New radial velocities for 30 candidate runaway stars and a possible binary supernova origin for HIP 9470 and PSR J0152–1637

Tetzlaff, N.; Torres, Guillermo; Bieryla, Allyson; Neuhäuser, R.

doi:10.1002/asna.201412125

Cited by 5 publications

(5 citation statements)

References 40 publications

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“…We use the α and β values identified above, and create synthetic runaway star velocity and NS-NS binary system period probability distributions. These too we find to agree well with the observational data of Tetzlaff et al (2014) and Andrews et al (2015) respectively.…”

supporting

confidence: 91%

Is the Link Between the Observed Velocities of Neutron Stars and their Progenitors a Simple Mass Relationship?

Bray

2016

Proc. IAU

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While the imparting of velocity ‘kicks’ to compact remnants from supernovae is widely accepted, the relationship of the ‘kick’ to the progenitor is not. We propose the ‘kick’ is predominantly a result of conservation of momentum between the ejected and compact remnant masses. We propose the ‘kick’ velocity is given by vkick = α(Mejecta/Mremnant)+β, where α and β are constants we wish to determine. To test this we use the BPASS v2 (Binary Population and Spectral Synthesis) code to create stellar populations from both single star and binary star evolutionary pathways. We then use our Remnant Ejecta and Progenitor Explosion Relationship (REAPER) code to apply ‘kicks’ to neutron stars from supernovae in these models using a grid of α and β values, (from 0 to 200 km s−1 in steps of 10 km s−1), in three different ‘kick’ orientations, (isotropic, spin-axis aligned and orthogonal to spin-axis) and weighted by three different Salpeter initial mass functions (IMF’s), with slopes of -2.0, -2.35 and -2.70. We compare our synthetic 2D and 3D velocity probability distributions to the distributions provided by Hobbs et al. (1995).

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supporting

confidence: 91%

Is the Link Between the Observed Velocities of Neutron Stars and their Progenitors a Simple Mass Relationship?

Bray

2016

Proc. IAU

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“…Pizzolato et al (2008) propose that the X-ray source 1E 161348-5055 is a neutron star in close orbit with a low-mass MS star. Tetzlaff et al (2014b) discuss a possible common origin for PSR J0152-1637 and the runaway star HIP 9470. However, the runaway star itself is a single-lined spectroscopic binary.…”

Section: Systematic Searches For Companionsmentioning

confidence: 96%

“…Moreover, a core-collapse SN may disrupt a binary system, ejecting its companion (Blaauw 1961;Hoogerwerf et al 2001). Some runaway stars (stars with velocities of around tens of km s −1 compared to their surrounding populations) can be tentatively linked with SN remnants and pulsars (Dufton et al 2011;Tetzlaff et al 2013Tetzlaff et al , 2014bDinçel et al 2015;Boubert et al 2017), suggesting that they were the companions of the SN progenitor at the moment of explosion.…”

Section: Searching For Surviving Binary Companionsmentioning

confidence: 99%

Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap

Zapartas

Mink

Dyk

et al. 2017

ApJ

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Many young, massive stars are found in close binaries. Using population synthesis simulations we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers or disrupted systems). All the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of a main-sequence companion star > 8-10 M , ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially 23 M . Although unlikely (<1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broad-lined Type Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that governs the evolution of SN progenitors.

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“…This solution was doubted when better astrometric data became available (Chatterjee et al 2004, Tetzlaff et al 2010, Kirsten et al 2015. Other cases, where a neutron star was traced back to an OB association, with or without a runaway star, were presented by Tetzlaff et al (2009Tetzlaff et al ( , 2010Tetzlaff et al ( , 2011bTetzlaff et al ( , 2012Tetzlaff et al ( , 2013Tetzlaff et al ( , 2014aTetzlaff et al ( , 2014b.…”

Section: Introduction: 60 Fe On Earthmentioning

confidence: 99%

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Neuhäuser

Gießler

Hambaryan

2019

Monthly Notices of the Royal Astronomical Society

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The detection of ∼ 1.5−3.2 Myr old 60 Fe on Earth indicates recent nearby core-collapse supernovae. For supernovae in multiple stars, the primary stars may become neutron stars, while former companions may become unbound and become runaway stars. We wrote software for tracing back the space motion of runaway and neutron stars to young associations of massive stars. We apply it here to the nearby young Scorpius-Centaurus-Lupus groups, all known runaway stars possibly coming from there, and all 400 neutron stars with known transverse velocity. We find kinematic evidence that the runaway ζ Oph and the radio pulsar PSR B1706-16 were released by a supernova in a binary 1.78 ± 0.21 Myr ago at 107 ± 4 pc distance (for pulsar radial velocity 260 ± 43 km/s); association age and flight time determine the progenitor mass (16-18 M ), which can constrain supernova nucleosynthesis yields and 60 Fe uptake on Earth. In addition, we notice that the only high-mass X-ray binary in Scorpius-Centaurus-Lupus (1H11255-567 with µ 1 and µ 2 Cru) may include a neutron star formed in another SN, up to ∼ 1.8 Myr ago at 89 − 112 pc, i.e. also yielding 60 Fe detectable on Earth. Our scenario links 60 Fe found on Earth to one or two individual supernovae in multiple stars.

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New radial velocities for 30 candidate runaway stars and a possible binary supernova origin for HIP 9470 and PSR J0152–1637

Cited by 5 publications

References 40 publications

Is the Link Between the Observed Velocities of Neutron Stars and their Progenitors a Simple Mass Relationship?

Is the Link Between the Observed Velocities of Neutron Stars and their Progenitors a Simple Mass Relationship?

Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

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