Chromospheric activity and unique solution of SZ Psc

Kang, Yong; Lee, Woo-Baik; Kim, Ho-il; Oh, Kyu-Dong

doi:10.1046/j.1365-8711.2003.06909.x

Cited by 11 publications

(3 citation statements)

References 15 publications

(29 reference statements)

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“…Their physical and orbital parameters were taken from compilations made by Popper (1988Popper ( , 1990, and supplemented by works of other authors (Imbert 1978;Arnold et al 1979;Cerruti-Sola et al 1980;Tümer et al 1985;Fekel 1991;Nelson et al 1991;Burki et al 1992;Eaton et al 1993;Young 1993;Hackert & Ordway 1995;Kang et al 2003), with the exception of CF Tuc, which analysis was revised by Dogru et al (2009). We also added to the sample three unpublished systems we have analysed (ASAS-06, ASAS-11, ASAS-16), one of which does not have reliable temperature estimations (ASAS-16).…”

Section: Giants With and Without Spots In Eclipsing Binariesmentioning

confidence: 99%

“…The 'spotted' sample is built of the three targets described here, V1980 Sgr and ASAS J010538-8003.7 from Ratajczak et al (2013) 3 , and a number of so-called 'classical RS CVn-type stars', namely: RZ Eri, GK Hya, CF Tuc, RU Cnc, VV Mon, SS Cam, CQ Aur, SS Boo, V792 Her, SZ Psc, LX Per, and RS CVn itself 4 . Their physical and orbital parameters were taken from compilations made by Popper (1988Popper ( , 1990, and supplemented by works of other authors (Imbert 1978;Arnold et al 1979;Cerruti-Sola et al 1980;Tümer et al 1985;Fekel 1991;Nelson et al 1991;Burki et al 1992;Eaton et al 1993;Young 1993;Hackert & Ordway 1995;Kang et al 2003), with the exception of CF Tuc, which analysis was revised by Dogru et al (2009). We also added to the sample three unpublished systems we have analysed (ASAS-06, ASAS-11, ASAS-16), one of which does not have reliable temperature estimations (ASAS-16).…”

Section: Giants With and Without Spots In Eclipsing Binariesmentioning

confidence: 99%

See 1 more Smart Citation

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Ratajczak

Hełminiak

Konacki

et al. 2016

Mon. Not. R. Astron. Soc.

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We present spectroscopic and photometric solutions for three spotted systems with red giant components. Absolute physical and orbital parameters for these double-lined detached eclipsing binary stars are presented for the first time. These were derived from the V -, and I -band ASAS and WASP photometry, and new radial velocities calculated from high quality optical spectra we obtained with a wide range of spectrographs and using the two-dimensional cross-correlation technique (TODCOR). All of the investigated systems (ASAS J184949-1518.7, BQ Aqr, and V1207 Cen) show the differential evolutionary phase of their components consisting of a main sequence star or a subgiant and a red giant, and thus constitute very informative objects in terms of testing stellar evolution models. Additionally, the systems show significant chromospheric activity of both components. They can be also classified as classical RS CVn-type stars. Besides the standard analysis of radial velocities and photometry, we applied spectral disentangling to obtain separate spectra for both components of each analysed system which allowed for a more detailed spectroscopic study. We also compared the properties of red giant stars in binaries that show spots, with those that do not, and found that the activity phenomenon is substantially suppressed for stars with Rossby number higher than ∼1 and radii larger than ∼20 R ⊙ .

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Section: Giants With and Without Spots In Eclipsing Binariesmentioning

confidence: 99%

Section: Giants With and Without Spots In Eclipsing Binariesmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Ratajczak

Hełminiak

Konacki

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Since the first light variation was detected by Jensch (1934), SZ Psc remained an exciting source for photometric and spectroscopic observations throughout the last century (Jakate et al 1976;Catalano et al 1978;Tumer & Kurutac 1979;Eaton et al 1982;Tunca 1984;Antonopoulou et al 1995;Lanza et al 2001). Starspot modeling performed on SZ Psc suggested the presence of several active regions on the surface of the cooler subgiant component (Eaton & Hall 1979;Lanza et al 2001;Kang et al 2003). The first Doppler images of SZ Psc were generated by Xiang et al (2016) using highresolution optical spectra.…”

Section: Introductionmentioning

confidence: 99%

Swift and XMM–Newton observations of an RS CVn-type eclipsing binary SZ Psc: superflare and coronal properties

Karmakar

Naik

Pandey

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present an in-depth study of a large and long duration (>1.3 days) X-ray flare observed on an RS CVn type eclipsing binary system SZ Psc using observations from Swift observatory. In the 0.35–10 keV energy band, the peak luminosity is estimated to be 4.2× 1033 $\rm {erg}~\rm {s}^{-1}$. The quiescent corona of SZ Psc was observed ∼5.67 d after the flare using Swift observatory, and also ∼1.4 yr after the flare using the XMM-Newton satellite. The quiescent corona is found to consist of three temperature plasma: 4, 13, and 48 MK. High-resolution X-ray spectral analysis of the quiescent corona of SZ Psc suggests that the high first ionization potential (FIP) elements are more abundant than the low-FIP elements. The time-resolved X-ray spectroscopy of the flare shows a significant variation in the flare temperature, emission measure, and abundance. The peak values of temperature, emission measure, and abundances during the flare are estimated to be 199±11 MK, 2.13±0.05 × 1056 cm−3, 0.66±0.09 $\rm {Z}_{\odot }$, respectively. Using the hydrodynamic loop modeling, we derive the loop length of the flare as 6.3±0.5 × 1011 cm, whereas the loop pressure and density at the flare peak are derived to be 3.5±0.7 × 103 dyne cm−2 and 8±2 × 1010 cm−3, respectively. The total magnetic field to produce the flare is estimated to be 490±60 G. The large magnetic field at the coronal height is supposed to be due to the presence of an extended convection zone of the sub-giant and the high orbital velocity.

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New observations of chromospheric and prominence activity on the RS CVn-type binary SZ Piscium

Cao

2012

A&A

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Aims. New high-resolution spectroscopic observations were made for the RS CVn-type binary SZ Psc aimed at searching for evidence of stellar prominences in this system and studying its chromospheric activity. Methods. By means of the spectral subtraction technique, we searched for prominence-like events in the H α spectra, and also analyzed several optical chromospheric activity indicators (the He i D 3 , Na i D 1 , D 2 , H α , and Ca ii IRT lines) included in our observations. Results. The emission in the H α and Ca ii IRT lines show that the cooler component is very active, supporting earlier work. Notably, some absorption features are detected in the subtracted H α profiles, and one of them may result from prominence-like material on the cooler component of the system. According to a model of stellar prominences, the distance of the prominence from the rotation axis of the cooler component is calculated to be close to the corotation radius and to exceed the Roche lobe of the cooler component.

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Chromospheric activity and unique solution of SZ Psc

Cited by 11 publications

References 15 publications

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Swift and XMM–Newton observations of an RS CVn-type eclipsing binary SZ Psc: superflare and coronal properties

New observations of chromospheric and prominence activity on the RS CVn-type binary SZ Piscium

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