Phenomenological study of massive accretion stars

Hellings, P.

doi:10.1007/bf00661941

Cited by 60 publications

(36 citation statements)

References 18 publications

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“…At the same time, the progenitor star initially should be somewhat more massive, since q0.7, and will naturally form a He core of 3-4 M e , consistent with the ejecta mass of ∼1.15 M e inferred by Silverman et al (2009). Thus, in the scenario of an extended SNIIb discussed here, the small difference in the evolutionary timescales owing to the similarity of the mass, as well as the possible absence of significant mass accretion onto the companion, results in only a limited rejuvenation of the companion (Hellings 1983(Hellings , 1984. This could explain the fact that the detected companion appears to lie close to the TAMS, as seen in Figure 3. A further consequence of possible non-conservative mass transfer is that SNIIb progenitors are expected to have a significant CSM around them just before the explosion, corresponding to mass loss rates on the order of 10 −5 to 10…”

Section: Binary Evolutionary Channel For the Sn 2001ig Progenitorsupporting

confidence: 72%

Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

Ryder

Dyk

Fox

et al. 2018

ApJ

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We present HST/WFC3 ultraviolet imaging in the F275W and F336W bands of the TypeIIb SN2001ig at an age of more than 14years. A clear point source is detected at the site of the explosion, with m F275W =25.39±0.10 and m F336W =25.88±0.13 mag. Despite weak constraints on both the distance to the host galaxy NGC7424 and the line-of-sight reddening to the supernova, this source matches the characteristics of an early B-type mainsequence star with 19,000<T eff <22,000 K and3.92 0.14 bol . A BPASS v2.1 binary evolution model, with primary and secondary masses of 13M e and 9M e, respectively, is found to simultaneously resemble, in the Hertzsprung-Russell diagram, both the observed location of this surviving companion, and the primary star evolutionary endpoints for other TypeIIb supernovae. This same model exhibits highly variable late-stage mass loss, as expected from the behavior of the radio light curves. A Gemini/GMOS optical spectrum at an age of 6 years reveals a narrow He II λ4686 emission line, indicative of continuing interaction with a dense circumstellar medium at large radii from the progenitor. We review our findings on SN2001ig in the context of binary evolution channels for stripped-envelope supernovae. Owing to the uncrowded nature of its environment in the ultraviolet, this study of SN2001ig represents one of the cleanest detections to date of a surviving binary companion to a TypeIIb supernova.

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Section: Binary Evolutionary Channel For the Sn 2001ig Progenitorsupporting

confidence: 72%

Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

Ryder

Dyk

Fox

et al. 2018

ApJ

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“…juvenate (Hellings 1983;de Mink et al 2014;Schneider et al 2016). If the primary is able explode and forms a neutron star, this system most likely evolves into an Be/X-ray binary.…”

Section: Case a Evolutionmentioning

confidence: 99%

Electron Capture Supernovae from Close Binary Systems

Poelarends

Wurtz

Tarka

et al. 2017

ApJ

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We present the first detailed study of the Electron Capture Supernova Channel (ECSN Channel) for a primary star in a close binary star system. Progenitors of ECSN occupy the lower end of the mass spectrum of supernovae progenitors and are thought to form the transition between white dwarfs progenitors and core collapse progenitors . The mass range for ECSN from close binary systems is thought to be wider than the range for single stars, because of the effects of mass transfer on the helium core. Using the MESA stellar evolution code we explored the parameter space of initial primary masses between 8 M and 17 M , using a large grid of models . We find that the initial primary mass and the mass transfer evolution are important factors in the final fate of stars in this mass range. Mass transfer due to Roche Lobe overflow during and after carbon burning causes the core to cool down so that it avoids neon ignition, even in helium-free cores with masses up to 1.52 M , which in single stars would ignite neon. If the core is able to contract to high enough densities for electron captures to commence, we find that, for the adopted Ledoux convection criterion, the initial mass range for the primary to evolve into an ECSN is between 13.5 M and 17.6 M . The mass ratio, initial period, and mass loss efficiency only marginally affect the predicted ranges.

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“…Semiconvective mixing affects the rejuvenation process in an essential way, as it is this process which transports hydrogen into the convective core of the accretion stars. While for infinitely fast semiconvective mixing -which corresponds to the use of the Schwarzschild criterion for convection -all accretion stars rejuvenate (Hellings 1983), this is not the case for finite semi-convective mixing time scales (Braun & Langer 1995). Longer mixing time scales lead to shorter core hydrogen burning life times of the secondaries.…”

Section: The Contact-free Regimementioning

confidence: 99%

Formation of contact in massive close binaries

Wellstein

Langer

Braun

2001

A&A

401

666

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Abstract. We present evolutionary calculations for 74 close binaries systems with initial primary masses in the range 12...25 M , and initial secondary masses between 6 and 24 M . The initial periods were chosen such that mass overflow starts during the core hydrogen burning phase of the primary (Case A), or shortly thereafter (Case B). We use a newly developed binary code with up-to-date physics input. Of particular relevance is the use of OPAL opacities, and the time-dependent treatment of semiconvective and thermohaline mixing. We assume conservative evolution for contact-free systems, i.e., no mass or angular momentum loss from those system except due to stellar winds. We investigate the borderline between contact-free evolution and contact, as a function of the initial system parameters. The fraction of the parameter space where binaries may evolve while avoiding contact -which we found already small for the least massive systems considered -becomes even smaller for larger initial primary masses. At the upper end of the considered mass range, no contact-free Case B systems exist. While for primary masses of 16 M and higher the Case A systems dominate the contact-free range, at primary masses of 12 M contact-free systems are more frequent for Case B. We identify the drop of the exponent x in the main sequence mass-luminosity relation of the form L ∝ M x as the main cause for this behaviour. For systems which evolve into contact, we find that this can occur for distinctively different reasons. While Case A systems are prone to contact due to reverse mass transfer during or after the primary's main sequence phase, all systems obtain contact for initial mass ratios below ∼ 0.65, with a merger as the likely outcome. We also investigate the effect of the treatment of convection, and found it relevant for contact and supernova order in Case A systems, particularly for the highest considered masses. For Case B systems we find contact for initial periods above ∼ 10 d. However, in that case (and for not too large periods) contact occurs only after the mass ratio has been reversed, due to the increased fraction of the donor's convective envelope. As most of the mass transfer occurs conservatively before contact is established, this delayed contact is estimated to yield to the ejection of only a fraction of the donor star's envelope. Our models yield the value of β, i.e., the fraction of the primaries envelope which is accreted by the secondary. We derive the observable properties of our systems after the major mass transfer event, where the mass gainer is a main sequence or supergiant O or early B type star, and the mass loser is a helium star. We point out that the assumption of conservative evolution for contact-free systems could be tested by finding helium star companions to O stars. Those are also predicted by non-conservative models, but with different periods and mass ratios. We describe strategies for increasing the probability to find helium star companions in observational search programs.

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Phenomenological study of massive accretion stars

Cited by 60 publications

References 18 publications

Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

Electron Capture Supernovae from Close Binary Systems

Formation of contact in massive close binaries

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