The radial and rotational velocity of <i>ζ</i> Ophiuchi

Zehe, T.; Mugrauer, M.; Neuhäuser, R.; Pannicke, A.; Lux, Oliver; Bischoff, Richard J.; Wöckel, D.; Wagner, D.

doi:10.1002/asna.201713383

Cited by 11 publications

(28 citation statements)

References 33 publications

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“…The data presented here, together with those of ζ Oph (Zehe et al 2018), are the first spectroscopic monitoring observations of runaway stars carried out at the University Observatory Jena so far. The RV measurements of AE Aur and ι Ori will also be made available online at VizieR (Ochsenbein et al 2000).…”

Section: Discussionmentioning

confidence: 84%

“…Furthermore, the star ζ Oph was also suggested to be a runaway star by Hoogerwerf et al (2001) but is considered to be ejected by a supernova in a binary, also based on Hipparcos astrometry and ground‐based RV. However, Zehe et al (2018) monitored the RV of ζ Oph and found that it is different from what was used in Hoogerwerf et al (2001), so ζ Oph and the pulsar, as suggested by Hoogerwerf et al (2001), could not have been ejected in the same supernova. Recently, Neuhäuser et al (2019) showed that ζ Oph originated from a supernova in a binary with the progenitor of PSR B1706‐16, a supernova, 1.78 ± 0.21 Myr ago at 107 ± 4 pc distance.…”

Section: Introductionmentioning

confidence: 95%

“…Therefore, in addition to the spectroscopic and visual multiple star systems, observed in the course of the Großschwabhausen Binary Survey (Bischoff et al 2017; Heyne et al 2020; Mugrauer et al 2017), beside ζ Oph (Zehe et al 2018), we have also monitored the runaway stars AE Aur and ι Ori to obtain current and accurate RV data of these targets. The survey is carried out at the University Observatory Jena (Pfau 1984) with the fiber‐linked Échelle spectrograph FLECHAS (Mugrauer et al 2014), which has been operated since 2013 at the Nasmyth focus ( D = 90 cm, f / D = 15) of the 90‐cm reflector telescope of the observatory.…”

Section: Introductionmentioning

confidence: 99%

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Radial velocity measurements of the runaway stars AE Aur and ι Ori

Heyne¹,

Mugrauer²,

Bischoff³

et al. 2020

Astron Nachr

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We present the results of our spectroscopic monitoring observations of the late O‐type runaway stars AE Aur and ι Ori, carried out between September 2016 and May 2018 using the Échelle spectrograph FLECHAS at the University Observatory Jena. For both stars, we obtained current radial velocity (RV) measurements with better precision than before. These results can be used for further advanced calculations of their space motion, needed to determine, for example, their place of origin in our Galaxy. In this paper, we describe the observations and the data reduction, as well as the analysis of all spectral data. We find a stable RV for AE Aur and confirm ι Ori as a double‐lined spectroscopic binary and derive its current Keplerian orbital elements.

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Section: Discussionmentioning

confidence: 84%

Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

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Radial velocity measurements of the runaway stars AE Aur and ι Ori

Heyne¹,

Mugrauer²,

Bischoff³

et al. 2020

Astron Nachr

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“…The O9.5 stars Oph and PSR B1929+10 were the first pair of a runaway star and a neutron star suggested to have been together as a massive binary (Hoogerwerf et al 2000(Hoogerwerf et al , 2001. 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 Oph to PSR B1706−16.…”

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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“…Next the noise of the continuum was estimated by determining the standard deviation of the observed flux outside the fitted line. The Full Width at Zero Intensity was then determined by measuring the high and low wavelengths at which V (λ) became indistinguishable from the noise.Adopting the same methodology asZehe et al (2018), the line widths LW were determined from the wavelengths at which the fitted line profiles reached the noise level where the continuum flux had a value of 1. The derived line widths LW with Voigt and Gaussian fits were nearly identical.…”

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confidence: 99%

The spin rates of O stars in WR+O Magellanic Cloud binaries

Shara

Crawford

Vanbeveren

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Some massive, merging black holes (BH) may be descendants of binary O stars. The evolution and mass transfer between these O stars determines the spins of their progeny BH. These will be measurable with future gravitational wave detectors, incentivizing the measurement of the spins of O stars in binaries. We previously measured the spins of O stars in Galactic Wolf-Rayet (WR) + O binaries. Here we measure the v e sini of four LMC and two SMC O stars in WR + O binaries to determine whether lower metallicity might affect the spin rates. We find that the O stars in Galactic and Magellanic WR + O binaries display average v e sini = 258 ± 18 km/s and 270 ± 15 km/s, respectively. Two LMC O stars measured on successive nights show significant line width variability, possibly due to differing orbital phases exhibiting different parts of the O stars illuminated differently by their WR companions. Despite this variability, the v e sini are highly super-synchronous but distinctly subcritical for the O stars in all these binaries; thus we conclude that an efficient mechanism for shedding angular momentum from O stars in WR + O binaries must exist. This mechanism, probably related to Roche lobe overflow-created dynamo magnetic fields, prevents nearly 100% breakup spin rates, as expected when RLOF operates, as it must, in these stars. A Spruit-Tayler dynamo and O star wind might be that mechanism.

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The radial and rotational velocity of ζ Ophiuchi

Cited by 11 publications

References 33 publications

Radial velocity measurements of the runaway stars AE Aur and ι Ori

Radial velocity measurements of the runaway stars AE Aur and ι Ori

A search for runaway stars in 12 Galactic supernova remnants

The spin rates of O stars in WR+O Magellanic Cloud binaries

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