X-ray impact on the protoplanetary disks around T Tauri stars

Aresu, G.; Kamp, I.; Meijerink, R.; Woitke, P.; Thi, W. F.; Spaans, Marco

doi:10.1051/0004-6361/201015449

Cited by 87 publications

(128 citation statements)

References 35 publications

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“…Inspection of Fig. 4 also shows that the o-H 2 O line flux is detected only for sources with X-ray luminosities higher than 10 30 erg s −1 , which is consistent with photochemical disc models that show that far-IR line fluxes increase significantly above this X-ray luminosity threshold (Aresu et al 2011). We note that log L x = 10 30 erg s −1 is above the median (mean) X-ray luminosity in Taurus (log L x = 29.8 (29.75) erg s −1 respectively, Güdel et al 2007).…”

Section: Resultssupporting

confidence: 83%

Detection of warm water vapour in Taurus protoplanetary discs byHerschel

Riviére-Marichalar

Ménard

Thi

et al. 2012

A&A

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Line spectra of 68 Taurus T Tauri stars were obtained with the Herschel-PACS (Photodetector Array Camera and Spectrometer) instrument as part of the GASPS (GAS evolution in Protoplanetary Systems) survey of protoplanetary discs. A careful examination of the linescans centred on the [OI] 63.18 μm fine-structure line unveiled a line at 63.32 μm in some of these spectra. We identify this line with the 8 18 → 7 07 transition of ortho-water. It is detected confidently (i.e., >3σ) in eight sources, i.e., ∼24% of the sub-sample with gas-rich discs. Several statistical tests were used to search for correlations with other disc and stellar parameters such as line fluxes of [O i] 6300 Å and 63.18 μm; X-ray luminosity and continuum levels at 63 μm and 850 μm. Correlations are found between the water line fluxes and the [O i] 63.18 μm line luminosity, the dust continuum, and possibly with the stellar X-ray luminosity. This is the first time that this line of warm water vapour has been detected in protoplanetary discs. We discuss its origins, in particular whether it comes from the inner disc and/or disc surface or from shocks in outflows and jets. Our analysis favours a disc origin, with the observed water vapour line produced within 2-3 AU from the central stars, where the gas temperature is of the order of 500-600 K.

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Section: Resultssupporting

confidence: 83%

Detection of warm water vapour in Taurus protoplanetary discs byHerschel

Riviére-Marichalar

Ménard

Thi

et al. 2012

A&A

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“…In contrast, the X-ray sensitive ionization fraction in the upper layers of the disk strongly influences ion chemistry. The following reactions are important (Aresu et al 2011):…”

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confidence: 99%

Ionization and heating by X-rays and cosmic rays

Güdel

2015

EPJ Web of Conferences

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Abstract. High-energy radiation from the central T Tauri and protostars plays an important role in shaping protoplanetary disks and influences their evolution. Such radiation, in particular X-rays and extreme-ultraviolet (EUV) radiation, is predominantly generated in unstable stellar magnetic fields (e.g., the stellar corona), but also in accretion hot spots. Even jets may produce X-ray emission. Cosmic rays, i.e., high-energy particles either from the interstellar space or from the star itself, are of crucial importance. Both highenergy photons and particles ionize disk gas and lead to heating. Ionization and heating subsequently drive chemical networks, and the products of these processes are accessible through observations of molecular line emission. Furthermore, ionization supports the magnetorotational instability and therefore drives disk accretion, while heating of the disk surface layers induces photoevaporative flows. Both processes are crucial for the dispersal of protoplanetary disks and therefore critical for the time scales of planet formation. This chapter introduces the basic physics of ionization and heating starting from a quantum mechanical viewpoint, then discusses relevant processes in astrophysical gases and their applications to protoplanetary disks, and finally summarizes some properties of the most important high-energy sources for protoplanetary disks.

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“…We apply the radiation thermo-chemical disk code ProDiMo (Protoplanetary Disk Model, Woitke et al 2009, Kamp et al 2010, Aresu et al 2011, Woitke et al 2016, to calculate the thermal and chemical structure of the disk. We use time-dependent chemistry and evolve the chemistry up to 2 million years (chemical age of the disk).…”

Section: Chemical Processing Of Disksmentioning

confidence: 99%

“…In contrast, the X-ray sensitive ionization fraction in the upper layers of the disk strongly influences ion chemistry. The following reactions are important (Aresu et al 2011; M indicates the total mass of the species in the disk):…”

Section: X-ray Driven Disk Ion Chemistrymentioning

confidence: 99%

The Gas Disk: Evolution and Chemistry

et al. 2016

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Protoplanetary disks are the birthplaces of planetary systems. The evolution of the star-disk system and the disk chemical composition determines the initial conditions for planet formation. Therefore a comprehensive understanding of the main physical and chemical processes in disks is crucial for our understanding of planet formation. We give an overview of the early evolution of disks, discuss the importance of the stellar high-energy radiation for disk evolution and describe the general thermal and chemical structure of disks. Finally we provide an overview of observational tracers of the gas component and disk winds.

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X-ray impact on the protoplanetary disks around T Tauri stars

Cited by 87 publications

References 35 publications

Detection of warm water vapour in Taurus protoplanetary discs byHerschel

Detection of warm water vapour in Taurus protoplanetary discs byHerschel

Ionization and heating by X-rays and cosmic rays

The Gas Disk: Evolution and Chemistry

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