Rotation-induced lithium depletion of solar-type stars in open
stellar clusters

Tschäpe, R.; Rüdiger, G.

doi:10.1051/0004-6361:20010482

Cited by 22 publications

(16 citation statements)

References 24 publications

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“…The relation confirms the result that was found in previous results (Rebolo & Beckman 1988;Tschäpe & Rüdiger 2001;Xing et al 2007a). A model for lithium depletion with age (Piau & Turck-Chièze 2002) and the relation between age and rotation evolution (Bouvier et al 1997;Xing et al 2007a;etc) indicate that younger objects rotate faster, and that they still retain lithium in their atmospheres.…”

Section: The Relationship Between the Equivalent Width Of LI I And Stsupporting

confidence: 89%

Chromospheric activity in several single late-type stars

Zhang¹,

Pi²,

Zhu³

2015

Res. Astron. Astrophys.

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New high-resolution echelle spectra of six single late-type Pleiades-like stars (V368 Cep, EP Eri, DX Leo, GJ 211, PW And and V383 Lac) were obtained with the 2.16 meter telescope at Xinglong Station in 2008-2010. Using the spectral subtraction technique, we analyzed our spectroscopic data and calculated the equivalent widths of excess emission from several indicators of chromospheric activity (Na I D 1 , D 2 , Hα and Ca II infrared triplet lines). All our results using chromospheric activity indicators confirmed the previous findings. In addition, the maximum amplitudes of chromospheric rotational modulation and the ratio of EW 8542 /EW 8498 were found to rise with increasing v sin i velocity.

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Section: The Relationship Between the Equivalent Width Of LI I And Stsupporting

confidence: 89%

Chromospheric activity in several single late-type stars

Zhang¹,

Pi²,

Zhu³

2015

Res. Astron. Astrophys.

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“…The lithium-rotation relation for ZAMS stars in Pleiades (e.g. Tschäpe & Rüdiger, 2001) and young low-mass man sequence stars (e.g. Rebolo & Beckman, 1988;Chaboyer, 1998) has long been known.…”

Section: B2 Li-rotation For Young Solar Type Starsmentioning

confidence: 99%

“…Rebolo & Beckman, 1988;Chaboyer, 1998) has long been known. In "older" clusters (Pleiades, Hyades) the faster rotating stars show less the Li depletion (Tschäpe & Rüdiger, 2001). In order to compare the possible effect of rotation upon lithium depletion between young solar-type main sequence stars and PMS, we take the P rot and EW(Li) for 7 ZAMS stars (Krishnamurthi et al, 19980;Soderblom et al, 1993;Messina, 2001) in the Pleiades cluster and 12 young low-mass main sequence stars (Rebolo & Beckman, 1988) in the Hyades cluster, and plotted the EW(Li) versus P rot of these stars with WTTSs in our sample in Fig.…”

Section: B2 Li-rotation For Young Solar Type Starsmentioning

confidence: 99%

The lithium-rotation correlation for WTTS in Taurus–Auriga

Shi

Wei

2007

New Astronomy

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Surface lithium abundance and rotation velocity can serve as powerful and mutually complementary diagnostics of interior structure of stars. So far, the processes responsible for the lithium depletion during pre-main sequence evolution are still poorly understood. We investigate whether a correlation exists between equivalent widths of Li (EW(Li)) and rotation period (P rot ) for Weak-line T Tauri stars (WTTSs). We find that rapidly rotating stars have lower EW(Li) and the fast burning of Li begins at the phase when star's P rot evolves towards 3 days among 0.9M ⊙ to 1.4M ⊙ WTTSs in Taurus-Auriga. Our results support the conclusion by Piau & Turch-Chiéze about a model for lithium depletion with age of the star and by Bouvier et al. in relation to rotation evolution. The turn over of the curve for the correlation between EW(Li) and P rot is at the phase of Zero-Age Main Sequence (ZAMS). The EW(Li) decreases with decreasing P rot before the star reaches the ZAMS, while it decreases with increasing P rot (decreasing rotation velocity) for young low-mass main sequence stars. This result could be explained as an age effect of Li depletion and the rapid rotation does not inhibit Li destruction among low mass PMS stars.

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“…Nevertheless, Pleiades UFRs of a single mass can show a range in surface rotation of a factor of 20 or more (Soderblom et al 1993b). Recent correlative analysis suggests a rotation-induced lithium depletion for the Pleiades stars but not for younger clusters like α Per (Tschäpe & Rüdiger 2001), which is another intriguing question awaiting answer.…”

Section: Surface Imaging Of Solar-type Stars In Open Clustersmentioning

confidence: 98%

Doppler imaging of stellar surface structure

Rice

Strassmeier

2001

A&A

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Abstract. We present the first Doppler image of a solar-type G dwarf in the Pleiades open cluster. As such, the star represents the Sun at an age of approximately 100 Myr and could be an important target for further progress in magnetic-braking and angular-momentum-transport theories. Our image reconstructions were done from a full spectrum inversion with a total of 38 spectral lines but we also present single-line inversions using the prominent Li i 6707-Å line and the nearby Ca i 6717-Å line. The maps reveal cool spots at or near the pole and within the equatorial regions, in contradiction to our predictions from flux-tube modelling that only medium-latitude spots should be seen. The maps also show several warm spots near the equatorial regions but their reality needs to be confirmed. A polar spot is recovered but likely consists of several smaller spots at very high latitudes touching the visible pole instead of a big cap-like spot as seen on some RS CVn binaries.Key words. stars: activity -starspots -stars: imaging -stars: individual: HII 314 -stars: late-type Surface imaging of solar-type stars in open clustersMagnetic braking of stellar rotation due to a stellar wind along predominantly equatorial magnetic field lines, as worked for our Sun, seems unable in every case to be effective in slowing down stars from their initial angular momentum gained during the contraction of the prestellar cloud. The ultra-fast rotators (UFRs) in the young open clusters α Per (age ≈50 Myr) and Pleiades (age ≈100 Myr) as well as the young field stars AB Dor, LQ Hya, EK Dra are the most cited examples. Their simple existence is something of a problem since magnetic braking of a solar-mass star should have had, by the age of these stars, enough time during pre-main-sequence evolution to halt the rapid rotation. Accretion disks in the early pre-main sequence stages certainly play an important and maybe dominant role in explaining the angular momentum loss of very young objects but cannot easily be incorporated into an explanation of the existence of several hundreds of cluster-ZAMS stars that are not in a close binary but still rapidly rotating (Stauffer et al. 1984;Soderblom et al. 1993b;O'Dell et al. 1995;Barnes & Sofia 1996; and others).What process then might allow these stars to maintain their angular momentum? The currently favored hypothesis is the onset of a dynamo saturation, i.e. a saturation of the atmospheric (coronal) volume with magnetic fields (Vilhu 1984;Keppens et al. 1995) so that there is no torque arm for magnetic braking via a stellar wind. For further reading we refer to Mestel (1999). Solanki et al. (1997) and Buzasi (1997) -and later Strassmeier et al. (1998 for post-main-sequence evolution -have suggested an alternative explanation to dynamo saturation in that magnetic fields concentrated in polar starspots could be the reason for the lack of angular momentum loss. Solanki et al. (1997) presented numerical simulations that show that the effect of polar magnetic fields in the evolution of stellar rotatio...

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Rotation-induced lithium depletion of solar-type stars in open stellar clusters

Cited by 22 publications

References 24 publications

Chromospheric activity in several single late-type stars

Chromospheric activity in several single late-type stars

The lithium-rotation correlation for WTTS in Taurus–Auriga

Doppler imaging of stellar surface structure

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