The flare activity of V390 Aur: First results of an international collaboration

Konstantinova-Antova, R.; Antov, A.; Zhilyaev, B. E.; Verlyuk, I. A.; Romaniuk, Ya. O.; Svyatogorov, O. A.; Avgoloupis, S.; Seiradakis, J. H.; Contadakis, M. E.

doi:10.1002/asna.200310337

Cited by 3 publications

(5 citation statements)

References 8 publications

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“…Temperature polar spots were reported for giants in RS CVn systems and for FK Com-type stars by Strassmeier (1997), Korhonen et al (2002), andStrassmeier (2002). This surface structure with close magnetic spots might explain the flare activity properties of the star reported in optical and X-ray (Konstantinova-Antova et al 2000;Gondoin 2003;Konstantinova-Antova et al 2005), such as the groups of optical flares and the "continuous flare activity" in the corona.…”

Section: Discussionmentioning

confidence: 69%

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Magnetic field structure in single late-type giants: the effectively single giant V390 Aurigae

Konstantinova-Antova

Aurière

Petit

et al. 2012

A&A

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Aims. We have studied the active giant V390 Aur using spectropolarimetry to obtain direct and simultaneous measurements of the magnetic field and the activity indicators to obtain a precise insight of its activity. Methods. We used the spectropolarimeter NARVAL at the Bernard Lyot Telescope (Observatoire du Pic du Midi, France) to obtain a series of Stokes I and Stokes V profiles. Using the least-squares deconvolution (LSD) technique we were able to detect the Zeeman signature of the magnetic field in each of our 13 observations and to measure its longitudinal component. Using the wide wavelength range of the spectra we were able to monitor the CaII K&H and IR triplet, as well as the H α lines, which are activity indicators. To reconstruct the magnetic field geometry of V390 Aur on the basis of modelling the Stokes V profiles, we applied the Zeeman Doppler imaging (ZDI) inversion method and present a map for the magnetic field. Based on the obtained spectra, we also refined the fundamental parameters of the star and the Li abundance using MARCS model atmospheres. Results. The ZDI revealed a structure in the radial magnetic field consisting of a polar magnetic spot of positive polarity and several negative spots at lower latitude. A high latitude belt is present on the azimuthal field map, indicative of a toroidal field close to the surface. Similar features are observed in some RS CVn and FK Com -type stars. It was found that the photometric period cannot fit the behaviour of the activity indicators formed in the chromosphere. Their behaviour suggests slower rotation compared to the photosphere, but our dataset is too short for us to be able to estimate their exact periods. All these results can be explained in terms of an α−ω dynamo operation, taking into account the stellar structure and rotation properties of V390 Aur that we studied with up-to-date stellar models computed at solar metallicity with the code STAREVOL. The calculated Rossby number also points to a very efficient dynamo.

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Section: Discussionmentioning

confidence: 69%

“…This surface structure with close magnetic spots could explain the flare activity properties of the star reported in optical and X-ray (Konstantinova-Antova et al 2000;Gondoin 2003;Konstantinova-Antova et al 2005), like the groups of optical flares and the "continuous flare activity" in the corona.…”

Section: Discussionmentioning

confidence: 75%

Magnetic field structure in single late-type giants: the effectively single giant V390 Aurigae

Konstantinova-Antova

Aurière

Petit

et al. 2012

A&A

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“…As a result, the components of this visual binary were observed together in the aperture of both previous spectral observations and ours. A detailed discussion on this point is presented in Konstantinova-Antova et al (2005) and in the present paper.…”

Section: Introductionmentioning

confidence: 84%

“…The mass of V390 Aur is estimated to be 1.8 M (Gondoin 2003). The secondary has been estimated as G1V (Stephenson& Sandwall 1969), or an F dwarf or a subgiant (Konstantinova-Antova et al 2005) and these authors suggest a mass of 1.3 M . With this last assumption and a circular orbit hypothesis, KonstantinovaAntova et al (2005) estimated a 140 year orbital period for ADS 3812.…”

Section: Magnetic Field and The Behaviour Of The Activity Indicatorsmentioning

confidence: 99%

“…Later studies of V390 Aur in the X-ray (Huensch et al 1998;Gondoin 1999Gondoin , 2003 and in the optical (Konstantinova-Antova et al 2000;Konstantinova-Antova et al 2005) revealed a high Xray luminosity of about 10 30 erg cm −2 s −1 , and optical flares. In the present study we obtained, for the first time, direct evidence of a magnetic field in this active giant at several phases of its rotational period, and we simultaneously followed the behaviour of the spectral line activity indicators CaII K&H, H α and the CaII IR triplet.…”

Section: Introductionmentioning

confidence: 98%

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Direct detection of a magnetic field at the surface of V390 Aurigae – an effectively single active giant

Konstantinova-Antova

Aurière

Iliev

et al. 2008

A&A

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Aims. We have studied the active giant V390 Aur using spectropolarimetry to obtain direct and simultaneous measurements of the magnetic field and the activity indicators in order to infer the origin of the activity. Methods. We used the new spectropolarimeter NARVAL at the Bernard Lyot Telescope (Observatoire du Pic du Midi, France) to obtain a series of Stokes I and Stokes V profiles. Using the LSD technique we were able to detect the Zeeman signature of the magnetic field in each of our 5 observations and to measure its longitudinal component. Using the wide wavelength range of the spectra we could monitor the CaII K&H and IR triplet, as well as the H α lines which are activity indicators. The Stokes I LSD profiles enabled us to detect and measure the profiles of two weak stellar companions. Analysis (RV and EW) of the absorption components of the Stokes I LSD profile shows that the secondary of the visual wide orbit binary ADS 3812 is itself a spectroscopic binary, and suggests that the synchronization effect does not play role for V390 Aur (the primary), and that the giant should be considered as effectively single with regard to its fast rotation and activity.

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Observations of high-frequency variability in the chromospherically active star V390 Aurigae

Zhilyaev¹,

Verlyuk²,

Андреев³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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The flare activity of V390 Aur: First results of an international collaboration

Cited by 3 publications

References 8 publications

Magnetic field structure in single late-type giants: the effectively single giant V390 Aurigae

Magnetic field structure in single late-type giants: the effectively single giant V390 Aurigae

Direct detection of a magnetic field at the surface of V390 Aurigae – an effectively single active giant

Observations of high-frequency variability in the chromospherically active star V390 Aurigae

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