Non Coeval Young Multiple Systems?

Duchêne, Gaspard; Ghez, A. M.; McCabe, C.

doi:10.1007/1-4020-2600-5_27

Cited by 2 publications

(2 citation statements)

References 21 publications

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“…However, the radio flux of V773 Tau declined while its X-ray emission remained steady, whereas the opposite behavior is observed in DoAr 21. The interpretation of the behavior of V773 Tau is now complicated by the discovery that it is a quadruple system consisting of a K2 V + K5 V spectroscopic binary with a nearby M dwarf at 0B12 (Ghez et al 1995) and an IR companion 0B21 away ( Duchene et al 2001). ROSAT could not spatially resolve these four components, raising the obvious question of whether the (variable) radio emission and (steady) X-ray emission originated in the same star.…”

Section: Time-resolvv Ed X-ray Spectroscopy Of a Largg E Flare On Doamentioning

confidence: 99%

SimultaneousChandraand Very Large Array Observations of Young Stars and Protostars in ρ Ophiuchus Cloud Core A

Gagné

Skinner

Daniel

2004

ApJ

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A 96 ks Chandra X-ray observation of Ophiuchus cloud core A detected 87 sources, of which 60 were identified with counterparts at other wavelengths. The X-ray detections include 12 of 14 known classical T Tauri stars (CTTSs) in the field, 15 of 17 known weak-lined TTSs ( WTTSs), and 4 of 15 brown dwarf candidates. The X-ray detections are characterized by hard, heavily absorbed emission. Most X-ray detections have visual extinctions in the range A V % 10 20 mag, but several sources with visual absorptions as high as A V % 40 56 mag were detected. The mean photon energy of a typical source is hEi % 3 keV, and more than half of the detections are variable. Prominent X-ray flares were detected in the unusual close binary system Oph S1, the X-ray-bright WTTS DoAr 21, and the brown dwarf candidate GY 31 ( M5.5). Time-resolved spectroscopic analysis of the DoAr 21 flare clearly reveals a sequence of secondary flares during the decay phase that may have reheated the plasma. We find that the X-ray luminosity distributions and spectral hardnesses of CTTSs and WTTSs are similar. We also conclude that the X-ray emission of detected brown dwarf candidates is less luminous than TTSs, but spectroscopically similar. Simultaneous multifrequency Very Large Array ( VLA) observations detected 31 radio sources at 6 cm, of which 10 were also detected by Chandra. We report new radio detections of the optically invisible IR source WLY 2-11 and the faint H emission line star Elias 24 (class II ). We confirm circular polarization in Oph S1 and report a new detection of circular polarization in DoAr 21. We find no evidence that X-ray and radio luminosities are correlated in the small sample of TTSs detected simultaneously with Chandra and the VLA. We describe a new nonparametric method for estimating X-ray spectral properties from unbinned photon event lists that is applicable to both faint and bright X-ray sources. The method is used to generate f X , log T , and L X light curves. In addition, we provide a publicly available electronic database containing multiwavelength data for 345 known X-ray, IR, and radio sources in the core A region.

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Section: Time-resolvv Ed X-ray Spectroscopy Of a Largg E Flare On Doamentioning

confidence: 99%

SimultaneousChandraand Very Large Array Observations of Young Stars and Protostars in ρ Ophiuchus Cloud Core A

Gagné

Skinner

Daniel

2004

ApJ

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“…Welty (1995) has shown that the main component, V 773 Tau A, is itself a spectroscopic binary with an orbital period of 51 days. Duchêne et al (2001) have briefly announced the possible presence of a fourth close component in the V 773 Tau system. In this paper astrometric and photometric properties of this object are given, and its physical membership to V 773 Tau is confirmed from its orbital motion.…”

Section: Introductionmentioning

confidence: 99%

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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Non Coeval Young Multiple Systems?

Cited by 2 publications

References 21 publications

SimultaneousChandraand Very Large Array Observations of Young Stars and Protostars in ρ Ophiuchus Cloud Core A

SimultaneousChandraand Very Large Array Observations of Young Stars and Protostars in ρ Ophiuchus Cloud Core A

A fourth component in the young multiple system V 773 Tauri

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