Photometric Monitoring of ROSAT-Selected Weak Line T Tauri Stars

Zhang, Xiaobin; Wei, J. Y.

doi:10.1088/1009-9271/6/6/10

Cited by 6 publications

(2 citation statements)

References 16 publications

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“…They confirmed the periods for four stars and were the first to detect periodicities for six objects. Concurrently, Xing et al (2006) reported the detection of periods for three more stars.…”

Section: Introductionmentioning

confidence: 88%

Magnetically active stars in Taurus-Auriga: Photometric variability and basic physical parameters

Grankin

2013

Astron. Lett.

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The paper presents an analysis of homogeneous long-term photometric observations of 28 well-known weak-line T Tauri stars (WTTS) and 60 WTTS candidates detected by the ROSAT observatory in the direction of the Taurus-Auriga starforming region. 22 known WTTS and 39 WTTS candidates are shown to exhibit periodic light variations that are attributable to the phenomenon of spotted rotational modulation. The rotation periods of these spotted stars lie within the range from 0.5 to 10 days. Significant differences between the long-term photometric behaviors of known WTTS and WTTS candidates have been found. We have calculated accurate luminosities, radii, masses, and ages for 74 stars. About 33% of the sample of WTTS candidates have ages younger than 10 Myr. The mean distance to 24 WTTS candidates with reliable estimates of their radii is shown to be 143 ± 26 pc. This is in excellent agreement with the adopted distance to the Taurus-Auriga star-forming region.

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Section: Introductionmentioning

confidence: 88%

Magnetically active stars in Taurus-Auriga: Photometric variability and basic physical parameters

Grankin

2013

Astron. Lett.

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“…A PI 1024×1024 CCD and Standard Johnson V filter were used. The field of view is 17 ′ × 17 ′ (Xing et al 2006).…”

Section: Observations and The Orbital Periodmentioning

confidence: 99%

The ROSAT bright source 1RXS J201607.0 + 251645: an active Algol-type binary

Yang

et al. 2009

Res. Astron. Astrophys.

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1RXS J201607.0+251645 is identified to be an eclipsing binary. We present the preliminary observations in V band with the 0.6-m telescope for three years and the extensive observations in V and R band with the 0.8-m telescope for six nights, respectively. The light curve of the system is EB type. Five light minimum times were obtained and the orbital period of 0. d 388058(±0. d 00044) is determined. The photometric solution given by the 2003-version Wilson-Devinney program suggests the binary is a semi-detached system with the photometric mass ratio 0.895(±0.006), which probably comprises a G5 primary and an oversize K5 secondary. The less massive component has completely filled its Roche lobe, while the other almost fills its Roche lobe with the filling factor of 93.4%. The system shows a varying O'Connell effect in its phase folded diagrams from 2005 to 2007, and is X-ray luminous with logL X /L bol ∼ −3.27. Possible mechanisms to account for these two phenomena are discussed. Finally, we infer the binary may be in thermal oscillation or may evolve into a contact binary.

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Lithium Abundances From Optical High-Resolution Spectroscopy of Weak-Line T Tauri Stars

Xing

2010

ApJ

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Photometric Monitoring of ROSAT-Selected Weak Line T Tauri Stars

Cited by 6 publications

References 16 publications

Magnetically active stars in Taurus-Auriga: Photometric variability and basic physical parameters

Magnetically active stars in Taurus-Auriga: Photometric variability and basic physical parameters

The ROSAT bright source 1RXS J201607.0 + 251645: an active Algol-type binary

Lithium Abundances From Optical High-Resolution Spectroscopy of Weak-Line T Tauri Stars

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