The evolution of massive stars losing mass angular momentum - Origin of Wolf-Rayet stars

Sreenivasan, Sameet; Wilson, William Jerome

doi:10.1086/159732

Cited by 17 publications

(6 citation statements)

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“…Assuming it is the most evolved member of the cluster, the lower mass limit of its progenitor should be, at least, the mass of the brightest cluster stars yet on the cluster MS. A simple calculation (see the next section) yields that the mass of the brightest star yet on the MS is ∼20 M ⊙ . Although this value is similar to that obtained by Massey et al (2001), it does not contradict the previous estimate made by Turner et al (1983), who found ∼30 M ⊙ using the Sreenivasan & Wilson (1982) models of binary star evolution, as the value obtained in this paper should be assumed just as a lower mass limit.…”

Section: Discussionsupporting

confidence: 85%

The young open cluster Markarian 50

Baume

Vazquez

Carraro

2004

Monthly Notices of the Royal Astronomical Society

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We report on a deep CCD UBV(RI) C photometric survey in the region of the young open cluster Markarian 50. The new photometric data allow us to extend the cluster membership down to V ≈ 17.5, about 2 mag deeper than any previous investigation. On the basis of these data we derive a distance d = 3460 ± 350 pc (V O − M V = 12.7 ± 0.2), which turns out to be only slightly lower than previous estimates. The cluster presents differential reddening, with E(B-V ) values ranging from 0.69 to 1.1. The brightest member (HD 219460) is a double star, which we separate photometrically for the first time, providing individual magnitudes and colours for each component. One of them is a Wolf-Rayet (WR) star and, according to evolutionary models, the mass of its progenitor should be greater than ∼20 M . The age obtained for the cluster is 7.5 ± 2 Myr and the mass function for the most massive stars (M > 1 M ) presents a slope x ≈ 1.0.

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Section: Discussionsupporting

confidence: 85%

The young open cluster Markarian 50

Baume

Vazquez

Carraro

2004

Monthly Notices of the Royal Astronomical Society

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“…Under this assumption, they find that they can naturally explain the observed rotational distribution of stars in these samples. Rapid rotation increases chemical mixing within the interior of the star, which increases the fuel available to that star and naturally extend its lifetime (Sreenivasan & Wilson 1982;Pols et al 1998;Maeder & Meynet 2000) to We should also note that the SMC is known to be highly efficient in forming high-mass X-ray binaries (HMXBs) that consist of a neutron star orbiting a rapidly rotating B-type main-sequence star (e.g., Shtykovskiy & Gilfanov 2005;Haberl & Sturm 2016). This characteristic is consistent with evidence that binary interaction (and to some extent, low metallicity) favours the formation of rapidly-rotating stars (e.g., Dray 2006;Antoniou et al 2010;Douna et al 2015;Haberl & Sturm 2016).…”

Section: The Effects Of Mass Loss Rapid Rotation and Binarymentioning

confidence: 99%

Section: The Effects Of Mass Loss Rapid Rotation and Binarymentioning

confidence: 99%

Measurement of the Core-collapse Progenitor Mass Distribution of the Small Magellanic Cloud

Auchettl

Lopez

Badenes

et al. 2019

ApJ

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The physics of core-collapse (CC) supernovae (SNe) and how the explosions depend on progenitor properties are central questions in astronomy. For only a handful of SNe, the progenitor star has been identified in preexplosion images. Supernova remnants (SNRs), which are observed long after the original SN event, provide a unique opportunity to increase the number of progenitor measurements. Here, we systematically examine the stellar populations in the vicinities of 23 known SNRs in the Small Magellanic Cloud (SMC) using the star formation history (SFH) maps of Harris & Zaritsky (2004). We combine the results with constraints on the SNR metal abundances and environment from X-ray and optical observations. We find that 22 SNRs in the SMC have local SFHs and properties consistent with a CC explosion, several of which are likely to have been high-mass progenitors. This result supports recent theoretical findings that high-mass progenitors can produce successful explosions. We estimate the mass distribution of the CC progenitors and find that this distribution is similar to a Salpeter IMF (within the uncertainties), while this result is shallower than the mass distribution found in M31 and M33 by Jennings et al. (2014) and Díaz-Rodríguez et al. (2018) using a similar approach. Additionally, we find that a number of the SMC SNRs exhibit a burst of star formation between 50-200 Myr ago. As these sources are likely CC, this signature may be indicative of massive stars undergoing delayed CC as a consequence of binary interaction, rapid rotation, or low metallicity. In addition, the lack of Type Ia SNRs in the SMC is possibly a result of the short visibility times of these sources as they may fall below the sensitivity limits of current radio observations.

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“…The effects of mass loss in the HR diagram have been discussed intensely by several authors (cf. Chiosi et al, 1979;de Loore et al, 1978;Stothers, 1979;Maeder, 1980Maeder, , 1981Maeder, ab, 1983de Loore, de Greve, 1981;Chiosi, 1981;Mitalas, 1981, 1983;Sreenivasan and Wilson, 1982;Brunish and Truran, 1982 ab). The details of the effects of mass loss on the MS evolution have been discussed by most of the above authors and we only briefly mention these effects here: decrease of luminosity but the star is overluminous for its actual mass; decrease of the core mass, but the core mass fraction is larger; increase of the MS lifetime; MS widening for low and intermediate mass loss rates, MS narrowing for very large rates; decline of semi-convection; possible change of surface abundances.…”

Section: Results From Evolutionary Models With Mass Loss A) Results Imentioning

confidence: 99%

Evolution of massive stars, supergiants and Wolf-Rayet stars

Maeder

1984

Symp. - Int. Astron. Union

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Massive stars (say M ≳ 9 M⊙) play a major role in Astrophysics. They are the main agents of nucleosynthesis and galactic enrichment and present many interesting properties, like high stellar winds, chemical surface enhancements, instabilities etc. which deserve further investigation. Furthermore, massive stars also are the powering sources of giant H II regions and have important radiative, mechanical and chemical interactions with the interstellar medium.

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The evolution of massive stars losing mass angular momentum - Origin of Wolf-Rayet stars

Cited by 17 publications

References 0 publications

The young open cluster Markarian 50

The young open cluster Markarian 50

Measurement of the Core-collapse Progenitor Mass Distribution of the Small Magellanic Cloud

Evolution of massive stars, supergiants and Wolf-Rayet stars

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