Observations of suspected low-mass post-T Tauri stars and their evolutionary status

Mundt, R.; Walter, Frederick M.; Feigelson, E. D.; Finkenzeller, U.; Herbig, G. H.; Odell, A. P.

doi:10.1086/161033

Cited by 76 publications

(30 citation statements)

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“…Intense line variability is evident in our data for this source, with a strong accretion outburst observed on 2009 Oct 31 (Figure 6). In the absence of the original spectra from Mundt et al (1983), it is unclear whether the low EW epochs are the consequence of line self absorption or an actual pause in the accretion flow on the central star. In any event, the detection of He I emission lines unambigously establishes this object as accreting in our survey.…”

Section: Accretion Statusmentioning

confidence: 99%

A search for passive protoplanetary discs in the Taurus–Auriga star-forming region

Duchêne

Becker

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We conducted a 12-month monitoring campaign of 33 T Tauri stars (TTS) in Taurus. Our goal was to monitor objects that possess a disk but have a weak Hα line, a common accretion tracer for young stars, to determine whether they host a passive circumstellar disk. We used medium-resolution optical spectroscopy to assess the objects' accretion status and to measure the Hα line. We found no convincing example of passive disks; only transition disk and debris disk systems in our sample are non-accreting. Among accretors, we find no example of flickering accretion, leading to an upper limit of 2.2% on the duty cycle of accretion gaps assuming that all accreting TTS experience such events. Combining literature results with our observations, we find that the reliability of traditional Hα-based criteria to test for accretion is high but imperfect, particularly for low-mass TTS. We find a significant correlation between stellar mass and the full width at 10 per cent of the peak (W 10% ) of the Hα line that does not seem to be related to variations in free-fall velocity. Finally, our data reveal a positive correlation between the Hα equivalent width and its W 10% , indicative of a systematic modulation in the line profile whereby the high-velocity wings of the line are proportionally more enhanced than its core when the line luminosity increases. We argue that this supports the hypothesis that the mass accretion rate on the central star is correlated with the Hα W 10% through a common physical mechanism.

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Section: Accretion Statusmentioning

confidence: 99%

A search for passive protoplanetary discs in the Taurus–Auriga star-forming region

Duchêne

Becker

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The quiescent X-ray luminosity derived for HD 560 B is comparable to that of the PTTS candidates observed by EINSTEIN (ref. 12,25). The X-ray luminosity of all these sources is ~ 1030 erg s " 1, i.e.…”

Section: Discussionmentioning

confidence: 97%

A giant X-ray flare from a B9 + Post-T Tauri system detected by EXOSAT

Tagliaferri

Giommi

Angelini

et al. 1989

International Astronomical Union Colloquium

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We report the serendipitous discovery by EXOSAT of a flaring X-ray source in the field of the Seyfert type I galaxy III ZW 2. We identify this source with the visual binary HD 560 (B9V + G5Ve) and argue that virtually all of the observed X-ray flux, including the flare, came from its late-type component (HD 560 B). Optical studies have lead to the identification of HD 560 B as a post-T Tauri star. Since these stars are difficult to detect by optical methods, X-ray observations may prove to be the best way to identify them.

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“…This result is particularly interesting, because the frequency is identical to that of the solar-type field stars (Duquennoy 8 H. Zinnecker & Mayor 1991) and also because the stars were mainly X-ray selected. The discovery of the first double-lined pre-Main Sequence stars, the X-ray selected T Tauri stars V826 in Taurus (Mundt et al 1983) and Parenago 1540 in Orion (Marschall & Mathieu 1988), preceded the above survey.…”

Section: Studies Of Young Binariesmentioning

confidence: 97%

Binary Stars: Historical Milestones

Zinnecker

2001

Symp. - Int. Astron. Union

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Abstract. This is a brief historical review of the discovery of binary stars, starting in the 18th and 19th century with the work of W. Herschel, W. Struve, and their famous sons. I describe how Ch. Doppler in 1842 found the Doppler effect in connection with the colours of double stars. I also describe how the observation of the stationary Calcium Hand K lines in the spectrum of the spectroscopic binary 6 Ori led to the discovery of the interstellar medium by J. Hartmann in 1904 with the Potsdam refractor. Some steps in the discovery of young binary stars are recounted, starting with the paper of Joy and van Biesbroeck in 1944. The history of ideas regarding the origin of binary systems is also briefly reviewed, beginning with J. Michell's statistical argument in 1767 that many close visual pairs of stars must indeed form physical systems, and W. Herschel's definition of a binary star as "a real double star -the union of two stars that are formed together in one system, by the laws of attraction" .

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Observations of suspected low-mass post-T Tauri stars and their evolutionary status

Cited by 76 publications

References 0 publications

A search for passive protoplanetary discs in the Taurus–Auriga star-forming region

A search for passive protoplanetary discs in the Taurus–Auriga star-forming region

A giant X-ray flare from a B9 + Post-T Tauri system detected by EXOSAT

Binary Stars: Historical Milestones

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