Chemical Evolution of a Protoplanetary Disk

Semenov, D.

doi:10.1017/s1743921311024914

Cited by 2 publications

(6 citation statements)

References 98 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…ALMA observations are needed to disentangle the various phenomena at work during the earliest stages of star formation, to test model predictions of collapsing magnetized pre-stellar cores and to unveil the physical and chemical structure of the embedded disks, precursors to the protoplanetary disks which will be reviewed in the next sections. [324], [139], [395], [138] and [37]. The various regions are labeled.…”

Section: Embedded Disks: Chemistry At the Dawn Of Planet Formationmentioning

confidence: 99%

“…The gas and dust are warm and radical and ions dominate the gas composition ( [395] [323]). Water vapor in the cold outer disk has been detected toward TW Hydrae by [209] with Herschel, revealing a hidden large reservoir of water ice at large radii (between 100 and 200 AU).…”

Section: "Naked" Protoplanetary Disksmentioning

confidence: 99%

“…_ " _ Fig. 14 Schematic structure of a "naked" protoplanetary disk, adapted from [324], [139], [395], [138] and [37]. The various regions are labeled.…”

Section: Embedded Disks: Chemistry At the Dawn Of Planet Formationmentioning

confidence: 99%

“…Despite being "naked" disks, thus easier to observe than during the earlier embedded phase, the physical and chemical processes at work are complex and more (interferometric) data are sorely needed to fully understand them. Figure 14 shows a schematic picture of a T Tauri disk, compiled from a combination of figures found in [324], [139], [395], [138] and [37]: (1) within the central 1 AU from the star, a pure gas disk and the dust inner rim are present. This zone is mainly probed by Br-γ lines (e.g.…”

Section: "Naked" Protoplanetary Disksmentioning

confidence: 99%

See 3 more Smart Citations

Our astrochemical heritage

Caselli

Ceccarelli

2012

Astron Astrophys Rev

430

422

View full text Add to dashboard Cite

Our Sun and planetary system were born about 4.5 billion years ago. How did this happen and what is our heritage from these early times? This review tries to address these questions from an astrochemical point of view. On the one hand, we have some crucial information from meteorites, comets and other small bodies of the Solar System. On the other hand, we have the results of studies on the formation process of Sun-like stars in our Galaxy. These results tell us that Sun-like stars form in dense regions of molecular clouds and that three major steps are involved before the planet formation period. They are represented by the pre-stellar core, protostellar envelope and protoplanetary disk phases. Simultaneously with the evolution from one phase to the other, the chemical composition gains increasing complexity. In this review, we first present the information on the chemical composition of meteorites, comets and other small bodies of the Solar System, which is potentially linked to the first phases of the Solar System's formation. Then we describe the observed chemical composition in the pre-stellar core, protostellar envelope and protoplanetary disk phases, including the processes that lead to them. Finally, we draw together pieces from the different objects and phases to understand whether and how much we inherited chemically from the time of the Sun's birth.Comment: Invited review to be published in "The Astronomy and Astrophysics Review

show abstract

Section: Embedded Disks: Chemistry At the Dawn Of Planet Formationmentioning

confidence: 99%

Section: "Naked" Protoplanetary Disksmentioning

confidence: 99%

“…_ " _ Fig. 14 Schematic structure of a "naked" protoplanetary disk, adapted from [324], [139], [395], [138] and [37]. The various regions are labeled.…”

Section: Embedded Disks: Chemistry At the Dawn Of Planet Formationmentioning

confidence: 99%

Section: "Naked" Protoplanetary Disksmentioning

confidence: 99%

See 2 more Smart Citations

Our astrochemical heritage

Caselli

Ceccarelli

2012

Astron Astrophys Rev

430

422

View full text Add to dashboard Cite

show abstract

“…Williams & Cieza 2011, and references therein) and are in continuous evolution (e.g. Semenov 2011). Although gas constitutes the bulk of the disc mass, before the advent of ALMA our knowledge of protoplanetary discs CN (e.g.Öberg et al 2011, and references therein), probe cold gas (20 K< T <50 K) at radii >20 au.…”

Section: Introductionmentioning

confidence: 99%

Herschel GASPS spectral observations of T Tauri stars in Taurus. Unraveling far-infrared line emission from jets and discs

Alonso-Martínez

Riviére-Marichalar

Meeus

et al. 2017

A&A

View full text Add to dashboard Cite

Context. At early stages of stellar evolution young stars show powerful jets and/or outflows that interact with protoplanetary discs and their surroundings. Despite the scarce knowledge about the interaction of jets and/or outflows with discs, spectroscopic studies based on Herschel and ISO data suggests that gas shocked by jets and/or outflows can be traced by far-IR (FIR) emission in certain sources. Aims. We want to provide a consistent catalogue of selected atomic ([OI] and [CII]) and molecular (CO, H 2 O, and OH) line fluxes observed in the FIR, separate and characterize the contribution from the jet and the disc to the observed line emission, and place the observations in an evolutionary picture. Methods. The atomic and molecular FIR (60-190 µm) line emission of protoplanetary discs around 76 T Tauri stars located in Taurus are analysed. The observations were carried out within the Herschel key programme Gas in Protoplanetary Systems (GASPS). The spectra were obtained with the Photodetector Array Camera and Spectrometer (PACS). The sample is first divided in outflow and nonoutflow sources according to literature tabulations. With the aid of archival stellar/disc and jet/outflow tracers and model predictions (PDRs and shocks), correlations are explored to constrain the physical mechanisms behind the observed line emission. Results. Outflow sources exhibit brighter atomic and molecular emission lines and higher detection rates than non-outflow sources. The line detection fractions decrease with SED evolutionary status (from Class I to Class III). We find correlations between [OI] 63.18 µm and [OI] 6300 Å, o-H 2 O 78.74 µm, CO 144.78 µm, OH 79.12+79.18 µm, and the continuum flux at 24 µm. The atomic line ratios can be explain either by fast (V shock >50 km s −1 ) dissociative J-shocks at low densities (n ∼ 10 3 cm −3 ) occurring along the jet and/or PDR emission (G 0 > 10 2 , n ∼ 10 3 − 10 6 cm −3 ). To account for the [CII] absolute fluxes, PDR emission or UV irradiation of shocks is needed. In comparison, the molecular emission is more compact and the line ratios are better explained with slow (V shock <40 km s −1 ) C-type shocks with high pre-shock densities (10 4 -10 6 cm −3 ), with the exception of OH lines, that are better described by J-type shocks. Disc models alone fail to reproduce the observed molecular line fluxes, but a contribution to the line fluxes from UVilluminated discs and/or outflow cavities is expected. Far-IR lines dominate disc cooling at early stages and weaken as the star+disc system evolves from Class I to Class III, with an increasing relative disc contribution to the line fluxes. Conclusions. Models which take into account jets, discs, and their mutual interaction are needed to disentangle the different components and study their evolution. The much higher detection rate of emission lines in outflow sources and the compatibility of line ratios with shock model predictions supports the idea of a dominant contribution from the jet/outflow to the line emission, in particular...

show abstract

Chemical Evolution of a Protoplanetary Disk

Cited by 2 publications

References 98 publications

Our astrochemical heritage

Our astrochemical heritage

Herschel GASPS spectral observations of T Tauri stars in Taurus. Unraveling far-infrared line emission from jets and discs

Contact Info

Product

Resources

About