Preliminary Orbits and System Masses for Five Binary T Tauri Stars

Tamazian, V. S.; Docobo, J. A.; White, R. J.; Woitas, J.

doi:10.1086/342621

Cited by 41 publications

(57 citation statements)

References 42 publications

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“…This has probably not a large influence on the general picture. V 773 Tau C will be resolved already at f ≤ 35 pixel, and the relative position of V 773 Tau B matches well the orbital fit by Tamazian et al (2002) and thus seems reliable. For spatial frequencies f > 35 pixel the signal is however affected by an unknown bias.…”

Section: Observations and Data Analysissupporting

confidence: 75%

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A fourth component in the young multiple system V 773 Tauri

Woitas

2003

A&A

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Abstract. I report on a new component in the pre-main sequence multiple system V 773 Tauri. This second visual companion, V 773 Tau C, with a projected separation of ≈0. 2 has been detected using speckle interferometry in the near-infrared. Repeated observations from 1996 to 2002 show significant orbital motion and thus confirm the character of the new companion as a gravitationally bound star. Together with the two components of the spectroscopic binary V 773 Tau A and the previously known visual companion V 773 Tau B, the V 773 Tau system appears as a young "mini-cluster" of four T Tauri stars within a sphere of a radius less than 100 AU. V 773 Tau A, B and C form a triple system that is not hierarchic, but is apparently stable despite of this. The brightness of V 773 Tau C has probably increased over the last years, which may explain its non-detection in previous binary surveys.

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Section: Observations and Data Analysissupporting

confidence: 75%

“…15 using speckle interferometry in the K-band. Since this companion, hereafter named V 773 Tau B, was close to its periastron at the time of detection, Tamazian et al (2002) could derive a first orbital solution based on 9 data points that cover ≈160…”

Section: Introductionmentioning

confidence: 99%

A fourth component in the young multiple system V 773 Tauri

Woitas

2003

A&A

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“…For instance, infrared observations of pre-main-sequence binaries allow unique probes of the evolution of binary fraction (e.g., Ghez et al, 1993) as well as important measurements of masses of young stellar objects (Tamazian et al, 2002). I expect interferometer observations to play an increasingly important role in this area as the sensitivity increases.…”

Section: 15mentioning

confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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“…The close pair in Elias 12 was also observed with adaptive optics on the Keck II telescope. Thiébaut et al (1995) and Tamazian et al (2002) estimated the orbital parameters for DF Tau. We performed preliminary orbital calculations for DF Tau and ZZ Tau and found that we have not yet observed enough of an orbit for these systems to determine the orbital parameters precisely.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Masses of Young Stars in Multiple Systems

et al. 2003

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We present recent measurements of the orbital motion in the young binaries DF Tau and ZZ Tau and the hierarchical triple Elias 12 that were obtained with the Fine Guidance Sensors on the Hubble Space Telescope and at the Keck Observatory using adaptive optics. Combining these observations with previous measurements from the literature, we compute preliminary orbital parameters for DF Tau and ZZ Tau. We find that the orbital elements cannot yet be determined precisely because the orbital coverage spans only $90 in position angle. Nonetheless, the range of possible values for the period and semimajor axis already defines a useful estimate for the total mass in DF Tau

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Preliminary Orbits and System Masses for Five Binary T Tauri Stars

Cited by 41 publications

References 42 publications

A fourth component in the young multiple system V 773 Tauri

A fourth component in the young multiple system V 773 Tauri

Optical interferometry in astronomy

Dynamical Masses of Young Stars in Multiple Systems

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