Spectroscopic Orbits of Subsystems in Multiple Stars. III.

Tokovinin, Andreï

doi:10.3847/1538-3881/aacb78

Cited by 19 publications

(26 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The RVs delivered by this procedure should be on the absolute scale if the wavelength calibration is good. A comparison of CHIRON RVs with several RV standards revealed a small offset of +0.16 km s −1 (Tokovinin 2018c); in the following this offset is neglected. Figure 5 illustrates the 3-component cross-correlation function (CCF) derived from the CHIRON spectrum.…”

Section: Chiron Observationsmentioning

confidence: 92%

The compact multiple system HIP 41431

Borkovits

Sperauskas

Tokovinin

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The nearby (50 pc) K7V dwarf HIP 41431 (EPIC 212096658) is a compact 3tier hierarchy. Three K7V stars with similar masses, from 0.61 to 0.63 solar, make a triple-lined spectroscopic system where the inner binary with a period of 2.9 days is eclipsing, and the outer companion on a 59-day orbit exerts strong dynamical influence revealed by the eclipse time variation in the Kepler photometry. Moreover, the centre-of-mass of the triple system moves on a 3.9-year orbit, modulating the proper motion. The mass of the 4-th star is 0.35 solar. The Kepler and ground-based photometry and radial velocities from four different spectrographs are used to adjust the spectro-photodynamical model that accounts for dynamical interaction. The mutual inclination between the two inner orbits is 2. • 16±0. • 11, while the outer orbit is inclined to their common plane by 21 • ±16 • . The inner orbit precesses under the influence of both outer orbits, causing observable variation of the eclipse depth. Moreover, the phase of the inner binary is strongly modulated with a 59-day period and its line of apsides precesses. The middle orbit with eccentricity e = 0.28 also precesses, causing the observed variation of its radial velocity curve. Masses and other parameters of stars in this unique hierarchy are determined. This system is dynamically stable and likely old.

show abstract

Section: Chiron Observationsmentioning

confidence: 92%

The compact multiple system HIP 41431

Borkovits

Sperauskas

Tokovinin

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, even more complex hierarchical systems with five or more bodies are known to exist, and the statistics of high-multiplicity systems are steadily improving (e.g., Tokovinin 2018aTokovinin ,b, 2019a. The Multiple Star Catalogue (MSC; Tokovinin 1997Tokovinin , 2018c in particular contains information of hierarchical systems with N = 3 up to and including N = 7 stars.…”

Section: Introductionmentioning

confidence: 99%

A census of main-sequence interactions in the Multiple Star Catalogue

Hamers

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Statistics of hierarchical systems containing three or more stars are continuously improving. The Multiple Star Catalogue (MSC) is currently the most comprehensive catalogue of multiplestar systems and contains component masses, orbital periods, and additional information. The systems in the MSC are interesting for several reasons, including the long-term dynamical evolution of few-body systems. Although the secular evolution of triples and quadruples has been explored before, a systematic study of the systems in the MSC including also quintuples and sextuples has not been carried out. Here, we explore the main-sequence (MS) evolution of stars from the MSC based on approximately 2 × 10 5 secular dynamical integrations. We estimate statistical probabilities for strong interactions during the MS such as tidal evolution and mass transfer, and the onset of dynamical instability. Depending on the assumed model for the unknown orbital elements, we find that the fraction of noninteracting systems is largest for triples (∼ 0.9), and decreases to ∼ 0.6-0.8 for sextuples. The fraction of strong interactions increases from ∼ 0.1 to ∼ 0.2 from triples to sextuples, and the fraction of dynamically unstable systems increases from ∼ 0.001 to ∼ 0.1-0.2. The larger fractions of strong interactions and dynamical instability in systems with increasing multiplicity can be attributed to increasingly complex secular evolution in these systems. Our results indicate that a significant fraction of high-multiplicity systems interact or become dynamically unstable already during the MS, with an increasing importance as the number of stars increases.

show abstract

“…Table V shows the orbital parameters of the main binary system. The sub-binary system has an orbital period approximately of 111 days (48).…”

Section: Resultsmentioning

confidence: 99%

“…This system is formed by three components: A, Ba, and Bb. First, the astrometrical satellite Hipparcos discovered the visual pair, AB, and Tokovinin (48), studying the radial velocities of the system confirmed that the B component is binary. According to this research, the components, Ba and Bb have different magnitudes and the couple can be considered a single-lined spectroscopic binary, SB1.…”

mentioning

confidence: 99%

Physical and Dynamical Parameters of the Triple Stellar System: HIP 109951

et al. 2019

View full text Add to dashboard Cite

The precise determination of the physical and dynamical parameters of the HIP 109951 triple star system (WDS J22161-0705AB) which is formed by the A, Ba, and Bb components are presented. The binary nature of component B was recently confirmed by studying the radial velocities. The analysis of the system follows Al-Wardat's complex method for analyzing CVBS which employs Kurucz (Atlas9) line blanketed plane-parallel atmospheres simultaneously with an analytic method for dynamical analysis (we used Docobo's method) to calculate the parameters of this triple system. The result of our study yielded the following parameters: T A eff = 5836 ± 80 K, R A = 1.090 ± 0.039R , logg A = 4.45 ± 0.06, M A = 1.05 ± 0.16M ; T Ba eff = 5115 ± 80 K, R Ba = 0.596 ± 0.05R , log g Ba = 4.60 ± 0.07, M Ba = 0.83 ± 0.16M , T Bb eff = 4500 ± 80 K, R Bb = 0.490 ± 0.06R , log g Bb = 4.65 ± 0.07, and M Bb = 0.67 ± 0.16M based on the revised Hipparcos parallax. The orbital solution gave a total mass as M = 2.59M based on Gaia parallax and M = 2.15M based on the revised Hipparcos parallax. The synthetic spectral energy distributions (SED) and synthetic stellar photometry of the entire system and individual components are given and compared with the available observational ones. Finally, the positions of the system components on the HR diagram and the evolutionary tracks are given and their formation and the evolution of the system are discussed.

show abstract

Spectroscopic Orbits of Subsystems in Multiple Stars. III.

Cited by 19 publications

References 26 publications

The compact multiple system HIP 41431

The compact multiple system HIP 41431

A census of main-sequence interactions in the Multiple Star Catalogue

Physical and Dynamical Parameters of the Triple Stellar System: HIP 109951

Contact Info

Product

Resources

About