Doppler images of the eclipsing binary ER Vulpeculae

Xiang, Yue; Gu, Shuhang; Cameron, A. Collier; Barnes, John

doi:10.1093/mnras/stu2458

Cited by 13 publications

(10 citation statements)

References 43 publications

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“…We conclude that there is significant spot coverage on the inner hemisphere (white dwarf facing side of the M star) observed on all maps. This spot distribution -where there is a higher density of spots on the hemisphere facing the companion star -is similar to that observed in many other systems, such as the pre-CV V471 Tau (Hussain et al 2006), the eclipsing binary ER Vul (Xiang et al 2015), and the close binary σ 2 CrB (Strassmeier & Rice 2003). Furthermore, Kriskovics et al (2013) suggested that the hot-spots mapped on the companion-facing hemisphere in V824 Ara may indicate the strong interaction between the magnetic fields of the component stars, as is commonly observed in close RS CVn-type binaries.…”

Section: Surface Mapssupporting

confidence: 84%

The crowded magnetosphere of the post-common-envelope binary QS Virginis

Parsons

Hill

Marsh

et al. 2016

Mon. Not. R. Astron. Soc.

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We present high speed photometry and high resolution spectroscopy of the eclipsing post common envelope binary QS Virginis (QS Vir). Our UVES spectra span multiple orbits over more than a year and reveal the presence of several large prominences passing in front of both the M star and its white dwarf companion, allowing us to triangulate their positions. Despite showing small variations on a timescale of days, they persist for more than a year and may last decades. One large prominence extends almost three stellar radii from the M star. Roche tomography reveals that the M star is heavily spotted and that these spots are longlived and in relatively fixed locations, preferentially found on the hemisphere facing the white dwarf. We also determine precise binary and physical parameters for the system. We find that the 14, 220 ± 350 K white dwarf is relatively massive, 0.782 ± 0.013M ⊙ , and has a radius of 0.01068 ± 0.00007R ⊙ , consistent with evolutionary models. The tidally distorted M star has a mass of 0.382 ± 0.006M ⊙ and a radius of 0.381 ± 0.003R ⊙ , also consistent with evolutionary models. We find that the magnesium absorption line from the white dwarf is broader than expected. This could be due to rotation (implying a spin period of only ∼700 seconds), or due to a weak (∼100kG) magnetic field, we favour the latter interpretation. Since the M star's radius is still within its Roche lobe and there is no evidence that its over-inflated we conclude that QS Vir is most likely a pre-cataclysmic binary just about to become semi-detached.

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Section: Surface Mapssupporting

confidence: 84%

The crowded magnetosphere of the post-common-envelope binary QS Virginis

Parsons

Hill

Marsh

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In order to investigate the starspot activities on active close binaries, we have carried out a series of highresolution spectroscopic observations on targets with various stellar parameters and evolutionary stages (Gu et al 2003;Xiang et al 2014Xiang et al , 2015. In this work, we have derived the surface images of the K subgiant component of SZ Psc for 2004 November, 2006 September, October, November and December, through Doppler imaging technique.…”

Section: Introductionmentioning

confidence: 99%

The first Doppler images of the eclipsing binary SZ Piscium

Xiang

Cameron

et al. 2015

Mon. Not. R. Astron. Soc.

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We present the first Doppler images of the active eclipsing binary system SZ Psc, based on the high-resolution spectral data sets obtained in 2004 November and 2006 September-December. The least-squares deconvolution technique was applied to derive high signal-to-noise profiles from the observed spectra of SZ Psc. Absorption features contributed by a third component of the system were detected in the LSD profiles at all observed phases. We estimated the mass and period of the third component to be about 0.9M ⊙ and 1283±10 d, respectively. After removing the contribution of the third body from the LSD profiles, we derived the surface maps of SZ Psc. The resulting Doppler images indicate significant starspot activities on the surface of the K subgiant component. The distributions of starspots are more complex than that revealed by previous photometric studies. The cooler K component exhibited pronounced high-latitude spots as well as numerous low-and intermediate-latitude spot groups during the entire observing seasons, but did not show any large, stable polar cap, different from many other active RS CVn-type binaries.

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“…Several active single rapid rotators, such as AB Dor (Collier Cameron & Unruh 1994) and FK Com-type stars (Strassmeier et al 1999), were also reported to have large polar active regions. In our previous works, we found persistent highlatitude or polar features on the active binaries with various rotational speeds, such as II Peg (v sin i = 22 km s −1 ; Xiang et al 2014), SZ Psc (v sin i = 67.7 km s −1 ; Xiang et al 2016) and ER Vul (v sin i = 80 km s −1 ; Xiang et al 2015).…”

Section: Discussionmentioning

confidence: 83%

“…The Doppler imaging technique can offer a better constraint on spot latitudes. In order to investigate the spot activities of active binary stars, we continued to monitor a set of RS CVn-type binary systems (Gu et al 2003;Xiang et al 2014Xiang et al , 2015Xiang et al , 2016. In this study, we performed high-resolution spectroscopic observations on the active binary prototype RS CVn using three telescopes located at different observing sites.…”

Section: Introductionmentioning

confidence: 99%

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

Xiang

Wolter

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the first Doppler images of the prototypical active binary star RS CVn, derived from high-resolution spectra observed in 2004, 2016 and 2017, using three different telescopes and observing sites. We apply the least-squares deconvolution technique to all observed spectra to obtain high signal-to-noise line profiles, which are used to derive the surface images of the active K-type component. Our images show a complex spot pattern on the K star, distributed widely in longitude. All starspots revealed by our Doppler images are located below a latitude of about 70°. In accordance with previous light-curve modeling studies, we find no indication of a polar spot on the K star. Using Doppler images derived from two consecutive rotational cycles, we estimate a surface differential rotation rate of ∆Ω = −0.039 ± 0.003 rad d −1 and α = ∆Ω/Ω eq = −0.030 ± 0.002 for the K star. Given the limited phase coverage during those two rotations, the uncertainty of our differential rotation estimate is presumably higher.

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Doppler images of the eclipsing binary ER Vulpeculae

Cited by 13 publications

References 43 publications

The crowded magnetosphere of the post-common-envelope binary QS Virginis

The crowded magnetosphere of the post-common-envelope binary QS Virginis

The first Doppler images of the eclipsing binary SZ Piscium

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

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