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

Cao, Dongtao; Gu, Shuhang

doi:10.1051/0004-6361/201118184

Cited by 13 publications

(4 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We obtain the chromospheric contribution in these activity indicators with the spectral subtraction technique by using the popular program STARMOD (Barden 1985;Montes et al 1995cMontes et al , 1997Montes et al , 2000. This technique has been widely and successfully used for chromospheric activity studies (e.g., Montes et al 1995cMontes et al , 1997Montes et al , 2000Gu et al 2002;Frasca et al 2008a;Zhang & Gu 2008;Cao & Gu 2012, 2014, 2015Zhang et al 2016). Although a spectral line from the third star has been found in the UX Ari spectrum, the contribution of the lines is very weak.…”

Section: Spectral Subtraction and Resultsmentioning

confidence: 99%

Optical flare events on the RS Canum Venaticorum star UX Arietis

Cao

2017

Res. Astron. Astrophys.

Self Cite

View full text Add to dashboard Cite

Based on long-term high-resolution spectroscopic observations obtained during five observing runs from 2001 to 2004, we study optical flare events and chromospheric activity variability of the very active RS CVn star UX Ari. By means of the spectral subtraction technique, several optical chromospheric activity indicators (including the He I D 3 , Na I D 1 , D 2 doublet, Hα and Ca II IRT lines) covered in our echelle spectra were analyzed. Four large optical flare events were detected on UX Ari during our observations, which show prominent He I D 3 line emission together with great enhancement in emission of the Hα and Ca II IRT lines and strong filled-in or emission reversal features in the Na I D 1 , D 2 doublet lines. The newly detected flares are much more energetic than previous discoveries, especially for the flare identified during the 2002 December observing run. Optical flare events on UX Ari are more likely to be observed around two quadratures of the system, except for our optical flares detected during the 2004 November observing run. Moreover, we have found rotational modulation of chromospheric activity in the Hα and Ca II IRT lines, which suggests the presence of chromospherically active longitudes over the surface of UX Ari. The change in chromospherically active longitudes among our observing runs, as well as the variation in chromospheric activity level from 2001 to 2004, indicates a long-term evolution of active regions.

show abstract

Section: Spectral Subtraction and Resultsmentioning

confidence: 99%

Optical flare events on the RS Canum Venaticorum star UX Arietis

Cao

2017

Res. Astron. Astrophys.

Self Cite

View full text Add to dashboard Cite

show abstract

“…These images revealed that the K1 IV star exhibits pronounced high-latitude spots as well as numerous intermediate-and low-latitude spot groups during the entire observing season. High level of chromospheric activity associated with the K1 IV primary component was also demonstrated by strong chromospheric emission in Mg ii h & k, Ca ii H & K, Hα, and Ca ii infrared-triplet lines (e.g., Jakate et al 1976;Bopp et al 1981;Zhang & Gu 2008;Cao & Gu 2012). Hα outbursts and flare like events were detected by Bopp et al (1981), Ramsey & Nations (1981), and Huenemoerder & Ramsey (1984).…”

Section: Introductionmentioning

confidence: 90%

“…The authors also found variation in Mg ii strength, possibly phase-dependent, and an apparent eclipse of a plage in Mg ii. However, excess absorption features in the subtracted Hα profiles caused by prominence-like material have been discussed by Zhang & Gu (2008) and Cao & Gu (2012). Several optical chromospheric activity indicators were analyzed by Cao et al (2019) using the spectral subtraction technique, and during their observation, a series of possibly associated magnetic activity phenomena, including flare-related prominence activation, optical flare, and post-flare loops, were detected.…”

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

View full text Add to dashboard Cite

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.

show abstract

“…They found EW 8542 /EW 8498 ratios of 1.0-1.7, which implies the presence of optically thick plages. This is typical of many late-type stars [111,[122][123][124][125][126]. The infrared triplet lines are formed in the lower chromosphere through subordinate transitions between the excited levels of Ca II 4 2 P 1/2,2/3 and meta-stable 3 2 D 3/2,5/2 [127,128].…”

Section: Spectroscopic Diagnosticsmentioning

confidence: 98%

Stellar Chromospheric Variability

Grijs

Kamath

2021

Universe

View full text Add to dashboard Cite

Cool stars with convective envelopes of spectral types F and later tend to exhibit magnetic activity throughout their atmospheres. The presence of strong and variable magnetic fields is evidenced by photospheric starspots, chromospheric plages and coronal flares, as well as by strong Ca ii H+K and Hα emission, combined with the presence of ultraviolet resonance lines. We review the drivers of stellar chromospheric activity and the resulting physical parameters implied by the observational diagnostics. At a basic level, we explore the importance of stellar dynamos and their activity cycles for a range of stellar types across the Hertzsprung–Russell diagram. We focus, in particular, on recent developments pertaining to stellar rotation properties, including the putative Vaughan–Preston gap. We also pay specific attention to magnetic variability associated with close binary systems, including RS Canum Venaticorum, BY Draconis, W Ursae Majoris and Algol binaries. At the present time, large-scale photometric and spectroscopic surveys are becoming generally available, thus leading to a resurgence of research into chromospheric activity. This opens up promising prospects to gain a much improved understanding of chromospheric physics and its wide-ranging impact.

show abstract

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

Cited by 13 publications

References 24 publications

Optical flare events on the RS Canum Venaticorum star UX Arietis

Optical flare events on the RS Canum Venaticorum star UX Arietis

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

Stellar Chromospheric Variability

Contact Info

Product

Resources

About