundary condition constraining theories on massive star formation.

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Marigo, Paola, Cesare Chiosi, Léo Girardi, and Rolf-Peter Kudritzki. "Evolution of zero-metallicity massive stars." Symposium - International Astronomical Union 212 (2003): 334–40. http://dx.doi.org/10.1017/s0074180900212400.

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We discuss the evolutionary properties of primordial massive and very massive stars, supposed to have formed from metal-free gas. Stellar models are presented over a large range of initial masses (8 M⊙ ≲ Mi ≲ 1000 M⊙), covering the hydrogen- and helium-burning phases up to the onset of carbon burning. In most cases the evolution is followed at constant mass. To estimate the possible effect of mass loss via stellar winds, recent analytic formalisms for the mass-loss rates are applied to the very massive models (Mi ≥ 120 M⊙).

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50

Rubio-Díez, M. M., F. Najarro, M. García, and J. O. Sundqvist. "Re-examing the Upper Mass Limit of Very Massive Stars: VFTS 682, an isolated ~130 M⊙ twin of R136’s WN5h core stars." Proceedings of the International Astronomical Union 12, S329 (November 2016): 131–35. http://dx.doi.org/10.1017/s1743921317002447.

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AbstractRecent studies of WNh stars at the cores of young massive clusters have challenged the previously accepted upper stellar mass limit (~150 M⊙), suggesting some of these objects may have initial masses as high as 300 M⊙. We investigated the possible existence of observed stars above ~150 M⊙ by i) examining the nature and stellar properties of VFTS 682, a recently identified WNh5 very massive star, and ii) studying the uncertainties in the luminosity estimates of R136’s core stars due to crowding. Our spectroscopic analysis reveals that the most massive members of R136 and VFTS 682 are very similar and our K-band photometric study of R136’s core stars shows that the measurements seem to display higher uncertainties than previous studies suggested; moreover, for the most massive stars in the cluster, R136a1 and a2, we found previous magnitudes were underestimated by at least 0.4 mag. As such, luminosities and masses of these stars have to be significantly scaled down, which then also lowers the hitherto observed upper mass limit of stars.

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