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Гранкин, В. П.; Aleshin, S. V.

doi:10.1023/a:1021517315190

Cited by 3 publications

(4 citation statements)

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“…Table .1 Rotational periods and stellar properties for 21 WTTSs. Reference to table 1: X&L: Xing et al (2006) and Li & Hu (1998); X&W: Xing et al (2006) and Wichmann et al (2000); X&Wa: Xing et al (2006) and Walter (1986); X&G: Xing et al (2006) and Gregorio-Hetermet & Hetem (2002); B: Bouvier et al (1993); G&W: Grankin (1996) and Walter et al (1988); B&W: Bouvier et al (1997) and Wichmann et al (2000). The mass of stars are taken directly from above literature or from comparison with evolutionary tracks of Cohen & Kuhi (1979).…”

Section: Discussionmentioning

confidence: 99%

“…Five objects have been taken from their sample. • Grankin (1993) presented the results of BVR photometry of 22 WTTSs.…”

Section: A1 Rotation Periodsmentioning

confidence: 99%

“…They presented a detailed study for Li-rich stars discovered by ROSAT in Taurus-Auriga SFRs, the results are based on high-resolution echelle spectra. • The Li I equivalent widths of theGrankin (1993) sample and the star NTTS045251+3016 fromXing et al (2006) were taken from the list ofWalter et al (1988), measured from high-dispersion spectra. • Two stars of theXing et al (2006) sample, [LH98]37 and [LH98]53, were identified as WTTSs by…”

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confidence: 99%

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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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Section: Discussionmentioning

confidence: 99%

“…Five objects have been taken from their sample. • Grankin (1993) presented the results of BVR photometry of 22 WTTSs.…”

Section: A1 Rotation Periodsmentioning

confidence: 99%

mentioning

confidence: 99%

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The lithium-rotation correlation for WTTS in Taurus–Auriga

Shi

Wei

2007

New Astronomy

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“…Photometric observations on these X-ray sources revealed a total number of 22 WTTSs or WTTS candidates (O'Neal et al 1990, Gregorio-Hetem & Hetem 1992, Wichmann et al 1996, Li & Hu 1998. Rotational periods of 3 definite WTTSs were determined by Zakinov et al (1993), Grankin (1994) and Bouvier et al (1997), respectively. One of them was found to be a short-period variable.…”

Section: Introductionmentioning

confidence: 99%

Photometric Monitoring of ROSAT-Selected Weak Line T Tauri Stars

Zhang

Wei

2006

Chin. J. Astron. Astrophys.

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We monitored the light variations of 22 weak-line T Tauri stars (WTTS) discovered among the X-ray sources in the field of the Taurus-Auriga cloud. The photometric variability of 12 out of these WTTS samples is confirmed. They are all proved to be in periodic variations. By using the methods of the Phase Dispersion Minimization (PDM) and Fourier analysis, the rotational periods of these stars were determined based on this observation. Most of them are found to be shorter than one day. This gives further evidences for the spin up of solar-type stars as predicted by models of angular momentum evolution of pre-main sequence stars.

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Recent Development of Gas–Solid Phase Chemiluminescence

Zhang

Lin

2017

J. Anal. Test.

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other luminescent organisms in the environment have been found, CL has aroused considerable interest for deeper research and application [2]. Definitely, CL analysis has excellent advantages including high sensitivity, low background interference, highly responsive signals, safe operation process and portable equipment [3], which has been applied to detection towards the concentration of catalyst, reactant, CL inhibitor and enhancer [4] Among numerous branches of CL systems, acting as a classic and interesting strategy, gas-solid phase CL has recently been a rapidly growing area. Such CL evolves in infrared, visible, and even in ultraviolet regions through chemical reactions between gas and solid reactants on the surface of solid matter. It acts as an indicator and monitor of gas-solid phase reactions to provide information during the process of reaction [10]. Moreover, this strategy also enables investigations of gas-solid phase reactions through sensitive and simple spectral method [11]. In addition, application of gas-solid phase CL has extended to gas-phase and solid-phase diagnose and detection due to its strong intensity of signals and unique property. Over decades of years of investigation and development, gas-solid phase CL has become an effective detection method in analytical chemistry. Recent progress mainly focuses on development of new gas-solid phase CL systems and their practical applications, while many interesting results have been reported. Obviously, the excellent sensitivity and intensity of gas-solid phase CL has made it a good candidate as a novel CL technology, which has revealed great potential for future analysis and test.Considering the aforementioned properties, gas-solid phase CL have received considerable attentions in different areas of Abstract Serving as a classic and interesting strategy, gassolid phase chemiluminescence (CL) has recently been a rapidly growing area where CL is emitted through chemical reactions between gas and solid reactants occurred on the surface of solid matter. This CL system provided a sensitive and simple spectral method for investigating gas-solid phase reactions while information on the rate constants, intermediate productions, surface states and reaction mechanisms of interaction could be acquired. Recent progresses mainly concentrate on development of new gas-solid phase CL systems and their practical applications. This review paper summarized main classifications, mechanisms and applications of gas-solid phase CL. The future prospects for gas-solid phase CL are discussed.

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Cited by 3 publications

References 3 publications

The lithium-rotation correlation for WTTS in Taurus–Auriga

The lithium-rotation correlation for WTTS in Taurus–Auriga

Photometric Monitoring of ROSAT-Selected Weak Line T Tauri Stars

Recent Development of Gas–Solid Phase Chemiluminescence

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