Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim

By Peter Woitke, I. Kamp, W. Thi. 2009

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Context. Emission lines from protoplanetary disks originate mainly in the irradiated surface layers, where the gas is generally warmer than the dust. Therefore, interpreting emission lines requires detailed thermo-chemical models, which are essential to converting line observations into understanding disk physics. Aims. We aim at hydrostatic disk models that are valid from 0.1 AU to 1000 AU to interpret gas emission lines from UV to sub-mm. In particular, our interest lies in interpreting far IR gas emission lines, such as will be observed by the Herschel observatory, related to the Gasps open time key program. This paper introduces a new disk code called ProDiMo. Methods. We combine frequency-dependent 2D dust continuum radiative transfer, kinetic gas-phase and UV photo-chemistry, ice formation, and detailed non-LTE heating & cooling with the consistent calculation of the hydrostatic disk structure. We include Fe ii and CO ro-vibrational line heating/cooling relevant to the high-density gas close to the star, and apply a modified escapeprobability treatment. The models are characterised by a high degree of consistency between the various physical, chemical, and radiative processes, where the mutual feedbacks are solved iteratively. Results. In application to a T Tauri disk extending from 0.5 AU to 500 AU, the models show that the dense, shielded and cold midplane

Subfields: Astronomy and Astrophysics, Spectroscopy

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Citations in the corpus

Photodissociation and photoionisation of atoms and molecules of astrophysical interest (2017, background): “…the dissociation of species and shielding by H and H2 line-by-line, to compute the photodestruction of molecules as functions of depth into a PDR (e.g., van Dishoeck & Black 1988; Viala et al. 1988; Jansen et al. 1995; Le Petit et al. 2006; Woitke et al. 2009; Walsh et al. 2013; Li et al. 2013).”
EVIDENCE OF FAST PEBBLE GROWTH NEAR CONDENSATION FRONTS IN THE HL TAU PROTOPLANETARY DISK (2015, methodology): “…ices we define the condensation temperature of species i as that where the thermal desorption and accretion rates are equal, i.e., niice × k i desorp = n i gas × k i accr , (4) where kidesorp and k i accr are calculated using the treatment outlined in Woitke et al. (2009) and Walsh et al. (2010).”
Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “…and far-infrared excess by adding a narrow scale height peak, but during our fitting procedure it became clear that a parametrized optically thick inner disk rim blocks a large amount of the UV irradiation, lowering the gas temperature significantly, as also demonstrated in Woitke et al. (2009).”
Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “This back-heating by Fe ii has also been found to be an important heating agent in other models (see Woitke et al. 2009).”
A NEW NETWORK FOR HIGHER-TEMPERATURE GAS-PHASE CHEMISTRY. I. A PRELIMINARY STUDY OF ACCRETION DISKS IN ACTIVE GALACTIC NUCLEI (2010, background): “…temperatures in excess of 1000 K, and the chemistry of these regions has become a topic of extreme interest, with models by many authors (e.g., Markwick et al. 2002; Gorti & Hollenbach 2008; Agúndez et al. 2008; Nomura et al. 2009; Woods & Willacy 2009; Glassgold et al. 2009; Woitke et al. 2009).”
EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “Physical Parameters Physical models of the dust and gas in protoplanetary disks have become increasingly complex (e.g., D’Alessio et al. 1998; Woitke et al. 2009; Fogel et al. 2011).”
CHEMICAL PROCESSES IN PROTOPLANETARY DISKS (2010, background): “…prescriptions for the UV radiation field in the disk leads to different distributions of radicals such as C2H and CN. Photodesorption and cosmic-ray induced desorption are now routinely included in modern chemical models of protoplanetary disks (e.g. Woitke et al. (2009); Henning et al. (2010)).”
A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, background): “Detailed models of the heating and cooling processes show the gas temperature smoothly transitions from the midplane value to a hotter atmospheric value at z/r ∼ 0.1 − 0.5 for r = 10 − 100 AU (Kamp & Dullemond 2004; Nomura et al. 2007; Gorti & Hollenbach 2008; Woitke et al. 2009).”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, background): “…account for the effects that X-ray heating, chemical differentiation, and gas-dust temperature departures have on the vertical structure of the disk (e.g., van Zadelhoff et al. 2001; Jonkheid et al. 2004; Kamp & Dullemond 2004; Kamp et al. 2010; Woitke et al. 2009, 2010; Aresu et al. 2011).”
TOWARD CHEMICAL CONSTRAINTS ON HOT JUPITER MIGRATION (2014, methodology): “The volume mixing ratios of these species for a solar composition disk are derived based on chemical equilibrium in the disk mid-plane (Woitke et al. 2009) as well as from observations of protoplanetary disks (Öberg et al. 2011; Draine 2003; Pontoppidan 2006); our adopted values are shown in Table…”
A SPITZER SURVEY OF MID-INFRARED MOLECULAR EMISSION FROM PROTOPLANETARY DISKS. I. DETECTION RATES (2010, background): “Woitke et al. (2009) modeled the abundance of water vapor throughout the disk surrounding a Herbig Ae star, including a detailed treatment of UV-driven photochemistry, and found that the inner disk abundance is high, if shielded, reaching 10−5 − 10−4 per hydrogen nucleus, and can maintain…”
Astrochemistry and compositions of planetary systems (2020, unknown): “2006), and protoplanetary disks (Gorti and Hollenbach 2004; Woitke et al. 2009; Kamp et al. 2010; Bruderer et al. 2012; Du and Bergin 2014).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “These abundance fractions are motivated by either theoretical chemical calculations (Case 1, Woitke et al. 2009) or observation of ice grains in protplanetary discs (Case 2, Draine 2003; Pontoppidan 2006; Öberg et al. 2011).”
Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “…> −6, (B.4) A47, page 9 of 10 where n is the number density of hydrogen atoms and χ describes the intensity of the UV radiation field, following Woitke et al. (2009) χ = 1 FDraine ∫ 205 nm 91.2 nm uλ dλ, (B.5) with FDraine = 1.921 × 1012 m−2 s−1, and where uλ is the energy density of the…”
The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, methodology): “We use the same elemental composition as Jonkheid et al. (2006) and Woitke et al. (2009a), which is summarized in Table A.1.”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “…other ionizing agents (e.g., Aikawa & Herbst 2001; Bergin et al. 2003; Semenov et al. 2006; Nomura et al. 2007; Willacy 2007; Dutrey et al. 2007; Woitke et al. 2009; Walsh et al. 2010; Kamp et al. 2010; Fogel et al. 2011; Cazzoletti et al. 2018), because many chemical reactions are regulated by…”