The mass-loss rates of red supergiants and the de Jager prescription

Mauron, N.; Josselin, E.

doi:10.1051/0004-6361/201013993

Cited by 224 publications

(261 citation statements)

References 65 publications

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“…The presence of a luminous yellow supergiant in one of these clusters is also consistent with the idea that this star evolved away from the RSG stage (Davies et al 2008). Mauron & Josselin (2011), on the other hand, still recommend using the de Jager et al (1988) rate for Galactic RSGs, indicating that this prescription agrees to within a factor of 4 with most mass-loss rate estimates based on the infrared 60 μm excess. This result is however compatible with the existence of short phases during which the mass-loss rates are much stronger.…”

Section: Discussion Of Various Possible Origins For the Low-luminositsupporting

confidence: 78%

Grids of stellar models with rotation

Georgy

Ekström

Meynet

et al. 2012

A&A

305

364

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Context. In recent years, many very interesting observations have appeared concerning the positions of Wolf-Rayet (WR) stars in the Hertzsprung-Russell diagram (HRD), the number ratios of WR stars, the nature of Type Ibc supernova (SN) progenitors, long and soft gamma ray bursts (LGRB), and the frequency of these various types of explosive events. These observations represent key constraints on massive star evolution. Aims. We study, in the framework of the single-star evolutionary scenario, how rotation modifies the evolution of a given initial mass star towards the WR phase and how it impacts the rates of Type Ibc SNe. We also discuss the initial conditions required to obtain collapsars and LGRB. Methods. We used a recent grid of stellar models computed with and without rotation to make predictions concerning the WR populations and the frequency of different types of core-collapse SNe. Current rotating models were checked to provide good fits to the following features: solar luminosity and radius at the solar age, main-sequence width, red-giant and red-supergiant (RSG) positions in the HRD, surface abundances, and rotational velocities. Results. Rotating stellar models predict that about half of the observed WR stars and at least half of the Type Ibc SNe may be produced through the single-star evolution channel. Rotation increases the duration of the WNL and WNC phases, while reducing those of the WNE and WC phases, as was already shown in previous works. Rotation increases the frequency of Type Ic SNe. The upper mass limit for Type II-P SNe is ∼19.0 M for the non rotating models and ∼16.8 M for the rotating ones. Both values agree with observations. Moreover, present rotating models provide a very good fit to the progenitor of SN 2008ax. We discuss future directions of research for further improving the agreement between the models and the observations. We conclude that the mass-loss rates in the WNL and RSG phases are probably underestimated at present. We show that up to an initial mass of 40 M , a surface magnetic field inferior to about 200 G may be sufficient to produce some braking. Much lower values are needed at the red supergiant stage. We suggest that the presence/absence of any magnetic braking effect may play a key role in questions regarding rotation rates of young pulsars and the evolution leading to LGRBs.

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Section: Discussion Of Various Possible Origins For the Low-luminositsupporting

confidence: 78%

Grids of stellar models with rotation

Georgy

Ekström

Meynet

et al. 2012

A&A

305

364

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“…This is in agreement with typical mass-loss rates of RSGs of this luminosity, significantly smaller than in super-AGB stars (Poelarends et al 2008;Mauron & Josselin 2011) and greater than in BSGs (Martins et al 2015). However, asymmetry and inhomogeneity (e.g., clumpiness) in the CSM can greatly affect our estimated optical depth.…”

Section: The Progenitor Of Sn 2010dasupporting

confidence: 88%

The Intermediate Luminosity Optical Transient Sn 2010da: The Progenitor, Eruption, and Aftermath of a Peculiar Supergiant High-Mass X-Ray Binary

Villar

Berger

Chornock

et al. 2016

ApJ

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We present optical spectroscopy, ultraviolet-to-infrared imaging,and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from −6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M e yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M bol −10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca II emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L X ≈ 6 × 10 39 erg s −1). We additionally attribute He II 4686 Å and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈10 37 erg s −1 to the presence of a compact companion.

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“…, van Loon et al 2005;Mauron & Josselin 2011) and exceeds the limit for mass loss due to the commonly assumed line-driven winds even in the case of a small filling factor f = 0.1 of the H-rich shell (e.g., Smith 2014, their Figure3). This scenario is explored in M15.…”

Section: The Origin Of the H-rich Shell In Sn 2014cmentioning

confidence: 88%

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Margutti

Kamble

Milisavljevic

et al. 2017

ApJ

171

269

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We present multi-wavelength observations of SN 2014C during the first 500 days. These observations represent the first solid detection of a young extragalactic stripped-envelope SN out to high-energy X-rays ∼40 keV. SN 2014C shows ordinary explosion parameters (E k ∼1.8×10 51 erg and M ej ∼1.7 M e ). However, over an ∼1 year timescale, SN 2014C evolved from an ordinary hydrogen-poor supernova into a strongly interacting, hydrogen-rich supernova, violating the traditional classification scheme of type-I versus type-II SNe. Signatures of the SN shock interaction with a dense medium are observed across the spectrum, from radio to hard X-rays, and revealed the presence of a massive shell of ∼1 M e of hydrogen-rich material at ∼6×10 16 cm. The shell was ejected by the progenitor star in the decades to centuries before collapse. This result challenges current theories of massive star evolution, as it requires a physical mechanism responsible for the ejection of the deepest hydrogen layer of H-poor SN progenitors synchronized with the onset of stellar collapse. Theoretical investigations point at binary interactions and/or instabilities during the last nuclear burning stages as potential triggers of the highly time-dependent mass loss. We constrain these scenarios utilizing the sample of 183 SNe Ib/c with public radio observations. Our analysis identifies SN 2014C-like signatures in ∼10% of SNe. This fraction is reasonably consistent with the expectation from the theory of recent envelope ejection due to binary evolution if the ejected material can survive in the close environment for 10 3 -10 4 years. Alternatively, nuclear burning instabilities extending to core C-burning might play a critical role.

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The mass-loss rates of red supergiants and the de Jager prescription

Cited by 224 publications

References 65 publications

Grids of stellar models with rotation

Grids of stellar models with rotation

The Intermediate Luminosity Optical Transient Sn 2010da: The Progenitor, Eruption, and Aftermath of a Peculiar Supergiant High-Mass X-Ray Binary

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

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