Heating Protoplanetary Disk Atmospheres

By A. Glassgold, J. Najita, J. Igea. 2004

210 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/6aa3cfbde2b805b1885100cc73d91d60b6479640

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In Astronomy and Astrophysics

1. S. Andrews
2. D. Wilner
3. J. Owen
4. Simon Bruderer
5. Xue-Ning Bai
6. A. Hughes
7. G. Herczeg
8. C. Clarke

In Spectroscopy

1. D. Wilner
2. S. Andrews
3. A. Hughes
4. Simon Bruderer
5. N. Calvet
6. C. Qi
7. Catherine C. Espaillat
8. C. Clarke

Citations in the corpus

• Planetary evaporation by UV and X‐ray radiation: basic hydrodynamics (2012, background): “…X-ray luminosities, and gas densities in planetary atmospheres, heating typically occurs to neutral column densities of N = 1022 cm−2, with the gas reaching temperatures in the range of a few hundred K to ∼ 104 K (e.g. Glassgold et al. 2004; Cecchi-Pestellini et al. 2006; Ercolano et al. 2009).”
• X-Ray-Irradiated Protoplanetary Disk Atmospheres. I. Predicted Emission-Line Spectrum and Photoevaporation (2008, methodology): “…understanding of a number of important contributors to the energetics of the system, such as accretion and wind-disk interactions, is still lacking; these ingredients can currently only be included through approximate and phenomenological approaches (e.g. see discussion in Glassgold et al., 2004).”
• The Sun in Time: Activity and Environment (2007, background): “This holds even for low viscous heating efficiency where the X-ray heating contribution entirely dominates (Glassgold et al., 2004).”
• Stellar Activity on the Young Suns of Orion: COUP Observations of K5-7 Pre-Main-Sequence Stars (2005, methodology): “…it is appropriate to update the formula given by GFM00 for the ionization rate at a radial distance r (in units of AU) from a YSO (see also Glassgold et al. 2004a): ¼ 6 ; 10 9 s 1 2 ; 10 30 Lchar ergs s 1ð Þ AU r 2 : ð7Þ This formula ignores likely attenuation and scattering of the X-rays…”
• EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, methodology): “…this assumption, we have computed a simple equilibrium gas temperature by balancing heating from stellar X-rays against grain–gas collisional cooling (Glassgold & Najita 2001; Glassgold et al. 2004; Qi et al. 2006) and find that the majority of the disk is below the thermal ionization threshold.”
• Radiation-hydrodynamic models of X-ray and EUV photoevaporating protoplanetary discs (2009, background): “…(2005) derived EUV fluxes from young solar type stars which are consistent with those required by photoevaporation, it has been pointed out (e.g. Glassgold et al. 2004; Ercolano et al. 2009b; Glassgold et al. 2009) that the EUV photons emitted by the star do not necessarily reach the disc,…”
• The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, methodology): “For protoplanetary disks, physical-chemical models have been applied by e.g. Kamp & van Zadelhoff (2001), Glassgold et al. (2004), Kamp & Dullemond (2004), Gorti & Hollenbach (2004), Nomura & Millar (2005), Aikawa & Nomura (2006), Jonkheid et al. (2004), Jonkheid et al. (2006), Jonkheid et al.…”
• Survival of molecular gas in cavities of transition disks - I. CO (2013, unknown): “Various thermo-chemical models of protoplanetary disks have been presented in the past (e.g. Kamp & van Zadelhoff 2001; Glassgold et al. 2004; Gorti & Hollenbach 2004; Jonkheid et al. 2004; Nomura & Millar 2005; Aikawa & Nomura 2006; Woitke et al. 2009; Woods & Willacy 2009; Ercolano et al. 2009;…”
• Which jet launching mechanism(s) in T Tauri stars (2006, background): “Indeed, it might be an intrinsic property of the MHD turbulence in accretion discs, regardless of the launchingof jets (see arguments developed by Kwan 1997 and Glassgold et al. 2004).”
• Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy (2006, background): “…in the disk (Ferreira & Casse 2004), for stellar spin-down (Königl 1991; Shu et al. 1994; Matt & Pudritz 2005), for heating the disk atmosphere (Glassgold et al. 2004), for hastening disk dissipation (Hollenbach et al. 2000), and for disrupting infalling material from the collapsing molecular…”
• On the theory of disc photoevaporation (2011, methodology): “Given the density at the sonic surface (∼106 cm−3), the molecular cooling would become important only if the CO abundance (XCO) exceeded 0.1 at 2000 K (using equation C7 of Glassgold et al. 2004) which is many orders of magnitude higher than expected in discs (e.g. Bruderer et al. 2009).”
• Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics (2017, background): “In reality, heating from X-rays (e.g., Glassgold et al. 2004; Ercolano et al. 2009) and AD (Garcia et al. 2001) can be substantial.”
• A SPITZER SURVEY OF MID-INFRARED MOLECULAR EMISSION FROM PROTOPLANETARY DISKS. I. DETECTION RATES (2010, background): “Also, X-rays, as compared to UV, are more effective in generating ionization in layers deep enough to facilitate efficient turbulent mixing (Igea & Glassgold 1999), but X-rays will not scale as rapidly with stellar type as UV as discussed section 5.2.2, arguing against this mechanism.”
• A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE (2009, background): “…and may be due to additional heating of gas in the upper disk by such processes as xray and UV irradiation, dissociative or mechanical heating (e.g. Glassgold et al. 2004; Kamp & Dullemond 2004; Nomura et al. 2007) Nevertheless, while the flux levels vary between the data and model prediction, the…”