A spectroscopic quadruple as a possible progenitor of sub-Chandrasekhar type Ia supernovae

Merle, Thibault; Hamers, Adrian S.; Eck, S. Van; Jorissen, A.; Swaelmen, M. Van der; Pollard, K. R.; Smiljanić, R.; Pourbaix, D.; Zwitter, T.; Traven, G.; Gilmore, G.; Randich, S.; Gonneau, A.; Hourihane, A.; Sacco, G. G.; Worley, C. C.

doi:10.1038/s41550-022-01664-5

Cited by 6 publications

(3 citation statements)

References 47 publications

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“…Leaving aside the unknown consequences of period resonance, we could use the code MSE, which combines secular and dynamical evolution of multiple stellar systems with stellar evolution (Hamers et al 2021b). Similar study was performed, for example, by Merle et al (2022). However, the ratio of orbital periods between the inner and outer orbits in CzeV343 is so large that individual model runs in MSE would take many tens of hours.…”

Section: Future Evolutionsupporting

confidence: 55%

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The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Pejcha

Cagaš

Landri

et al. 2022

A&A

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CzeV343 (=V849 Aur) was previously identified as a candidate double eclipsing binary (2+2 quadruple), where the orbital periods of the two eclipsing binaries (P A ≈ 1.2 days and P B ≈ 0.8 days) lie very close to a 3:2 resonance. Here, we analyze 11 years of ground-based photometry, four sectors of Transiting Exoplanet Survey Satellite (TESS) 2-minute and full-frame photometry, and two optical spectra. We construct a global model of our photometry, including apsidal motion of binary A and the light-travel time effect (LTTE) of the mutual outer orbit, and explore the parameter space with Markov Chain Monte Carlo. We estimate component masses for binary A (1.8 + 1.3 M ) and binary B (1.4 + 1.2 M ). We identify the pseudo-synchronous rotation signal of binary A in TESS photometry. We detect apsidal motion in binary A with a period of about 33 years, which is fully explained by tidal and rotational contributions of stars aligned with the orbit. The mutual orbit has a period of about 1450 days and an eccentricity of about 0.7. The LTTE amplitude is small, which points to low inclination of the outer orbit and a high degree of misalignment with the inner orbits. We find that when apsidal motion and the mutual orbit are taken into account, the orbital period resonance is exact to within 10 −5 cycles/day. Many properties of CzeV343 are not compatible with requirements of the 3:2 resonance capture theory for coplanar orbits. Future evolution of CzeV343 can lead to mergers, triple common envelope, double white dwarf binaries, or a Type Ia supernova. More complex evolutionary pathways will likely arise from dynamical instability caused by orbital expansion when either of thez binaries undergoes mass transfer. This instability has not been explored so far in 2+2 quadruples.

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Section: Future Evolutionsupporting

confidence: 55%

“…In this case, some of these evolutionary pathways would actually include mass transfer from the merged product of binary A to binary B. This mass transfer can either remain stable or it can culminate in triple common envelope evolution (Glanz & Perets 2021;Hamers et al 2022a;Merle et al 2022).…”

Section: Future Evolutionmentioning

confidence: 99%

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Pejcha

Cagaš

Landri

et al. 2022

A&A

View full text Add to dashboard Cite

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“…It is possible, however, that the C&D components merge at an earlier time due to secularly driven high eccentricity. In this scenario, and depending on the outer orbit, the merger remnant could potentially fill its Roche lobe around the A&B black hole binary system as it evolves (see, e.g., de Vries et al 2014;Glanz & Perets 2021;Hamers et al 2022;Merle et al 2022). This could in turn lead to either stable mass transfer or common-envelope evolution; in the latter case, the black holes could merge during the process in a gas-rich environment, and potentially produce EM counterpart observations.…”

Section: Speculation On the Role Of The Third And Fourth Companionsmentioning

confidence: 99%

Investigating the Chemically Homogeneous Evolution Channel and Its Role in the Formation of the Enigmatic Binary Black Hole Progenitor Candidate HD 5980

Sharpe,

van Son,

de Mink

et al. 2024

ApJ

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Chemically homogeneous evolution (CHE) is a promising channel for forming massive binary black holes. The enigmatic, massive Wolf–Rayet binary HD 5980 A&B has been proposed to have formed through this channel. We investigate this claim by comparing its observed parameters with CHE models. Using MESA, we simulate grids of close massive binaries, then use a Bayesian approach to compare them with the stars’ observed orbital period, masses, luminosities, and hydrogen surface abundances. The most probable models, given the observational data, have initial periods ∼3 days, widening to the present-day ∼20 days orbit as a result of mass loss—correspondingly, they have very high initial stellar masses (≳150 M ⊙). We explore variations in stellar-wind mass loss and internal mixing efficiency, and find that models assuming enhanced mass loss are greatly favored to explain HD 5980, while enhanced mixing is only slightly favored over our fiducial assumptions. Our most probable models slightly underpredict the hydrogen surface abundances. Regardless of its prior history, this system is a likely binary black hole progenitor. We model its further evolution under our fiducial and enhanced wind assumptions, finding that both stars produce black holes with masses ∼19–37 M ⊙. The projected final orbit is too wide to merge within a Hubble time through gravitational waves alone. However, the system is thought to be part of a 2+2 hierarchical multiple. We speculate that secular effects with the (possible) third and fourth companions may drive the system to promptly become a gravitational-wave source.

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A star under multiple influences

Kővári,

Strassmeier,

Kriskovics

et al. 2024

A&A

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Close binaries with magnetically active components are astrophysical laboratories for studying the effects of binarity on activity. Of particular interest are binary and multiple star systems that contain a solar-type active component with an internal structure similar to the Sun, allowing us to study how the dynamo of a solar-type star would work under different conditions. We have conducted a comprehensive investigation of V815\,Her using photometric and spectroscopic data to understand the origin of the activity and what influences it in the short and long term. Using space photometry we performed light curve modeling in order to derive astrophysical and orbital parameters for the eclipsing binary subsystem V815\,Her B. Using archival photometric data covering a century we carried out a time frequency analysis. Spectral synthesis was applied to determine the basic astrophysical parameters of the rapidly rotating primary using high-resolution STELLA spectra recorded in 2018. Photometric analysis of archived data revealed multiple cycles on timescales between sim 6.5 and sim 26 years, some of which may be harmonic. From TESS photometry we obtained an orbital solution for the V815\,Her B subsystem. By placing the primary component on the Hertzsprung$-$Russell-diagram, we could deduce an age of approx 30\,Myr, in line with the high Li-6707 abundance. The STELLA spectra covering the 200 day-long observing season enabled us to create 19 time-series Doppler images, which revealed a constantly changing spotted surface on a timescale of a few weeks. From the consecutive image pairs we built up the average cross-correlation function map to measure the surface differential rotation of the spotted star, from which we derive a weak solar-type surface shear. We found evidence that the V815\,Her B component previously apostrophized as a "third body" is actually an eclipsing close binary subsystem of two M dwarfs with a period of 0.5\,d, that is, V815\,Her is a 2+2 hierarchical quadruple system. The system is apparently young, only a few times ten million years old, consistent with the spotted primary V815\,Her Aa being a zero-age main-sequence star. Spot activity on the primary was found to be vivid. Fast starspot decay suggests that convective-turbulent erosion plays a more significant role in such a rapidly rotating star. The weak surface shear of V815\,Her Aa due to differential rotation is presumably confined by tidal forces of the close companion V815\,Her Ab. The slowly increasing photometric cycle of about 6.5 years on average is interpreted as a spot cycle of V815\,Her Aa, which is probably modulated by the eccentric wide orbit.

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A spectroscopic quadruple as a possible progenitor of sub-Chandrasekhar type Ia supernovae

Cited by 6 publications

References 47 publications

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance

Investigating the Chemically Homogeneous Evolution Channel and Its Role in the Formation of the Enigmatic Binary Black Hole Progenitor Candidate HD 5980

A star under multiple influences

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