Rotation of surviving companion stars after type Ia supernova explosions in the WD+MS scenario

Liu, Zheng-Wei; Pakmor, Rüdiger; Röpke, F. K.; Edelmann, P. V. F.; Hillebrandt, W.; Kerzendorf, Wolfgang; Wang, Bo; Han, Zhanwen

doi:10.1051/0004-6361/201220903

Cited by 44 publications

(70 citation statements)

References 56 publications

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“…These expectations, that follow from simple angular-momentum conservation considerations, have been confirmed by numerical simulations (e.g. Pan et al 2012a;Liu et al 2013), though we note that none of the simulations in Pan et al (2012a) can explain the observed properties of Tycho G as none can fit the observed gravity (log g) and the observed rotational velocity simultaneously. Fig.…”

Section: Companion Radius and Rotational Velocitysupporting

confidence: 64%

A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

Meng

Podsiadlowski

2017

Monthly Notices of the Royal Astronomical Society

120

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The single-degenerate (SD) model is one of the principal models for the progenitors of type Ia supernovae (SNe Ia), but some of the predictions in the most widely studied version of the SD model, i.e. the optically thick wind (OTW) model, have not been confirmed by observations. Here, we propose a new version of the SD model in which a common envelope (CE) is assumed to form when the mass-transfer rate between a carbon-oxygen white dwarf (CO WD) and its companion exceeds a critical accretion rate. The WD may gradually increase its mass at the base of the CE. Due to the large nuclear luminosity for stable hydrogen burning, the CE may expand to giant dimensions and will lose mass from the surface of the CE by a CE wind (CEW). Because of the low CE density, the binary system will avoid a fast spiral-in phase and finally re-emerge from the CE phase. Our model may share the virtues of the OTW model but avoid some of its shortcomings. We performed binary stellar evolution calculations for more than 1100 close WD + MS binaries. Compared with the OTW model, the parameter space for SNe Ia from our CEW model extends to more massive companions and less massive WDs. Correspondingly, the Galactic birth rate from the CEW model is higher than that from the OTW model by ∼30%. Finally, we discuss the uncertainties of the CEW model and the differences between our CEW model and the OTW model.

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Section: Companion Radius and Rotational Velocitysupporting

confidence: 64%

A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

Meng

Podsiadlowski

2017

Monthly Notices of the Royal Astronomical Society

120

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“…We expect that some small morphological differences, such as the post-impact density distribution of all removed companion material and SN ejecta, would be seen if the orbital motion of the companion star is included, but it should not affect the basic results presented in this work (see also Liu et al 2013b). …”

Section: Impact Velocity Of the Companion Starmentioning

confidence: 90%

The interaction of core-collapse supernova ejecta with a companion star

Liu

Tauris

Röpke

et al. 2015

A&A

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Context. The progenitors of many core-collapse supernovae (CCSNe) are expected to be in binary systems. After the SN explosion in a binary, the companion star may suffer from mass stripping and be shock heated as a result of the impact of the SN ejecta. If the binary system is disrupted by the SN explosion, the companion star is ejected as a runaway star, and in some cases as a hypervelocity star. Aims. By performing a series of three-dimensional (3D) hydrodynamical simulations of the collision of SN ejecta with the companion star, we investigate how CCSN explosions affect their binary companion. Methods. We use the BEC stellar evolution code to construct the detailed companion structure at the moment of SN explosion. The impact of the SN blast wave on the companion star is followed by means of 3D smoothed particle hydrodynamics (SPH) simulations using the Stellar GADGET code. Results. For main-sequence (MS) companion stars, we find that the amount of removed stellar mass, the resulting impact velocity, and the chemical contamination of the companion that results from the impact of the SN ejecta strongly increases with decreasing binary separation and increasing explosion energy. Their relationship can be approximately fitted by power laws, which is consistent with the results obtained from impact simulations of Type Ia SNe. However, we find that the impact velocity is sensitive to the momentum profile of the outer SN ejecta and, in fact, may decrease with increasing ejecta mass, depending on the modeling of the ejecta. Because most companion stars to Type Ib/c CCSNe are in their MS phase at the moment of the explosion, combined with the strongly decaying impact effects with increasing binary separation, we argue that the majority of these SNe lead to inefficient mass stripping and shock heating of the companion star following the impact of the ejecta. Conclusions. Our simulations show that the impact effects of Type Ib/c SN ejecta on the structure of MS companion stars, and thus their long-term post-explosion evolution, is in general not dramatic. We find that at most 10% of their mass is lost and their resulting impact velocities are less than 100 km s −1 .

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“…Thus, stars in a cluster or a binary system can be kicked out by a perturbation of the system, for instance, such as in a threebody encounter or a supernova explosion (e.g., Hoogerwerf et al 2000;Perets 2009;Irrgang et al 2010;Zhang et al 2013). To be more specific, there are several possible formation scenarios for HVSs: (1) interaction of single stars with a central massive black hole (MBH); (2) tidal break-up of binary stars in the vicinity of a MBH; (3) three-body interactions involving single-star encounters with a binary or cluster of MBHs; (4) double detonation of SN Ia with a close system of a rapidly orbiting low-mass compact He star and a massive (∼1−1.2 M ) CO-white dwarf (Geier et al 2015); (5) single-degenerate SN type Ia consisting of a white dwarf and a main-sequence star (Liu et al 2013); (6) binary star disruption in dense interacting regions such as globular clusters or the Galactic bulge or disk; or (7) tidal disruption of dwarf galaxies in the Galaxy (Li et al 2015, and references therein). The last case would lead to old rapidly traveling stars.…”

Section: High-velocity Starsmentioning

confidence: 99%

Chemical abundances in a high-velocity RR Lyrae star near the bulge

Hansen¹,

Rich

Koch

et al. 2016

A&A

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Low-mass variable high-velocity stars are interesting study cases for many aspects of Galactic structure and evolution. Until recently, the only known high-or hyper-velocity stars were young stars thought to originate from the Galactic center. Wide-area surveys such as APOGEE and BRAVA have found several low-mass stars in the bulge with Galactic rest-frame velocities higher than 350 km s −1 . In this study we present the first abundance analysis of a low-mass RR Lyrae star that is located close to the Galactic bulge, with a space motion of ∼-400 km s −1 . Using medium-resolution spectra, we derived abundances (including upper limits) of 11 elements. These allowed us to chemically tag the star and discuss its origin, although our derived abundances and metallicity, at [Fe/H] = −0.9 dex, do not point toward one unambiguous answer. Based on the chemical tagging, we cannot exclude that it originated in the bulge. However, its retrograde orbit and the derived abundances combined suggest that the star was accelerated from the outskirts of the inner (or even outer) halo during many-body interactions. Other possible origins include the bulge itself, or the star might have been stripped from a stellar cluster or the Sagittarius dwarf galaxy when it merged with the Milky Way.

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Rotation of surviving companion stars after type Ia supernova explosions in the WD+MS scenario

Cited by 44 publications

References 56 publications

A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

The interaction of core-collapse supernova ejecta with a companion star

Chemical abundances in a high-velocity RR Lyrae star near the bulge

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