THE PHOTOEVAPORATIVE WIND FROM THE DISK OF TW Hya

Pascucci, Ilaria; Sterzik, M.; Alexander, R. D.; Alencar, S. H. P.; Gorti, Uma; Hollenbach, D. J.; Owen, James E.; Ercolano, Barbara; Edwards, Suzan

doi:10.1088/0004-637x/736/1/13

Cited by 95 publications

(135 citation statements)

References 68 publications

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“…This is not surprising given TW Hya near face-on inclination and the fact that the [OI]6300 line is emitted from the very inner regions of the disc wind , where the underlying disc is devoid of dust, allowing us to see the redshifted outflowing gas. The 10 km/s FWHM and ∼ 10 −5 L line luminosity measured by Pascucci et al (2011) for [OI]6300 are also well reproduced by the X-ray photoevaporation models presented by Ercolano & Owen (2016) for accretion and X-ray luminosities and the inclination of TW Hya. (2007) found that large grains disappear quickly (10 4 yr) from the inner disc due to radial drift, suggesting that a gap would turn quickly into a hole, with no detectable central point source.…”

Section: Evidence Of X-ray Photoevaporation In Tw Hyasupporting

confidence: 66%

“…The [OI]6300 has also been shown to be produced in a slow-moving quasi-neutral X-ray photoevaporative wind (Ercolano & Owen, 2016), and is often observed to be blue-shifted with a low-velocity component of a few km/s. In the case of TW Hya the [OI]6300 was found to be centred on the stello-centric velocity (Pascucci et al 2011). This is not surprising given TW Hya near face-on inclination and the fact that the [OI]6300 line is emitted from the very inner regions of the disc wind , where the underlying disc is devoid of dust, allowing us to see the redshifted outflowing gas.…”

Section: Evidence Of X-ray Photoevaporation In Tw Hyamentioning

confidence: 99%

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A photoevaporative gap in the closest planet-forming disc

Ercolano

Rosotti

Picogna

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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The dispersal of the circumstellar discs of dust and gas surrounding young lowmass stars has important implications for the formation of planetary systems. Photoevaporation from energetic radiation from the central object is thought to drive the dispersal in the majority of discs, by creating a gap which disconnects the outer from the inner regions of the disc and then disperses the outer disc from the inside-out, while the inner disc keeps draining viscously onto the star. In this Letter we show that the disc around TW Hya, the closest protoplanetary disc to Earth, may be the first object where a photoevaporative gap has been imaged around the time at which it is being created. Indeed the detected gap in the ALMA images is consistent with the expectations of X-ray photoevaporation models, thus not requiring the presence of a planet. The photoevaporation model is also consistent with a broad range of properties of the TW Hya system, e.g. accretion rate and the location of the gap at the onset of dispersal. We show that the central, unresolved 870 µm continuum source might be produced by free free emission from the gas and/or residual dust inside the gap.

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Section: Evidence Of X-ray Photoevaporation In Tw Hyasupporting

confidence: 66%

Section: Evidence Of X-ray Photoevaporation In Tw Hyamentioning

confidence: 99%

A photoevaporative gap in the closest planet-forming disc

Ercolano

Rosotti

Picogna

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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“…These results all suggest that photoevaporation plays a dominant role in disk evolution at late times. This theoretical view is supported by recent observations of blue-shifted forbidden emission lines from some T Tauri stars (Pascucci and Sterzik, 2009;Pascucci et al, 2011). These observations unambiguously detect a slow (∼ 10 km/s), ionized wind, and are broadly consistent with the predictions of photoevaporation models (Alexander, 2008b;Ercolano and Owen, 2010); further such data will provide important new insight into the processes driving disk clearing.…”

Section: Importance Of Photoevaporation In Disk Evolutionsupporting

confidence: 75%

Circumstellar disks and planets

Wolf

Malbet

Alexander

et al. 2012

Astron Astrophys Rev

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We present a review of the interplay between the evolution of circumstellar disks and the formation of planets, both from the perspective of theoretical models and dedicated observations. Based on this, we identify and discuss fundamental questions concerning the formation and evolution of circumstellar disks and planets which can be addressed in the near future with optical and infrared long-baseline interferometers. Furthermore, the importance of complementary observations with long-baseline (sub)millimeter interferometers and high-sensitivity infrared observatories is outlined.

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“…5 presents a compilation of the Hα line profiles for our class II and class III sources). The errors on the EWs and fluxes were computed using a Monte Carlo approach: we added a normally distributed noise to the spectrum, following the error at each wavelength, and gave as error the standard deviation of the EW distribution of 1000 such spectra (Pascucci et al 2011). The errors on the flux determination are larger for the fainter lines, as the continuum calibration around these lines is more uncertain.…”

Section: Emission Lines As Accretion Diagnosticsmentioning

confidence: 99%

X-shooter spectroscopy of young stellar objects

Rigliaco

Natta

Testi

et al. 2012

A&A

177

291

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We present high-quality, medium-resolution X-shooter/VLT spectra in the range 300−2500 nm for a sample of 12 very low mass stars in the σ Orionis cluster. The sample includes eight stars with evidence of disks from Spitzer and four without disks, with masses ranging from 0.08 to 0.3 M . The aim of this first paper is to investigate the reliability of the many accretion tracers currently used to measure the mass accretion rate in low-mass young stars and the accuracy of the correlations between these secondary tracers (mainly accretion line luminosities) found in the literature. We use our spectra to measure the accretion luminosity from the continuum excess emission in the UV and visual; the derived mass accretion rates range from 10 −9 M yr −1 down to 5 × 10 −11 M yr −1 , allowing us to investigate the behavior of the accretion-driven emission lines in very low mass accretion rate regimes. We compute the luminosity of ten accretion-driven emission lines from the UV to the near-IR, which are all obtained simultaneously. In general, most of the secondary tracers correlate well with the accretion luminosity derived from the continuum excess emission. We recompute the relationships between the accretion luminosities and the line luminosities, and we confirm the validity of the correlations given in the literature, with the possible exception of Hα. Metallic lines, such as the CaII IR triplet or the Na I line at 589.3 nm, show a larger dispersion. When looking at individual objects, we find that the hydrogen recombination lines, from the UV to the near-IR, give good and consistent measurements of L acc that often better agree than the uncertainties introduced by the adopted correlations. The average L acc derived from several hydrogen lines, measured simultaneously, have a much reduced error. This suggests that some of the spread in the literature correlations may be due to the use of nonsimultaneous observations of lines and continuum. Three stars in our sample deviate from this behavior, and we discuss them individually.

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THE PHOTOEVAPORATIVE WIND FROM THE DISK OF TW Hya

Abstract: Received; accepted suggest that most of the emitting gas traced at optical wavelengths is bound to the system rather than unbound. We discuss the implications of our results for a planet-induced versus a photoevaporation-induced gap.

Cited by 95 publications

References 68 publications

A photoevaporative gap in the closest planet-forming disc

A photoevaporative gap in the closest planet-forming disc

Circumstellar disks and planets

X-shooter spectroscopy of young stellar objects

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