Type IIb supernovae by the grazing envelope evolution

Naiman, Binyamin V.; Sabach, Efrat; Gilkis, Avishai; Soker, Noam

doi:10.1093/mnras/stz3224

Cited by 13 publications

(29 citation statements)

References 80 publications

(97 reference statements)

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“…The adopted yield is estimated from GW170817 (Cowperthwaite et al 2017;Côté et al 2018b) with assuming a disk ejecta of mass 0.04 M . However, we note that in Naiman et al (2018), the adopted yield is three times higher that what we have adopted in our study.…”

Section: Mp-ricontrasting

confidence: 49%

“…III stars by following the evolution of pristine gas in each simulation cell with a subgrid model of turbulent mixing that is crucial for properly identifying Pop. III stars whose ejecta are the precursor to the formation of CEMP stars (Sarmento et al 2017;Naiman et al 2018); (iii) Adopting a high dark matter particle mass resolution in order to resolve halos where the MP and CEMP stars form in the early universe.…”

Section: Introductionmentioning

confidence: 99%

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On Neutron Star Mergers as the Source of r-process-enhanced Metal-poor Stars in the Milky Way

Safarzadeh

Sarmento

Scannapieco

2019

ApJ

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We model the history of Galactic r -process enrichment using high-redshift, high-resolution zoom cosmological simulations of a Milky Way (MW) type halo. We assume that all r -process sources are neutron star mergers (NSMs) with a power law delay time distribution. We model the time to mix pollutants at subgrid scales, which allows us to to better compute the properties of metal poor (MP) and carbon enhanced metal poor (CEMP) stars, along with statistics of their r -process enhanced subclasses. Our simulations underpredict the cumulative ratios of r -process enhanced MP and CEMP stars (MP-r ,CEMP-r ) over MP and CEMP stars by about one order of magnitude, even when the minimum coalescence time of the double neutron stars (t min ) is set to 1 Myr. No r -process enhanced stars form if t min = 100 Myr. Our results show that even when we adopt the r -process yield estimates observed in GW170817, NSMs by themselves can only explain the observed frequency of r -process enhanced stars if the birth rate of double neutron stars per unit mass of stars is boosted to ≈ 10 −4 M −1 .

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Section: Mp-ricontrasting

confidence: 49%

Section: Introductionmentioning

confidence: 99%

On Neutron Star Mergers as the Source of r-process-enhanced Metal-poor Stars in the Milky Way

Safarzadeh

Sarmento

Scannapieco

2019

ApJ

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“…A likely mechanism for removing the hydrogen envelope, or part of it, is the interaction between a massive star in a binary system and its companion (Podsiadlowski, Joss & Hsu 1992;Yoon, Woosley & Langer 2010;Claeys et al 2011;Yoon, Dessart & Clocchiatti 2017;Lohev et al 2019, Sravan, Marchant & Kalogera 2019, Naiman et al 2020). The minimal hydrogen mass which would give rise to a Type IIb appearance (vs. a Type Ib) is uncertain, with estimates ranging from M H,min,IIb ≈ 0.001 M (Dessart et al 2011) to M H,min,IIb ≈ 0.033 M (Hachinger et al 2012).…”

Section: Introductionmentioning

confidence: 99%

How much hydrogen is in Type Ib and IIb supernova progenitors?

Gilkis,

Arcavi

2021

Preprint

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Core-collapse supernovae showing little or no hydrogen (denoted Type IIb and Ib, respectively) are the explosions of massive stars that lost some or most of their outer envelopes. How they lose their mass is unclear, but it likely involves binary interaction. So far, seven progenitors of such supernovae have been identified in pre-explosion imaging (five for Type IIb events and two for Type Ib events). Here we evolve detailed binary stellar evolution models in order to better understand the nature of these progenitors. We find that the amount of hydrogen left in the envelope at the time of explosion greatly depends on the post-interaction mass-loss rate. The leftover hydrogen, in turn, strongly affects progenitor properties, such as temperature and photospheric radius, in non-trivial ways. Together with extinction and distance uncertainties in progenitor data, it is difficult to deduce an accurate progenitor hydrogen mass from pre-explosion imaging. We quantify this uncertainty and find that available data is consistent with the proposed Type Ib -IIb hydrogen mass threshold of 0.033 M (Hachinger et al. 2012) but not with the proposed threshold of 0.001 M (Dessart et al. 2011), implying that even Type Ib progenitors are not pure helium stars. These results alleviate the proposed tension between the Type Ib classification of SN 2019yvr and its candidate progenitor properties (Kilpatrick et al. 2021). We also estimate the brightness of a surviving 2019yvr progenitor companion, which might be detected in future observations.

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“…The jets remove mass efficiently from the envelope, and by that postpone or prevent the onset of a CEE; instead, the binary system experiences the grazing envelope evolution (GEE; Soker 2015). Naiman et al (2020) study the GEE channel for circular binary orbits with the binary module of the mesa code (Modules for Experiments in Stellar Astrophysics; Paxton et al 2011Paxton et al , 2019 by mimicking the extra mass loss due to jets with a simple numerical prescription. The GEE channel forms mainly bluecompact SN IIb progenitors, because post-GEE winds remove most, but not always all, of the remaining hydrogen.…”

Section: Introductionmentioning

confidence: 99%

Eccentric grazing envelope evolution towards type IIb supernova progenitors

Shishkin,

Soker

2020

Preprint

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We simulate the evolution of eccentric binary systems in the frame of the grazing envelope evolution (GEE) channel for the formation of Type IIb supernovae (SNe IIb), and find that extra mass removal by jets increases the parameter space for the formation of SNe IIb in this channel. To explore the role of eccentricity and the extra mass removal by jets in the GEE we use the stellar evolutionary code MESA binary. The initial primary and secondary masses are M 1,i = 15M and M 2,i = 2.5M , respectively. We examine initial semi-major axes of 600 − 1000R , and eccentricities in the range of e = 0 to e = 0.9. Both Roche lobe overflow (RLOF) and mass removal by jets, followed by a wind from the SN IIb progenitor, leave a hydrogen mass in the exploding star of M H,f ≈ 0.05M . This is compatible with a SN IIb progenitor. We find that in many cases, with and without the extra mass removal by jets, the system can enter a common envelope evolution (CEE) phase, and then gets out from it. Despite the large uncertainties, extra mass removal by jets substantially increases the likelihood of the system to get out from a CEE. This strengthens earlier conclusions for circular orbits. In some cases RLOF alone, without mass removal by jets, can form SN IIb progenitors. We estimate that the extra mass removal by jets in the GEE channel increases the number of progenitors relative to that by RLOF alone by about a factor of two.

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Type IIb supernovae by the grazing envelope evolution

Cited by 13 publications

References 80 publications

On Neutron Star Mergers as the Source of r-process-enhanced Metal-poor Stars in the Milky Way

On Neutron Star Mergers as the Source of r-process-enhanced Metal-poor Stars in the Milky Way

How much hydrogen is in Type Ib and IIb supernova progenitors?

Eccentric grazing envelope evolution towards type IIb supernova progenitors

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