The photometric variability of the chromospherically active binary star HD 80715

Strassmeier, K. G.; Hooten, James T.; Hall, D. S.; Fekel, Francis C.

doi:10.1086/132407

Cited by 48 publications

(85 citation statements)

References 5 publications

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“…We used v sin i = 4.0 km s −1 because with this value the match between the synthetic and observed spectra was the best. The same rotation speed was determined by Strassmeier et al (1988), Berdyugina (1994), and Montes et al (1994). This value is also close to v sin i = 4.5 km s −1 determined by Gray (1989).…”

Section: Spectrum Synthesessupporting

confidence: 89%

Chemical composition of AY Ceti: A flaring, spotted star with a white dwarf companion

et al. 2011

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Section: Spectrum Synthesessupporting

confidence: 89%

Chemical composition of AY Ceti: A flaring, spotted star with a white dwarf companion

et al. 2011

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“…HD 37847 = TW Lep is a SB2 spectroscopic binary with an orbital period of 28.344 days (Balona 1987) that has been recentely observed by several authors (see, among others, Strassmeier et al 1993a;Fox et al 1994;Cutispoto 1995 and references therein). It was detected by the ROSAT satellite during the all-sky EUV survey (Pye et al 1995).…”

Section: Resultsmentioning

confidence: 97%

“…HD 81410 = IL Hya is an SB1 spectroscopic binary that has been observed by several authors at different wavelenghts (see Strassmeier et al 1993a;Cutispoto 1993, 1995 andreferences therein). More recently, it has been detected by the ROSAT and EUVE satellites (Pye et al 1995;Bowyer et al 1996;Mitrou et al 1997).…”

Section: Resultsmentioning

confidence: 98%

“…For a detailed study of the physical parameters of HD 106225 see Strassmeier (1994). The optical variability has been studied by several authors in recent years (see Strassmeier et al 1997Strassmeier et al , 1993aCutispoto 1996;Hall & Henry 1992 and references therein). The observations presented here were obtained over the 15-30 Mar.…”

Section: Resultsmentioning

confidence: 99%

“…From the v sin i values computed by Randich et al (1993) and by Favata et al (1995) the minimum stellar radius results in the 7.7 − 9.7 R range. The spectral classification of HD 136905 is given as K1 III + [G−K V] by Strassmeier et al (1993a) and as K1 III + F by Bidelman & MacConnell (1973). The two best fits of the observed colors are obtained by assuming K1 III + G5 IV or K1/2 III + G0 IV systems with active components.…”

Section: Resultsmentioning

confidence: 99%

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Long-term monitoring of active stars

Cutispoto

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. In the framework of an extensive program focusing on the global properties and evolution of active stars, high-precision UBV (RI) c photometry of 19 selected stars, collected at the European Southern Observatory over the 15-31 March 1991 interval is presented. Significant evolution of the light curves, period variations and evidence for long-term variability of the global degree of spottedness are found. Most of the spectral classifications are discussed. A flare event was detected for the star HD 127535 = V 841 Cen. These observations contribute to the establishment of a time-extended photometric database which can give important clues on topics such as the stability of spotted areas, differential rotation, solar-like cycles and the correlation between inhomogeneities at different atmospheric levels 1 .

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Spot signatures of a solar‐type dynamo in close binary stars

Holzwarth

2004

Astron Nachr

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Abstract. Magnetic activity signatures in the atmosphere of active stars can be used to place constrains on the underlying processes of flux transport and dynamo operation in its convective envelope. The 'solar paradigm' for magnetic activity suggests that the magnetic field is amplified and stored at the base of the convection zone. Once a critical field strength is exceeded, perturbations initiate the onset of instabilities and the growth of magnetic flux loops, which rise through the convection zone, emerge at the stellar surface, and eventually lead to the formation of starspots and active regions. In close binaries, the proximity of the companion star breaks the rotational symmetry. Although the magnitude of tidal distortions is rather small, non-linear MHD simulations have nevertheless shown in the case of main-sequence binary components that they can cause non-uniform surface distributions of flux tube eruptions. The present work extends the investigation to post-mainsequence components to explore the specific influence of the stellar structure on the surface pattern of erupting flux tubes. In contrast to the case of main-sequence components, where the consistency between simulation results and observations supports the presumption of a solar-like dynamo mechanism, the numerical results here do not recover the starspot properties frequently observed on evolved binary components. This aspect points out an insufficiency of the applied flux tube model and leads to the conclusion that additional flux transport and possibly amplification mechanisms have to be taken into account.

show abstract

The photometric variability of the chromospherically active binary star HD 80715

Cited by 48 publications

References 5 publications

Chemical composition of AY Ceti: A flaring, spotted star with a white dwarf companion

Chemical composition of AY Ceti: A flaring, spotted star with a white dwarf companion

Long-term monitoring of active stars

Spot signatures of a solar‐type dynamo in close binary stars

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