Reconnection X-winds: spin-down of low-mass protostars

Ferreira, Jonathan; Pelletier, G.; Appl, S.

doi:10.1046/j.1365-8711.2000.03215.x

Cited by 93 publications

(90 citation statements)

References 10 publications

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“…It is interesting to briefly consider the study of Ferreira et al (2000), which explores CTTS interactions with the surrounding disk for both dipole and higher order magnetic field components. This study is primarily concerned with the rotational spin down of young protostars into and through the TTS phase; however, the authors explicity ignore the torque associated with the surrounding accretion disk.…”

Section: Discussionmentioning

confidence: 99%

“…This is not to suggest that the above studies are the only such studies of magnetospheric accretion in CTTSs. There are a number of others, some of which derive their results from numerical studies of the governing equations (e.g., Paatz & Camenzind 1996), while some focus on the instabilities that can result between the star, its magnetosphere, and the disk, which may launch winds and jets (e.g., Hayashi, Shibata, & Matsumoto 1996;Goodson, Winglee, & Bö hm 1997;Miller & Stone 1997;Goodson, Böhm, & Winglee 1999;Ferreira, Pelletier, & Appl 2000). These studies are not directly testable in the fashion explored in this paper; however, important tests of many of these works may be possible with variability studies (see Goodson et al 1999).…”

Section: Magnetospheric Accretion Predictionsmentioning

confidence: 99%

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New Tests of Magnetospheric Accretion in T Tauri Stars

Johns–Krull

Gafford

2002

ApJ

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We examine three analytic theories of magnetospheric accretion onto classical T Tauri stars (CTTSs) under the assumption that the magnetic field strength does not vary appreciably from star to star. From these investigations we derive predicted relationships among the stellar mass, radius, rotation period, and disk accretion rate. Data from five studies of the accretion parameters of CTTSs are used to test the predicted correlations. We generally find that the data do not display the predicted correlations except for that predicted by the model of Shu et al. as detailed by Ostriker & Shu and extended here to include nondipole field topologies. Their identification of the trapped flux as an important quantity in the model appears to be critical for reconciling the observed data to the theory. While the data do generally support the extended Ostriker & Shu predictions, only one of the two studies for which the requisite data exist shows the highest correlation when considering all the relevant parameters. This suggests that great care must be taken when trying to use existing observations to test the theory.

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Section: Discussionmentioning

confidence: 99%

Section: Magnetospheric Accretion Predictionsmentioning

confidence: 99%

New Tests of Magnetospheric Accretion in T Tauri Stars

Johns–Krull

Gafford

2002

ApJ

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“…Since it is believed that a sporadic outflow is driven by the star-disk magnetic interaction (Ferreira et al 2000;Matt et al 2002), we examine such cases as well. In this case we adopt a similar function:…”

Section: Time Variabilitymentioning

confidence: 99%

Two-component jet simulations

Matsakos¹,

Massaglia²,

Trussoni

et al. 2009

A&A

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Context. Theoretical arguments along with observational data of YSO jets suggest the presence of two steady components: a disk wind type outflow needed to explain the observed high mass loss rates and a stellar wind type outflow probably accounting for the observed stellar spin down. Each component's contribution depends on the intrinsic physical properties of the YSO-disk system and its evolutionary stage. Aims. The main goal of this paper is to understand some of the basic features of the evolution, interaction and co-existence of the two jet components over a parameter space and when time variability is enforced. Methods. Having studied separately the numerical evolution of each type of the complementary disk and stellar analytical wind solutions in Paper I of this series, we proceed here to mix together the two models inside the computational box. The evolution in time is performed with the PLUTO code, investigating the dynamics of the two-component jets, the modifications each solution undergoes and the potential steady state reached. Results. The co-evolution of the two components, indeed, results in final steady state configurations with the disk wind effectively collimating the inner stellar component. The final outcome stays close to the initial solutions, supporting the validity of the analytical studies. Moreover, a weak shock forms, disconnecting the launching region of both outflows with the propagation domain of the twocomponent jet. On the other hand, several cases are being investigated to identify the role of each two-component jet parameter. Time variability is not found to considerably affect the dynamics, thus making all the conclusions robust. However, the flow fluctuations generate shocks, whose large scale structures have a strong resemblance to observed YSO jet knots. Conclusions. Analytical disk and stellar solutions, even sub modified fast ones, provide a solid foundation to construct twocomponent jet models. Tuning their physical properties along with the two-component jet parameters allows a broad class of realistic scenarios to be addressed. The applied flow variability provides very promising perspectives for the comparison of the models with observations.

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“…Their characteristics seem to reproduce several features of the observed jets [5] so that they still represent one of the best candidates to explain the jet phenomenon in CTTS. A scenario in which a disk field interacts with the stellar magnetic flux has been proposed (Reconnection X-wind, [35]) and it deserves future investigation. On the other hand, if the open stellar flux is compressed in a small region of the disk, the local magnetic field becomes strong enough to potentially launch a more energetic outflow.…”

Section: Disk Windsmentioning

confidence: 99%

Magnetospheric outflows in young stellar objects

Zanni

2014

EPJ Web of Conferences

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Abstract. Different classes of outflows are associated with the magnetospheric activity of accreting T Tauri protostars. Stellar winds are accelerated along the open field lines anchored in the stellar surface; disk winds (extended or X-type) can be launched along the open magnetic surfaces threading the accretion disk; another type of ejection can arise from the region of interaction of the closed magnetosphere with the accretion disk (magnetospheric ejections, conical winds), where the magnetic surfaces undergo quasiperiodic episodes of inflation and reconnection. In this chapter I will present the main dynamical properties of these different types of outflow. Two main issues will be addressed. First, I will try to understand if these ejection phenomena can account for the origin of the jets often observed in young forming stellar systems. Second, I will evaluate the impact of these outflows on the angular momentum evolution of the central protostar.

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Reconnection X-winds: spin-down of low-mass protostars

Cited by 93 publications

References 10 publications

New Tests of Magnetospheric Accretion in T Tauri Stars

New Tests of Magnetospheric Accretion in T Tauri Stars

Two-component jet simulations

Magnetospheric outflows in young stellar objects

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