Spectroscopic orbit determination of the long‐periodic binary system <i>θ</i> Cep

Bischoff, Richard J.; Mugrauer, M.; Lux, Oliver; Zehe, T.; Heyne, T.; Wagner, D.; Geymeier, M.

doi:10.1002/asna.202013850

Cited by 4 publications

(3 citation statements)

References 13 publications

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“…In order to monitor the RV stability of the instrument throughout our monitoring project, the central wavelengths of the lines of the interstellar sodium doublet were measured in all spectra, which are detected in the same spectral order as the D3-line. The RV of the interstellar sodium lines exhibits a standard deviation of 0.5 km/s, consistent with the RV stability of the instrument, reported in other studies (see, e.g., Bischoff et al 2020) before. For the RV of BD+53 2790 we obtain -73.6 km/s on average with a standard deviation of 9.4 km/s (cf.…”

Section: Observational Data and Analysis (Radial Velocity)supporting

confidence: 90%

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Hambaryan,

Stoyanov,

Mugrauer

et al. 2022

Preprint

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Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+53 2790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age∼4-10 Myr) with its brightest star BD+53 2820 (B0V; L∼10 4.7 L ). The kinematic age of 4U 2206+54 is about 2.8 ± 0.4 Myr, it is at a distance of 3.1-3.3 kpc and has a space velocity of 75-100 km/s with respect to this member star (BD+53 2820 ) of the Cep OB1 association. This runaway velocity indicates that the progenitor of the neutron star hosted by 4U 2206+54 lost about 4-9 M during the supernova explosion and the latter one received a kick velocity of at least 200-350 km/s . Since the high-mass X-ray binary 4U 2206+54/BD+53 2790 was born as a member of a subgroup of Cep OB1, the initially most massive star in the system terminated its evolution within < ∼ 7 − 9 Myr, corresponding to an initial mass > ∼ 32 M .

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Section: Observational Data and Analysis (Radial Velocity)supporting

confidence: 90%

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Hambaryan,

Stoyanov,

Mugrauer

et al. 2022

Preprint

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“…Each calibration file has an individual integration time of 5 s. About 700 detected emission lines are available in the ThAr spectra for wavelength calibration. The long-term stability of the wavelength calibration of FLECHAS was confirmed in studies by Irrgang et al (2016), Bischoff et al (2017), Heyne et al (2020) and Bischoff et al (2020a). Additionally, for the dark subtraction, three dark frames for all used integration times were taken in every observing night.…”

Section: Sample Selection Observations and Data Reductionmentioning

confidence: 65%

Identification of additional young nearby runaway stars based on Gaia data release 2 observations and the lithium test

Bischoff¹,

Mugrauer²,

Torres

et al. 2021

Astron Nachr

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Runaway stars are characterized by their remarkably high space velocities, and the study of their formation mechanisms has attracted considerable interest.Young, nearby runaway stars are the most favorable for identifying their place of origin, and for searching for possible associated objects such as neutron stars.Usually, the research field of runaway stars focuses on O-and B-type stars, because these objects are better detectable at larger distances than late-type stars. Early-type runaway stars have the advantage that they evolve faster and can therefore better be confirmed to be young. In contrast to this, the catalog of Young runaway stars within 3 kpc by Tetzlaff, N., Neuhäuser, R., & Hohle, M. M. (2011, MNRAS, 410(1), 190-200) contains also stars of spectral type A and later.The objects in this catalog were originally classified as young (≤ 50 Myr) runaway stars by using Hipparcos data to estimate the ages from their location in the Hertzsprung-Russell diagram and evolutionary models. In this article, we redetermine and/or constrain their ages not only by using the more precise second data release of the Gaia mission, but also by measuring the equivalent width of the lithium (6,708 Å) line, which is a youth indicator. Therefore, we searched for lithium absorption in the spectra of 51 target stars, taken at the University Observatory Jena between March and September 2020 with the Échelle spectrograph FLECHAS, and within additional TRES-spectra from the Fred L. Whipple Observatory. The main part of this campaign with its 308 reduced spectra, accessible at VizieR, was already published. In this work, which is the continuation and completion of the in 2015 initiated observing campaign, we found three additional young runaway star candidates.

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“…Each calibration file has an individual integration time of 5 s. About 700 detected emission lines are available in the ThAr spectra for wavelength calibration. The long-term stability of the wavelength calibration of FLECHAS was confirmed in studies by Irrgang, Desphande, Moehler, Mugrauer, & Janousch (2016), Bischoff et al (2017), Heyne et al (2020) and Bischoff, Mugrauer, Lux, et al (2020). Additionally, for the dark subtraction, three dark frames for all used integration times were taken in every observing night.…”

Section: Sample Selection Observations and Data Reductionmentioning

confidence: 77%

Identification of additional young nearby runaway stars based on Gaia data release 2 observations and the lithium test

Bischoff,

Mugrauer,

Torres

et al. 2021

Preprint

View full text Add to dashboard Cite

Runaway stars are characterised by their remarkably high space velocities, and the study of their formation mechanisms has attracted considerable interest. Young, nearby runaway stars are the most favorable for identifying their place of origin, and for searching for possible associated objects such as neutron stars.Usually the research field of runaway stars focuses on O-and B-type stars, because these objects are better detectable at larger distances than late-type stars. Early-type runaway stars have the advantage, that they evolve faster and can therefore better be confirmed to be young. In contrast to this, the catalogue of Young runaway stars within 3 kpc by Tetzlaff, Neuhäuser, & Hohle (2011) contains also stars of spectral type A and later. The objects in this catalogue were originally classified as young (≤ 50 Myr) runaway stars by using Hipparcos data to estimate the ages from their location in the Hertzsprung-Russell diagram and evolutionary models.In this article, we redetermine and/or constrain their ages not only by using the more precise second data release of the Gaia mission, but also by measuring the equivalent width of the lithium (6708 Å) line, which is a youth indicator. Therefore, we searched for lithium absorption in the spectra of 51 target stars, taken at the University Observatory Jena between March and September 2020 with the Échelle spectrograph FLECHAS, and within additional TRES-spectra from the Fred L. Whipple Observatory. The main part of this campaign with its 308 reduced spectra, accessible at VizieR, was already published. In this work, which is the continuation and completion of the in 2015 initiated observing campaign, we found three additional young runaway star candidates.

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Spectroscopic orbit determination of the long‐periodic binary system θ Cep

Cited by 4 publications

References 13 publications

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Identification of additional young nearby runaway stars based on Gaia data release 2 observations and the lithium test

Identification of additional young nearby runaway stars based on Gaia data release 2 observations and the lithium test

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