The first Doppler imaging of the active binary prototype RS Canum Venaticorum

Xiang, Yue; Gu, Shuhang; Wolter, Uwe; Schmitt, J. H. M. M.; Cameron, A. Collier; Barnes, John; Mittag, M.; Perdelwitz, V.; Kohl, Sina

doi:10.1093/mnras/staa063

Cited by 10 publications

(4 citation statements)

References 59 publications

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“…The active longitude switches from one hemisphere to the other. Xiang et al (2020) presented the first Doppler images of the active K-type component of the prototypical binary star RS Canum Venaticorum. The maps showed that the spots located below a latitude of about 70°, but distributed widely in longitude.…”

Section: Introductionmentioning

confidence: 99%

Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

Niu¹,

Fu²,

Wang³

et al. 2022

Res. Astron. Astrophys.

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The LAMOST spectra and Kepler light curves are combined to investigate the detached eclipsing binary KIC 8098300, which shows the O’Connell effect caused by spot/facula modulation. The radial velocity (RV) measurements are derived by using the tomographic spectra disentangling technology. The mass ratio q = K 1/K 2 = 0.812 ± 0.007, and the orbital semimajor axis a sin i = 14.984 ± 0.048 R ⊙ are obtained by fitting the RV curves. We optimize the binary model concerning the spot/facula activity with the code PHOEBE and obtain precise parameters of the orbit including the eccentricity e = 0.0217 ± 0.0008, the inclination i = 87.°71 ± 0.°04, and the angle of periastron ω = 284.°1 ± 0.°5. The masses and radii of the primary and secondary star are determined as M 1 = 1.3467 ± 0.0001 M ⊙, R 1 = 1.569 ± 0.003 R ⊙, and M 2 = 1.0940 ± 0.0001 M ⊙, R 2 = 1.078 ± 0.002 R ⊙, respectively. The ratio of temperatures of the two component stars is r teff = 0.924 ± 0.001. We also obtain the periastron precession speed of 0.000024 ± 0.000001 day cycle−1. The residuals of out-of-eclipse are analyzed using the auto-correlation function and the discrete Fourier transform. The spot/facula activity is relatively weaker, but the lifetime is longer than that of most single main sequence stars in the same temperature range. The average rotation period of the spots P rot = 4.32 days is slightly longer than the orbital period, which may be caused by either the migration of spots/faculae along the longitude or the latitudinal differential rotation. The activity may be spot-dominated for the secondary star and facula-dominated for the primary star. The method of this work can be used to analyze more eclipsing binaries with the O’Connell effect in the Kepler field to obtain the precise parameters and investigate the difference of spot behavior between binaries and single stars. It is helpful for a deeper understanding of the stellar magnetic activity and dynamo theory.

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Section: Introductionmentioning

confidence: 99%

Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

Niu¹,

Fu²,

Wang³

et al. 2022

Res. Astron. Astrophys.

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“…Based on the detailed investigation of the eclipse time variations in Kepler binaries, Balaji et al (2015) found that half of close binaries exhibit asynchronous differential rotations on their component stars. Furthermore, to uncover stellar differential rotation, the Doppler imaging technique (Gu et al 2003;Özdarcan et al 2016;Xiang et al 2020) has been proposed by tracing the spot migration on the stellar surface. However, this technique requires high-resolution and long-term spectroscopic observations, which greatly limit its application over a wide range.…”

Section: Introductionmentioning

confidence: 99%

OO Leo: An Active Contact Binary with Possible Solar-like Differential Rotation

Meng,

Wu,

et al. 2024

ApJ

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With Transiting Exoplanet Survey Satellite (TESS) high-precision photometry and Large Sky Area Multi-object Fiber Spectroscopic Telescope medium-resolution spectra, we present the first light and radial velocity curve analyses for the eclipsing binary OO Leo. The simultaneous solution suggests that OO Leo is a W-subtype contact binary with a relatively low mass ratio (1/q = 0.173) and a moderate degree of contact (f = 28.1%). The asymmetry and continuous changes observed in the TESS light curve were properly modeled by one retrograde cool spot on its secondary surface. A detailed investigation of the Hα line also confirmed that the secondary star had a high level of magnetic activity. The retrograde longitudinal motion of the spot can be explained by a solar-like differential rotation in the secondary component. The orbital period investigation revealed that OO Leo is undergoing a secular decrease and a cyclic variation in its orbital period. The secular decrease may be mainly caused by mass transfer from the more massive secondary star to the less massive primary star. The cyclic period variation can be explained by the light–time effect of an invisible third body or the cyclic magnetic activity of the secondary star. The long-lived spot migration in the longitudinal direction makes OO Leo an excellent target for investigating the differential rotations of contact binaries.

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“…Starspots on binaries with rapidly rotating late-type components are prominent (Holzwarth & Schüssler 2003a,b;Lurie et al 2017), such as RS CVn stars (Gu et al 2003;Xiang et al 2020a) and W UMa stars (Barnes et al 2004;Şenavcı et al 2011). The properties of starspot on binary can be studied from Doppler/Zeeman Doppler images (Gu et al 2003;Xiang et al 2020b) and photometry (Özavcı et al 2018;Pi et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Properties and Evolutions of Starspots on Three Detached Eclipsing Binaries in the LAMOST-Kepler survey

Wang,

Fu,

Zong

et al. 2022

Preprint

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The spotted detached eclipsing binary (DEB) offers insights into starspots on the binary. Three spotted DEBs, KIC 8097825, KIC 6859813, and KIC 5527172, which were observed by the 𝐾𝑒 𝑝𝑙𝑒𝑟 photometry and LAMOST spectroscopy, are studied in this work. The physical parameters of binaries are determined by binary modeling. The sizes, lifetimes, and single/double-dip ratio (SDR) of starspots are derived by starspot analysis. KIC 8097825 has large starspots. KIC 6859813 has a spot rotation period shorter than its orbital period but the system should be synchronized inferred from timescale estimation. The difference may be the result of the surface differential rotation. The KIC 5527172 has a long spot lifetime and an M dwarf component with an inflation radius. The primaries of these binaries and the secondary of KIC 8097825 have spots. Adding spotted DEBs of literature, we compare the starspots on binaries with those on the single stars. The spot sizes of starspots on 65% binaries are smaller than the median of those on single stars. The lifetimes of starspots on binaries are consistent with those on single stars when the rotation periods are larger than 3 days. SDRs for half of the binaries are consistent with those of single star systems, while another half are smaller. The relative lifetime positively correlates with the RMS and SDR but negatively correlates with the rotation period. These relations are similar to those of spots on the single star systems. Binaries with luminosity ratios close to the unit tend to have more double dips.

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The first Doppler imaging of the active binary prototype RS Canum Venaticorum

Cited by 10 publications

References 59 publications

Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions

OO Leo: An Active Contact Binary with Possible Solar-like Differential Rotation

The Properties and Evolutions of Starspots on Three Detached Eclipsing Binaries in the LAMOST-Kepler survey

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