Effects of radiation in accretion regions of classical T Tauri stars

@article{Colombo2019EffectsOR,
  title={Effects of radiation in accretion regions of classical T Tauri stars},
  author={Salvatore Colombo and Laurent Ibgui and Salvatore Orlando and Rafael Rodr{\'i}guez and Guadalupe Espinosa and Matthias Gonz'alez and Chantal Stehl'e and Lionel de S'a and Costanza Argiroffi and Rosaria Bonito and Giovanni Peres},
  journal={Astronomy \& Astrophysics},
  year={2019}
}
Context. Models and observations indicate that the impact of matter accreting onto the surface of young stars produces regions at the base of accretion columns where optically thin and thick plasma components coexist. Thus, an accurate description of these impacts is necessary to account for the effects of absorption and emission of radiation. Aims. We study the effects of radiation emerging from shock-heated plasma in impact regions on the structure of the pre-shock down-falling material. We… 

Figures from this paper

Laboratory evidence for an asymmetric accretion structure upon slanted matter impact in young stars

Aims. Investigating the process of matter accretion onto forming stars through scaled experiments in the laboratory is important in order to better understand star and planetary system formation and

Accreting protoplanets: Spectral signatures and magnitude of gas and dust extinction at H α

Context. Accreting planetary-mass objects have been detected at H α, but targeted searches have mainly resulted in non-detections. Accretion tracers in the planetary-mass regime could originate from

Non-LTE radiation hydrodynamics in PLUTO

Context. Modeling the dynamics of most astrophysical structures requires an adequate description of the interaction of radiation and matter. Several numerical (magneto-) hydrodynamics codes were

References

SHOWING 1-10 OF 39 REFERENCES

Hydrodynamic Modeling of Accretion Impacts in Classical T Tauri Stars: Radiative Heating of the Pre-shock Plasma

Context. It is generally accepted that, in Classical T Tauri Stars, the plasma from the circumstellar disc accretes onto the stellar surface with free fall velocity, and the impact generates a shock.

New insight on accretion shocks onto young stellar objects

Context. Material accreted onto classical T Tauri stars is expected to form a hot quasi-periodic plasma structure that radiates in X-rays. Simulations of this phenomenon only partly match

Magnetohydrodynamic Modeling of the Accretion Shocks in Classical T Tauri Stars: The Role of Local Absorption in the X-Ray Emission

We investigate the properties of X-ray emission from accretion shocks in classical T Tauri stars (CTTSs), generated where the infalling material impacts the stellar surface. Both observations and

X-ray emitting MHD accretion shocks in classical T Tauri stars - Case for moderate to high plasma-β values

Context. Plasma accreting onto classical T Tauri stars (CTTS) is believed to impact the stellar surface at free-fall velocities, generating a shock. Current time-dependent models describing accretion

The Structure and Emission of the Accretion Shock in T Tauri Stars

We have examined one of the key predictions of the magnetospheric infall model for classical T Tauri stars (CTTS), namely, the formation of a shock on the stellar surface. We find that accretion

New view of the corona of classical T Tauri stars: Effects of flaring activity in circumstellar disks

Context. Classical T Tauri stars (CTTSs) are young low-mass stellar objects that accrete mass from their circumstellar disks. They are characterized by high levels of coronal activity, as revealed by

On the observability of T Tauri accretion shocks in the X-ray band

Context. High resolution X-ray observations of classical T Tauri stars (CTTSs) show a soft X-ray excess due to high density plasma (ne = 10 11 −10 13 cm −3 ). This emission has been attributed to

Radiative accretion shocks along nonuniform stellar magnetic fields in classical T Tauri stars

Context. According to the magnetospheric accretion model, hot spots form on the surface of classical T Tauri stars (CTTSs) in regions where accreting disk material impacts the stellar surface at

Impacts of fragmented accretion streams onto classical T Tauri stars: UV and X-ray emission lines

Context. The accretion process in classical T Tauri stars (CTTSs) can be studied through the analysis of some UV and X-ray emission lines which trace hot gas flows and act as diagnostics of the

YSO accretion shocks: magnetic, chromospheric or stochastic flow effects can suppress fluctuations of X-ray emission

Context. Theoretical arguments and numerical simulations of radiative shocks produced by the impact of the accreting gas onto young stars predict quasi-periodic oscillations in the emitted