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

Neuhäuser, R.; Gießler, F.; Hambaryan, V.

doi:10.1093/mnras/stz2629

Cited by 34 publications

(41 citation statements)

References 123 publications

(226 reference statements)

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“…This explanation for the origin of ζ Oph was questioned by Chatterjee et al (2004) with improved astrometric data. Neuhäuser et al (2019) used Gaia DR2 astrometry to kinematically connect ζ Oph and the pulsar PSR B1706-16, suggesting they were ejected from a supernova in a binary system 1.78 ± 0.21 Myr ago. Tetzlaff et al (2010) also identified the isolated neutron star RX J1856-3754 as probably originating from Upper-Sco ∼0.3 Myr ago, with an O-type progenitor.…”

Section: The High-mass Starsmentioning

confidence: 99%

OB Associations and their origins

Wright

2020

New Astronomy Reviews

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OB associations are unbound groups of young stars made prominent by their bright OB members, and have long been thought to be the expanded remnants of dense star clusters. They have been important in astrophysics for over a century thanks to their luminous massive stars, though their low-mass members have not been well studied until the last couple of decades. This has changed thanks to data from X-ray observations, spectroscopic surveys and astrometry from Gaia that allows their full stellar content to be identified and their dynamics to be studied, which in turn is leading to changes in our understanding of these systems and their origins, with the old picture of Blaauw (1964a) now being superseded. It is clear now that OB associations have considerably more substructure than once envisioned, both spatially, kinematically and temporally. These changes have implications for the star formation process, the formation and evolution of planetary systems, and the build-up of stellar populations across galaxies.

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Section: The High-mass Starsmentioning

confidence: 99%

OB Associations and their origins

Wright

2020

New Astronomy Reviews

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“…In addition to checking how the present day position and velocity of HD 95086 compares to the known young associations, we can also trace back the star's position and association distributions to determine how close they were in the past. To study the Galactocentric motion of HD 95086, Carina and LCC we make use of the code described in Neuhäuser et al (2019), which computes the orbits by a numerical integration of their equations of motion as defined by the Galaxy gravitational potential consisting of a three compo- Figure 2. The cumulative distribution function of the distance between HD 95086 and the centre of the young associations Carina (solid line) and LCC (dashed line).…”

Section: Hd 95086mentioning

confidence: 99%

The age of the carina young association and potential membership of HD 95086

Booth

Burgo

Hambaryan

2020

Monthly Notices of the Royal Astronomical Society

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Carina is a nearby young stellar association. So far, only a small number of stars have been clearly identified as members of this association. In this paper we reanalyse the membership of the association in light of Gaia DR2 data, in particular finding that HD 95086 is a potential member (probability of 71%). This star is noteworthy as one of the few stars that hosts both a detected debris disc and a directly imaged planet. It has previously only been considered as a potential member of the Lower Centaurus Crux (LCC) – part of the Scorpius-Centaurus association. We also reanalyse the age of the Carina association. Using a Bayesian inference code applied to infer a solution from stellar evolution models for the most probable (>99%) members of Carina, we infer an age for the association of 13.3$^{+1.1}_{-0.6}$ Myr, much younger than previous studies. Whilst we have revised HD 95086’s association membership from LCC to Carina, the fact that we also find Carina to have a younger age, similar to that of LCC, means that the estimates of HD 95086b’s mass remain unchanged. However, the younger age of Carina does mean that the companion to another Carina member, HD 44627 (AB Pic), has a mass that is more clearly in the planet rather than brown dwarf range.

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“…However, later works (Chatterjee et al 2004; Tetzlaff et al 2010; Zehe et al 2018) show that the association is very unlikely. Recently, Neuhäuser et al (2019) connected ζ Oph to PSR B1706−16. Using Monte Carlo simulations, they traced both objects back to a common origin in Upper‐Centaurus‐Lupus, a subgroup of the Scorpius‐Centaurus‐Lupus OB association, 1.78 ± 0.21 megayears (Myr) ago.…”

Section: Introductionmentioning

confidence: 99%

A search for runaway stars in 12 Galactic supernova remnants

et al. 2021

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Runaway stars can result from core-collapse supernovae in multiple stellar systems. If the supernova disrupts the system, the companion is ejected with its former orbital velocity. A clear identification of a runaway star can yield the time and place of the explosion, as well as orbital parameters of the pre-supernova binary system. Previous searches have mostly considered O-and B-type stars as runaway stars because they are always young in absolute terms (not much older than the lifetime of the progenitor) and can be detected up to larger distances. Here, we present a search for runaway stars of all spectral types. For late-type stars, a young age can be inferred from the lithium test. We used Gaia data to identify and characterize runaway star candidates in nearby supernova remnants, obtained spectra of 39 stars with UVES at the VLT and HDS at the Subaru telescope, and found a significant amount of lithium in the spectra of six dwarf stars. We present the spectral analysis, including measurements of radial velocities, atmospheric parameters, and lithium abundances. Then, we estimate the ages of our targets from the Hertzsprung-Russell diagram and, using the lithium test, present a selection of promising runaway star candidates and draw constraints on the number of ejected runaway stars compared to model expectations.

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

Cited by 34 publications

References 123 publications

OB Associations and their origins

OB Associations and their origins

The age of the carina young association and potential membership of HD 95086

A search for runaway stars in 12 Galactic supernova remnants

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