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Montes, D.; Sanz-Forcada, J.; Fernández-Figueroa, M. J.; Castro, E. de; Cornide, M.; Ramsey, Lawrence W.

doi:10.1023/a:1002199320789

Cited by 165 publications

(332 citation statements)

References 2 publications

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“…Our hypothesis of the broad component being due to microflaring is also supported by the position of V410 Tau in Fig. 21 of Montes et al (1997). The left panel on their figure presents a correlation between the equivalent width of the H α broad component and that of the whole line for stars that show microflaring.…”

Section: The H α Broad Emission Componentsupporting

confidence: 65%

“…These events are thought to be associated with emerging magnetic flux regions where field reconnection occurs. An extensive description of the microflaring activity is given by Montes et al (1997). Our hypothesis of the broad component being due to microflaring is also supported by the position of V410 Tau in Fig.…”

Section: The H α Broad Emission Componentsupporting

confidence: 64%

“…Due to the strong evidence against the presence of circumstellar disk detectable remnant (Beckwith et al 1990), we consider it more likely that the platform or extended wings are due to microflaring. This explanation has been provided by Montes et al (1997Montes et al ( , 1998 for the broad H α component of chromospherically active binary systems and weak-line T Tauri stars, and is supported by its similarity to the broad components found in the chromospheric Mg II h & k lines, as well as in several transition region lines, of active stars. Linsky & Wood (1994) have interpreted the broad component of the transition region lines as the result of microflaring, on the basis of the broad profiles observed in explosive events in the solar transition region.…”

Section: The H α Broad Emission Componentsupporting

confidence: 59%

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The weak-line T Tauri star V410 Tau

Fernández¹,

Stelzer

Henden

et al. 2004

A&A

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Abstract. We show that V410 Tau, a weak-line T Tauri star, is a flaring star. This result comes from an intensive, coordinated monitoring campaign carried out in November 2001 at visible and X-ray wavelength ranges. It is confirmed by previous, isolated observations found in the literature. Flares tend to occur mainly around the star's minimum brightness, when the most active regions face us. We report on the strongest flare detected up to now on this star, for which we have obtained simultaneous visible Strömgren photometry and intermediate resolution spectroscopy. We derive decay times from 3 to 0.7 h at several wavelengths for the continuum in the 3600−5600 Å range. We estimate the energy involved in this and the other flares for which we have good time sampling, and conclude that the strongest event, at least, could have important consequences for the matter in the surroundings of the star. If similar events took place on the young Sun and lasted for several Myr, they could explain the anomalous abundances of elemental isotopes found in some meteorites. They could have also contributed to eliminate part of the primary atmospheres of the planet embryos and would have provided enough energy for the melting of solid iron-magnesium silicates, a process that may explain the presence of chondrules in chondritic meteorites. High resolution spectroscopy of the H α emission line in the quiescent states of V410 Tau enables us to study the variability of the broad component. We suggest that this component is related to microflaring activity, such as the one observed on more evolved, magnetically-active stars. The large velocities and the energy associated with this component support this hypothesis.

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Section: The H α Broad Emission Componentsupporting

confidence: 65%

Section: The H α Broad Emission Componentsupporting

confidence: 64%

Section: The H α Broad Emission Componentsupporting

confidence: 59%

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The weak-line T Tauri star V410 Tau

Fernández¹,

Stelzer

Henden

et al. 2004

A&A

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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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“…Such events may play more prominent roles in stellar atmospheres that have higher levels of magnetic activity than the Sun, or even at other stages of stellar evolution where the activity levels of stars are higher, similar to the levels when they are first formed. Montes & Ramsey (1998) reported the possible detection of a Li I λ 6708 Å line enhancement during an unusual long-duration optical flare in the chromospherically active binary 2RE J0743+224 with a K1 III primary. During the flare, the Li I photospheric line strength gradually increased by about 40%, and the 6 Li/ 7 Li ratio, as measured by the wavelength of the Li I doublet, increased to about 10%.…”

Section: Introductionmentioning

confidence: 99%

A detailed study of lithium in 107 CHEPS dwarf stars

Pavlenko

Jenkins

Ivanyuk

et al. 2018

A&A

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Context. We report results from lithium abundance determinations using high resolution spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire Extrasolar Planet Search programme. Aims. We aim to set out to understand the lithium distribution of the population of stars taken from this survey. Methods. The lithium abundance taking account of non-local thermodynamical equilibrium effects was determined from the fits to the Li I 6708 Å resonance doublet profiles in the observed spectra. Results. We find that a) fast rotators tend to have higher lithium abundances; b) log N(Li) is higher in more massive and hot stars; c) log N(Li) is higher in stars of lower log g; d) stars with the metallicities >0.25 dex do not show the lithium lines in their spectra; e) most of our planet hosts rotate slower; and f) a lower limit of lithium isotopic ratio is 7 Li/ 6 Li > 10 in the atmospheres of two stars with planets (SWP) and two non-SWP stars. Conclusions. Measurable lithium abundances were found in the atmospheres of 45 stars located at distances of 20−170 pc from the Sun, for the other 62 stars the upper limits of log N(Li) were computed. We found well defined dependences of lithium abundances on T eff , V sin i, and less pronounced for the log g. In case of V sin i we see two sequences of stars: with measurable lithium and with the upper limit of log N(Li). About 10% of our targets are known to host planets. Only two SWP have notable lithium abundances, so we found a lower proportion of stars with detectable Li among known planet hosts than among stars without planets. However, given the small sample size of our planet-host sample, our analysis does not show any statistically significant differences in the lithium abundance between SWP and stars without known planets.

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Cited by 165 publications

References 2 publications

The weak-line T Tauri star V410 Tau

The weak-line T Tauri star V410 Tau

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

A detailed study of lithium in 107 CHEPS dwarf stars

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