Tidal stripping and disk kinematics in the RW Aurigae
 system

Cabrit, S.; Pety, J.; Pesenti, N.; Dougados, C.

doi:10.1051/0004-6361:20054047

Cited by 133 publications

(241 citation statements)

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“…This star underwent a deep extinction in 2011 and has remained in this state, while the accretion rate has not changed by much (Bouvier et al 2013). Unlike AA Tau, the disk of RW Aur A is inclined by between 45 to 60 degrees as estimated in Cabrit et al (2006). We note that a few other weak-line TTS have shown longer eclipses by foreground dust (see e.g.…”

Section: Introductionmentioning

confidence: 61%

“…They attributed this drop to an occultation by part of a tidally disrupted disk as evidenced in Cabrit et al (2006) and noted that such a long-lasting event had not been observed before. Chou et al (2013) collected high-resolution spectra during the beginning of the minimum indicating that no significant changes in the emission line spectrum had occurred.…”

Section: Introductionmentioning

confidence: 91%

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Another deep dimming of the classical T Tauri star RW Aurigae A

Петров¹,

Gahm²,

Djupvik³

et al. 2015

A&A

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Context. RW Aur A is a classical T Tauri star (CTTS) with an unusually rich emission line spectrum. In 2014 the star faded by ∼3 mag in the V band and went into a long-lasting minimum. In 2010 the star underwent a similar fading, although less pronounced. These events in RW Aur A are very unusual among the CTTS, and have been attributed to occultations by passing dust clouds. Aims. We want to find out if any spectral changes took place after the last fading of RW Aur A with the intention of gathering more information on the occulting body and the cause of the phenomenon. Methods. We collected spectra of the two components of RW Aur. The photometry was performed before and during the minimum. Results. The overall spectral signatures reflecting emission from accretion flows from disk to star did not change after the fading. However, blue-shifted absorption components related to the stellar wind increased in strength in certain resonance lines, and the profiles and strengths but not the fluxes of forbidden lines became drastically different. Conclusions. The extinction through the obscuring cloud is grey indicating the presence of large dust grains. At the same time, there are no traces of related absorbing gas. The cloud occults the star and the interior part of the stellar wind, but not the wind or jet further out. The dimming in 2014 was not accompanied by changes in the accretion flows at the stellar surface. There is evidence that the structure and velocity pattern of the stellar wind did change significantly. The dimmings could be related to passing condensations in a tidally disrupted disk, as proposed earlier, but we also speculate that large dust grains have been stirred up from the inclined disk into the line of sight through the interaction with an enhanced wind.

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Section: Introductionmentioning

confidence: 61%

Section: Introductionmentioning

confidence: 91%

Another deep dimming of the classical T Tauri star RW Aurigae A

Петров¹,

Gahm²,

Djupvik³

et al. 2015

A&A

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“…RW Aur is a binary system that was imaged in 12 CO by Cabrit et al (2006), who find evidence for a very small (50 AU radius) disk, but did not detect 13 CO emission. Our negative result is consistent with their findings.…”

Section: Discussionmentioning

confidence: 99%

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

Guilloteau¹,

Folco²,

Dutrey³

et al. 2013

A&A

108

151

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Aims. We investigate the suitability of several molecular tracers, in particular CN N = 2−1 line emission, as a confusion-free probe of the kinematics of circumstellar disks. Methods. We use the IRAM 30-m telescope to perform a sensitive search for CN N = 2−1 in 42 T Tauri or Herbig Ae systems located principally in the Taurus-Auriga region. 13 CO J = 2−1 is observed simultaneously to provide an indication of the level of confusion with the surrounding molecular cloud. The bandpass also contains two transitions of ortho-H 2 CO, one of SO and the C 17 O J = 2−1 line which provide complementary information on the nature of the emission. Results. While 13 CO is in general dominated by residual emission from the cloud, CN exhibits a high disk detection rate >50% in our sample. We even report CN detection in stars for which interferometric searches failed to detect 12 CO, presumably because of obscuration by a foreground, optically thick, cloud. Comparison between CN and o-H 2 CO or SO line profiles and intensities divide the sample in two main categories. Sources with SO emission are bright and have strong H 2 CO emission, leading in general to [H 2 CO/CN] > 0.5. Furthermore, their line profiles, combined with a priori information on the objects, suggest that the emission is coming from outflows or envelopes rather than from a circumstellar disk. On the other hand, most sources have [H 2 CO/CN] < 0.3, no SO emission, and some of them exhibit clear double-peaked profiles characteristics of rotating disks. In this second category, CN is likely tracing the proto-planetary disks. From the line flux and opacity derived from the hyperfine ratios, we constrain the outer radii of the disks, which range from 300 to 600 AU. The overall gas disk detection rate (including all molecular tracers) is ∼68%, and decreases for fainter continuum sources. Conclusions. The current study demonstrates that gas disks, like dust disks, are ubiquitous around young PMS stars in regions of isolated star formation, and that a large fraction of them have R out > ∼ 300 AU. It also shows the potential of the CN N = 2−1 transition to probe the kinematics of these disks, thereby measuring the stellar mass, using high resolution observations with ALMA.

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“…The jet rotation sense traced in near ultra-violet (NUV) emission lines at higher flow velocities is coherent for DG Tau, but these emission lines are below the detection threshold for CW Tau (Coffey et al 2007). In RW Aur, the optical jet and disk rotations appear opposite (see Coffey et al 2004;Cabrit et al 2006). Here, jet rotation traced in the NUV was found to be compatible with the disk rotation sense (i.e., opposite to the optical jet rotation), but could only be measured in one lobe and at one of the two epochs (spaced by six months; see Coffey et al 2012); because of its complexity and variability the authors declared RW Aur as unsuitable for jet rotation studies.…”

Section: Introductionmentioning

confidence: 99%

ALMA observations of the Th 28 protostellar disk

Louvet

Dougados

Cabrit

et al. 2016

A&A

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Aims. Recently, differences in Doppler shifts across the base of four close classical T Tauri star jets have been detected with the HST in optical and near-ultraviolet (NUV) emission lines, and these Doppler shifts were interpreted as rotation signatures under the assumption of steady state flow. To support this interpretation, it is necessary that the underlying disks rotate in the same sense. Agreement between disk rotation and jet rotation determined from optical lines has been verified in two cases and rejected in one case. Meanwhile, the near-ultraviolet lines, which may trace faster and more collimated inner spines of the jet than optical lines, either agree or show no clear indication. We propose to perform this test on the fourth system, Th 28. Methods. We present ALMA high angular resolution Band 7 continuum, 12 CO(3−2) and 13 CO(2−1) observations of the circumstellar disk around the T Tauri star Th 28. Results. The sub-arcsecond angular resolution (0.46 × 0.37 ) and high sensitivity reached enable us to detect, in CO and continuum, clear signatures of a disk in Keplerian rotation around Th 28. The 12 CO emission is clearly resolved, allowing us to derive estimates of disk position angle and inclination. The large velocity separation of the peaks in 12 CO, combined with the resolved extent of the emission, indicate a central stellar mass in the range 1−2 M . The rotation sense of the disk is well detected in both 13 CO and 12 CO emission lines, and this direction is opposite to that implied by the transverse Doppler shifts measured in the optical lines of the jet. Conclusions. The Th 28 system is now the second system, among the four investigated so far, where counter-rotation between the disk and the optical jet is detected. These findings imply either that optical transverse velocity gradients detected with HST do not trace jet rotation or that modeling the flow with the steady assumption is not valid. In both cases jet rotation studies that rely solely on optical lines are not suitable to derive the launching radius of the jet.

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Tidal stripping and disk kinematics in the RW Aurigae system

Cited by 133 publications

References 40 publications

Another deep dimming of the classical T Tauri star RW Aurigae A

Another deep dimming of the classical T Tauri star RW Aurigae A

A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars

ALMA observations of the Th 28 protostellar disk

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Tidal stripping and disk kinematics in the RW Aurigae system

Cited by 133 publications

References 40 publications

Another deep dimming of the classical T Tauri star RW Aurigae A

Another deep dimming of the classical T Tauri star RW Aurigae A

A sensitive survey for13CO, CN, H2CO, and SO in the disks of T Tauri and Herbig Ae stars

ALMA observations of the Th 28 protostellar disk

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Product

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A sensitive survey for¹³CO, CN, H₂CO, and SO in the disks of T Tauri and Herbig Ae stars