Ejection of a Low-Mass Star in a Young Stellar System in Taurus

Loinard, Laurent; Rodrı́guez, Luis F.; Rodríguez, Mónica

doi:10.1086/375157

Cited by 38 publications

(61 citation statements)

References 33 publications

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“…It could be argued that the existence of this extended halo of radio emission might affect the astrometries reported by Johnston et al (2003) and Loinard et al (2003). A detailed analysis of this issue will be presented in a forthcoming article.…”

Section: Discussionmentioning

confidence: 93%

“…A detailed analysis of this issue will be presented in a forthcoming article. Here we merely mention (1) that the existence of this structure may indeed explain some of the discrepancies between radio (particularly at the longest wavelengths) and infrared data noted by various authors and (2) that the effect on the 2 cm data used by Johnston et al (2003) and Loinard et al (2003) appears to be limited, thanks first to the positive spectral index of the compact component compared to the flat energy distribution of the extended one; and second to the better resolution and more effective spatial filtering at 2 cm than at 3.6 cm.…”

Section: Discussionmentioning

confidence: 96%

“…According to Loinard et al (2003), the compact radio source directly associated with T Tau Sb has accelerated westward to about 20 km s À1 , starting around 1996, after being on a relatively slow (5Y10 km s À1 ) elliptical orbit from 1983 to 1995. That both the offset from the compact source to the center of the extended component and the morphology of this extended component have changed just when this acceleration occurred is unlikely to be a coincidence.…”

Section: Discussion Of the Extended Component In T Tau Srmentioning

confidence: 99%

“…While the northern radio source corresponds to the optical star T Tau, the southern component is clearly associated with the infrared companion. Detailed comparisons between radio and infrared data obtained almost simultaneously in late 2000/early 2001 suggest that it is associated with T Tau Sb ( Loinard et al 2003;Johnston et al 2003). However, the exact relation between the infrared sources and the radio emission remains disputed.…”

Section: Radio Observationsmentioning

confidence: 99%

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On the Nature of the Extended Radio Emission Surrounding T Tauri South

Loinard¹,

Rodrı́guez²,

D’Alessio³

et al. 2007

ApJ

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At centimeter wavelengths, the young stellar system T Tauri is known to be composed of two sources, the northern one associated with the optical star T Tau itself, and the southern one related to the infrared companion T Tau S. Here we reexamine the origin of the radio emission from these two components using archival 2 cm, 3.6 cm, and 6 cm VLA observations. The emission from the northern member is confirmed to be largely dominated by free-free radiation from an ionized wind, while the southern radio source is confirmed to consist of a compact component of magnetic origin, surrounded by an extended halo. Only moderately variable, the extended structure associated with the southern source is most likely the result of free-free radiation related to stellar winds. However, its flat spectral energy distribution, its extent, and the lack of variation of its size with the frequency of observation are incompatible with the classical picture of a fully ionized wind with constant velocity and mass-loss rate leading to an electron density distribution of n e (r) / r À2 . Instead, we propose a model in which the ionization results from the impact of a supersonic wind driven by T Tau Sb onto dense surrounding material, possibly associated with the circumbinary disk recently identified around the T Tau Sa /T Tau Sb pair. The timescales for cooling and recombination in such a situation are in good agreement with the observed morphological changes undergone by the extended structure as its driving source moves through the environment.

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Section: Discussionmentioning

confidence: 93%

Section: Discussionmentioning

confidence: 96%

Section: Discussion Of the Extended Component In T Tau Srmentioning

confidence: 99%

Section: Radio Observationsmentioning

confidence: 99%

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On the Nature of the Extended Radio Emission Surrounding T Tauri South

Loinard¹,

Rodrı́guez²,

D’Alessio³

et al. 2007

ApJ

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“…While it has been suggested that this system may be on an unbound orbit (Loinard et al 2003), other studies have found possible closed orbits and derived a total mass of 2−6 M for T Tau S (Johnston et al 2003;Beck et al 2004). Using a refined method, Johnston et al (2004a,b) attempted for the first time to determine the individual masses of T Tau Sa and Sb.…”

Section: Introductionmentioning

confidence: 99%

Accurate stellar masses in the multiple system T Tauri

Duchêne¹,

Beust²,

Adjali³

et al. 2006

A&A

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Aims. We obtain accurate estimates for the individual masses of the components of the tight binary system T Tau S to settle the ongoing debate on the nature of T Tau Sa, a so-called infrared companion. Methods. We take advantage of the fact that T Tau S belongs to a triple system composed of two hierarchical orbits to simultaneously analyze the motion of T Tau Sb in the rest frames of T Tau Sa and T Tau N. With this method, it is possible to pinpoint the location of the center of mass of T Tau S and, thereby, to determine individual masses for T Tau Sa and T Tau Sb with no prior assumption about the mass/flux ratio of the system. This improvement over previous studies of the system results in much better constraints on orbital parameters. Results. We find individual masses of 2.73 ± 0.31 M for T Tau Sa and of 0.61 ± 0.17 M for T Tau Sb (in agreement with its early-M spectral type), including the uncertainty on the distance to the system. These are among the most precise estimates of the mass of any Pre-Main Sequence star, a remarkable result since this is the first system in which individual masses of T Tauri stars can be determined from astrometry only. This model-independent analysis confirms that T Tau Sa is an intermediate-mass star, presumably a very young Herbig Ae star, that may possess an almost edge-on disk.

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