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Journal articles on the topic 'Very massive stars'

Author: Grafiati

Published: 14 March 2023

Last updated: 31 July 2025

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1

Yusof, Norhasliza. "Wolf-Rayet stars from Very Massive Stars." Proceedings of the International Astronomical Union 9, S307 (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

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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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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 (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

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4

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

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5

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

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7

Bomans, Dominik J., and Kerstin Weis. "Massive variable stars at very low metallicity?" Proceedings of the International Astronomical Union 6, S272 (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 fo

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8

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

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9

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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10

Martinet, Sébastien, Georges Meynet, Sylvia Ekström, et al. "Very Massive Stars: Near and Far." Proceedings of the International Astronomical Union 18, S361 (2022): 369–75. http://dx.doi.org/10.1017/s1743921322002149.

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AbstractIn addition to being spectacular objects, very massive stars (VMS) are suspected to have a tremendous impact on their environment and on the whole cosmic evolution. The nucleosynthesis both during their advanced stages and their final explosion likely contribute greatly to the overall enrichment of the Universe. Their resulting Supernovae are candidates for the most superluminous events and their extreme conditions lead also to very important radiative and mechanical feedback effects, from local to cosmic scale. With the recent implementation of a new equation of state in the GENEC ste

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11

Garcia, Miriam. "Observations of Very Low-Metallicity Massive Stars." Proceedings of the International Astronomical Union 18, S361 (2022): 36–45. http://dx.doi.org/10.1017/s174392132200312x.

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AbstractVery metal-poor massive stars hold the key to interpret high-redshift star-forming galaxies and the early reionization epoch, but also contemporary events such as gravitational waves. To study these objects in resolved environments, we need to resort to dwarf irregular galaxies far from the potential wells of M31 and the Milky Way, and therefore distant. While the archives, recently boosted by the ULLYSES and XSHOOTU programs, store a healthy dataset of massive stars in the Milky Way and the Magellanic Clouds, the number of observed targets with poorer metal content than the SMC (1/5 Z

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12

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

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13

Vink, Jorick S., Alexander Heger, Mark R. Krumholz, et al. "Very Massive Stars in the local Universe." Proceedings of the International Astronomical Union 10, H16 (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 betw

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14

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

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15

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

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16

Yusof, Norhasliza, Raphael Hirschi, Georges Meynet, et al. "Evolution and fate of very massive stars." Monthly Notices of the Royal Astronomical Society 433, no. 2 (2013): 1114–32. http://dx.doi.org/10.1093/mnras/stt794.

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17

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

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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 (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 th

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19

Eenens, Philippe, Joseph Cassinelli, Peter Conti, et al. "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-Ray

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20

Bagnulo, S., G. A. Wade, Y. Nazé, 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 s

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21

Ekström, Sylvia, Georges Meynet, and André Maeder. "Can Very Massive Stars Avoid Pair-Instability Supernovae?" Proceedings of the International Astronomical Union 3, S250 (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

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22

Yang, Shuaishuai, Shichao Zhang, Lu Zhang, and Hongjie Li. "A Study of Abundance Patterns in the Sextans and Sculptor Dwarf Spheroidal Galaxies." Astrophysical Journal 981, no. 2 (2025): 155. https://doi.org/10.3847/1538-4357/adb57c.

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Abstract In this work, we employ a multicomponent decomposition model to study the Sextans and Sculptor dwarf spheroidal galaxies, which have distinct evolutionary histories. Sextans exhibits massive stars dominating in the early stages of its evolution and a lower contribution from type Ia supernovae (SNe Ia). With increasing metallicity, the evolution of massive stars in Sextans shows two turning points, at [Fe/H] ∼ −2.8 and [Fe/H] ∼ −2.0, indicating episodes of accretion events and galactic winds during its evolution. In the late stages, influenced by galactic winds, the contribution from m

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23

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 (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 c

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24

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 (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

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25

Lei 雷, Lei 磊., Yi-Ying 艺颖 Wang 王, Guan-Wen 官文 Yuan 袁, Tong-Lin 彤琳 Wang 王, Martin A. T. Groenewegen, and Yi-Zhong 一中 Fan 范. "Can Dark Stars Account for the Star Formation Efficiency Excess at Very High Redshifts?" Astrophysical Journal 980, no. 2 (2025): 249. https://doi.org/10.3847/1538-4357/ada93b.

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Abstract The James Webb Space Telescope (JWST) has recently conducted observations of massive galaxies at high redshifts, revealing a notable anomaly in their star formation efficiency (SFE). Motivated by the recent identification of three ~106 M ⊙ dark star candidates, we investigate whether dark stars can be the origin of the SFE excess. It turns out that the excess can be reproduced by a group of dark stars with M ≳ 103 M ⊙, because of their domination in generating primary UV radiation in high-redshift galaxies. The genesis of these dark stars is attributed to the capture of weakly interac

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26

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 prima

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27

Salvadori, S., P. Bonifacio, E. Caffau, et al. "Probing the existence of very massive first stars." Monthly Notices of the Royal Astronomical Society 487, no. 3 (2019): 4261–84. http://dx.doi.org/10.1093/mnras/stz1464.

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28

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

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

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30

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 (2001): 197–200. http://dx.doi.org/10.1016/s0375-9474(01)00697-2.

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31

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

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32

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

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33

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 (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 t

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34

Hanson, Margaret M., Lex Kaper, Arjan Bik, et al. "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

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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 gravita

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36

Lomax, Jamie R., Matthew Peters, John Wisniewski, et al. "Massive Stars in M31." Proceedings of the International Astronomical Union 12, S329 (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 fo

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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 (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\,

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Tsuruta, Sachiko, Takuya Ohkubo, Hideyuki Umeda, et al. "Explosion of very massive stars and the origin of intermediate mass black holes." Proceedings of the International Astronomical Union 2, S238 (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 cont

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39

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 (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 ve

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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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41

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 (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 pressu

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Vink, Jorick S. "Mass loss and stellar superwinds." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2105 (2017): 20160269. http://dx.doi.org/10.1098/rsta.2016.0269.

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Mass loss bridges the gap between massive stars and supernovae (SNe) in two major ways: (i) theoretically, it is the amount of mass lost that determines the mass of the star prior to explosion and (ii) observations of the circumstellar material around SNe may teach us the type of progenitor that made the SN. Here, I present the latest models and observations of mass loss from massive stars, both for canonical massive O stars, as well as very massive stars that show Wolf–Rayet type features. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.

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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

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Sabhahit, Gautham N., Jorick S. Vink, Erin R. Higgins, and Andreas A. C. Sander. "Mass loss implementation and temperature evolution of very massive stars." Proceedings of the International Astronomical Union 17, S370 (2021): 263–68. http://dx.doi.org/10.1017/s1743921322003623.

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AbstractVery massive stars (VMS) dominate the physics of young clusters due to their extreme stellar winds. The mass lost by these stars in their winds determine their evolution, chemical yields and their end fates. In this contribution we study the main-sequence evolution of VMS with a new mass-loss recipe that switches from optically-thin O star winds to optically-thick Wolf-Rayet type winds through the model independent transition mass loss.

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45

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

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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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Beradze, Sopia, and Nino Kochiashvili. "Observations of Bright Massive Stars Using Small Size Telescopes." Proceedings of the International Astronomical Union 12, S329 (2016): 385. http://dx.doi.org/10.1017/s1743921317002526.

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AbstractThe size of a telescope determines goals and objects of observations. During the latest decades it becomes more and more difficult to get photometric data of bright stars because most of telescopes of small sizes do not operate already. But there are rather interesting questions connected to the properties and evolution ties between different types of massive stars. Multi-wavelength photometric data are needed for solution of some of them. We are presenting our observational plans of bright Massive X-ray binaries, WR and LBV stars using a small size telescope. All these stars, which ar

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

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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 (2014): 912–15. http://dx.doi.org/10.1126/science.1252633.

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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 (2014): 44. http://dx.doi.org/10.1088/0004-637x/792/1/44.

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