Long-Term Evolution of Protostellar and Protoplanetary Disks. I. Outbursts

Zhu, Zhaohuan; Hartmann, L.; Gammie, Charles F.; Book, Laura G.; Simon, Jacob B.; Engelhard, Eric K.

doi:10.1088/0004-637x/713/2/1134

Cited by 149 publications

(179 citation statements)

References 45 publications

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“…This process remains speculative because detailed physical conditions in the disk, such as viscosity, magnetic field, etc., are unknown. However, we note that these unstabilities may eventually trigger FU Ori outbursts as they propagate inward (Zhu et al 2010;Bae et al 2013), thus potentially making AA Tau a pre-FUOr candidate. Disk instabilities may also trigger dense disk winds (e.g., Lesur et al 2013;Bai & Stone 2013) that may be the source of enhanced lineof-sight extinction if they are able to lift up dust from the disk mid-plane (Owen et al 2011;Bans & Königl 2012).…”

Section: Discussionmentioning

confidence: 89%

AA Tauri’s sudden and long-lasting deepening: enhanced extinction by its circumstellar disk

Bouvier

Grankin

Ellerbroek

et al. 2013

A&A

108

143

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Context. AA Tau has been monitored for more than 20 years since 1987 and exhibited a nearly constant brightness level of V = 12.5 mag. We report here that in 2011 it suddenly faded, becoming 2 mag fainter in the V-band, and has remained in this deep state since then. Aims. We investigate the origin of the sudden dimming of the AA Tau system. Methods. We report on new optical and near-IR photometry and spectroscopy obtained during the fading event.Results. The system appears to be much redder and fainter than it was in the bright state. Moreover, the 8.2 d photometric period continuously observed for more than 20 years is not detected during most of the deep state. The analysis of the system's brightness and colors suggests that the visual extinction on the line of sight has increased by about 3-4 mag in the deep state. At optical wavelengths, the system appears to be dominated by scattered light, probably originating from the upper surface layers of a highly inclined circumstellar disk. The profiles of the Balmer lines have significantly changed as well, with the disappearance of a central absorption component regularly observed in the bright state. We ascribe this change to the scattering of the system's spectrum by circumstellar dust. Remarkably, the mass accretion rate in the inner disk and onto the central star has not changed as the system faded. Conclusions. We conclude that the deepening of the AA Tau system is due to a sudden increase of circumstellar dust extinction on the line of sight without concomitant change in the accretion rate. We suggest that the enhanced obscuration may be produced by a nonaxisymmetric overdense region in the disk, located at a distance of 7.7 AU or more, that was recently brought into the line of sight by its Keplerian motion around the central star.

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Section: Discussionmentioning

confidence: 89%

AA Tauri’s sudden and long-lasting deepening: enhanced extinction by its circumstellar disk

Bouvier

Grankin

Ellerbroek

et al. 2013

A&A

108

143

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“…Thus the ratios of mass infall rate from outer to inner disc during each outburst is related to the duration of Model presented by Zhu et al (2010) includes an MRI instability contribution to viscosity parameter if the temperature of the disc goes above MRI triggering temperature (T M ) and also includes an effective viscosity contribution from gravitational instability beyond the radius given by Toomre's instability parameter Q. The relation between R limit andṀ in this model is R limit ∝Ṁ 2 9 Thus, τ visc ∝Ṁ > ( 52 21 ) 9 ≈ 3500.…”

Section: Implication On Models Of Outburstmentioning

confidence: 99%

REAPPEARANCE OF McNEIL'S NEBULA (V1647 ORIONIS) AND ITS OUTBURST ENVIRONMENT

Ninan

Ojha

Bhatt

et al. 2013

ApJ

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We present a detailed study of McNeil's nebula (V1647 Ori) in its ongoing outburst phase starting from September 2008 to March 2013. Our 124 nights of photometric observations were carried out in optical V, R, I and near-infrared (NIR) J, H, K bands, and 59 nights of medium resolution spectroscopic observations were done in 5200 -9000Å wavelength range. All observations were carried out with 2-m Himalayan Chandra Telescope (HCT) and 2-m IUCAA Girawali Telescope. Our observations show that over last four and a half years, V1647 Ori and the region C near Herbig-Haro object, HH 22A, have been undergoing a slow dimming at a rate of ∼ 0.04 mag yr −1 and ∼ 0.05 mag yr −1 respectively in R-band, which is 6 times slower than the rate during similar stage of V1647 Ori in 2003 outburst. We detected change in flux distribution over the reflection nebula implying changes in circumstellar matter distribution between 2003 and 2008 outbursts. Apart from steady wind of velocity ∼ 350 km s −1 we detected two episodic magnetic reconnection driven winds. Forbidden [O I] 6300Å and [Fe II] 7155Å lines were also detected implying shock regions probably from jets. We tried to explain the outburst timescales of V1647 Ori using the standard models of FUors kind of outburst and found that pure thermal instability models like Bell & Lin (1994) cannot explain the variations in timescales. In the framework of various instability models we conclude that one possible reason for sudden ending of 2003 outburst in 2005 November was due to a low density region or gap in the inner region (∼ 1 AU) of the disc.

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“…The excitation of nonlinear spiral waves by giant planets also plays an important role in structuring protoplanetary disks and in driving the migration of embedded planets (Bryden et al 1999;Kley 1999;Nelson et al 2000). Models for the origin of FU Orionis outbursts have been presented where spiral waves, originating in the gravitationally unstable outer regions of protostellar disks during the early infall phase, propagate into the inner disk regions and trigger the magnetorotational instability (MRI) by heating and ionizing the disk gas there (Gammie 1999;Armitage et al 2001;Zhu et al 2010;Bae et al 2014). Recent work has also shown that the infall of low angular momentum material onto a protostellar disk during the early infall phase can also generate global spiral waves (Lesur et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Self-Destructing Spiral Waves: Global Simulations of a Spiral-Wave Instability in Accretion Disks

Bae¹,

Nelson²,

Hartmann³

et al. 2016

ApJ

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We present results from a suite of three-dimensional global hydrodynamic simulations that shows that spiral density waves propagating in circumstellar disks are unstable to the growth of a parametric instability that leads to break down of the flow into turbulence. This spiral wave instability (SWI) arises from a resonant interaction between pairs of inertial waves, or inertial-gravity waves, and the background spiral wave. The development of the instability in the linear regime involves the growth of a broad spectrum of inertial modes, with growth rates on the order of the orbital time, and results in a nonlinear saturated state in which turbulent velocity perturbations are of a similar magnitude to those induced by the spiral wave. The turbulence induces angular momentum transport and vertical mixing at a rate that depends locally on the amplitude of the spiral wave (we obtain a stress parameter α∼5×10 −4 in our reference model). The instability is found to operate in a wide range of disk models, including those with isothermal or adiabatic equations of state, and in viscous disks where the dimensionless kinematic viscosity ν10 −5 . This robustness suggests that the instability will have applications to a broad range of astrophysical disk-related phenomena, including those in close binary systems, planets embedded in protoplanetary disks (including Jupiter in our own solar system) and FU Orionis outburst models. Further work is required to determine the nature of the instability and to evaluate its observational consequences in physically more complete disk models than we have considered in this paper.

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Long-Term Evolution of Protostellar and Protoplanetary Disks. I. Outbursts

Cited by 149 publications

References 45 publications

AA Tauri’s sudden and long-lasting deepening: enhanced extinction by its circumstellar disk

AA Tauri’s sudden and long-lasting deepening: enhanced extinction by its circumstellar disk

REAPPEARANCE OF McNEIL'S NEBULA (V1647 ORIONIS) AND ITS OUTBURST ENVIRONMENT

Self-Destructing Spiral Waves: Global Simulations of a Spiral-Wave Instability in Accretion Disks

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