Radial velocity measurements and orbit determination of eight single‐lined spectroscopic binary systems

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

doi:10.1002/asna.201713365

Cited by 23 publications

(37 citation statements)

References 14 publications

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“…The RVs of the measured telluric lines scatter on average on the 0.9 km s −1 level, which is consistent with the reached RV precision of the different observed targets. The long‐term RV stability of the spectrograph was already verified by Irrgang et al and Bischoff et al , and is also confirmed by our measurements, taken in the course of this project.…”

Section: Rv Measurementssupporting

confidence: 89%

“…Since 2013, the fiber‐linked Échelle spectrograph FLECHAS (Mugrauer et al ) is mounted on the 90‐cm reflector telescope while it is operated in the Nasmyth mode ( D = 90 cm, f / D = 15). As part of the Großschwabhausen binary survey (Mugrauer et al ), a radial velocity (RV) monitoring program was started in 2015 (Bischoff et al ) in order to redetermine, verify, improve, and constrain the Keplerian orbital solutions of spectroscopic binaries, selected from the ninth Catalogue of Spectroscopic Binary Orbits (SB9 hereafter, see Pourbaix et al ). The SB9 yields information about orbital elements of several thousand spectroscopic binary systems.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533

et al. 2020

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We present the results of our second radial velocity (RV) monitoring campaign, carried out with the Échelle spectrograph FLECHAS at the University Observatory Jena in the course of the Großschwabhausen binary survey between December 2016 and June 2018. The aim of this project is to obtain precise RV measurements for spectroscopic binary stars in order to redetermine, verify, improve, and constrain their Keplerian orbital solutions. In this paper, we describe the observations, data reduction, and analysis and present the results of this project. In total, we have taken 721 RV measurements of 11 stars and derived well‐determined orbital solutions for nine systems (seven single‐ and two double‐lined spectroscopic binaries) with periods in the range between 2 and 70 days. In addition, we could rule out the orbital solutions for the previously classified spectroscopic binary systems HIP 107136 and HIP 107533, whose radial velocities are found to be constant on the km s−1‐level over a span of time of more than 500 days. In the case of HIP 2225, a significant change of its systematic velocity is detected between our individual observing epochs, indicating the presence of an additional companion, which is located on a wider orbit in this system.

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Section: Rv Measurementssupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533

et al. 2020

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“…This is the time when the L1 side of the primary is facing the line of sight, and it coincides with pulsation amplitude maximum, as we show below in Section 4. We find the best values for K and γ from the Bischoff et al (2017) RV data are unchanged from their values, 72.3 ± 0.3 and 0.7 ± 0.2 km s −1 , respectively.…”

Section: Co Cammentioning

confidence: 51%

“…The most recent radial velocity (RV) data on CO Cam were given by Bischoff et al (2017). We used the data from their Table A1 to reproduce the RV curve which we show here in Fig.…”

Section: Co Cammentioning

confidence: 99%

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The single-sided pulsator CO Camelopardalis

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et al. 2020

Monthly Notices of the Royal Astronomical Society

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CO Cam (TIC 160268882) is the second "single-sided pulsator" to be discovered. These are stars where one hemisphere pulsates with a significantly higher amplitude than the other side of the star. CO Cam is a binary star comprised of an Am δ Sct primary star with T eff = 7070±150 K, and a spectroscopically undetected G main-sequence secondary star. The dominant pulsating side of the primary star is centred on the L 1 point. We have modelled the spectral energy distribution combined with radial velocities, and independently the TESS light curve combined with radial velocities. Both of these give excellent agreement and robust system parameters for both stars. The δ Sct star is an oblique pulsator with at least four low radial overtone (probably) f modes with the pulsation axis coinciding with the tidal axis of the star, the line of apsides. Preliminary theoretical modelling indicates that the modes must produce much larger flux perturbations near the L 1 point, although this is difficult to understand because the pulsating star does not come near to filling its Roche lobe. More detailed models of distorted pulsating stars should be developed. These newly discovered single-sided pulsators offer new opportunities for astrophysical inference from stars that are oblique pulsators in close binary stars.

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The radial and rotational velocity of ζ Ophiuchi

Zehe¹,

Mugrauer²,

Neuhäuser³

et al. 2018

Astron Nachr

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We present the results of our spectroscopic monitoring campaign of Oph, carried out at the University observatory Jena with the spectrograph FLECHAS between July 2015 and September 2016. The main aim of the project was to determine the radial velocity of the star precisely, as a wide range of radial velocity measurements of Oph are given in the literature. Besides the proper motion and parallax, the radial velocity is an important input parameter for the calculation of the space motion of the star. Oph is considered to be a runaway star and potential former companion of the progenitor star of the pulsar PSR J1932+1059, both of which may have been located in a binary system and were then released during a supernova explosion about 1 Myr ago in the Upper Scorpius OB association. For the conclusion that the pulsar and Oph could have been at the same place, a radial velocity of −9.0 km s −1 for Oph was used in the literature. By analyzing the hydrogen and helium lines in 48 FLECHAS spectra, we determined the radial velocity of Oph to be 12.2 ± 3.3 km s −1 and the projected rotational velocity to be 432 ± 16 km s −1 with no indication of variability.

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Radial velocity measurements and orbit determination of eight single‐lined spectroscopic binary systems

Cited by 23 publications

References 14 publications

Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533

Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533

The single-sided pulsator CO Camelopardalis

The radial and rotational velocity of ζ Ophiuchi

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