scholarly journals Erratum: Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds

2021 ◽  
Vol 508 (2) ◽  
pp. 2492-2492
Author(s):  
Masanobu Kunitomo ◽  
Takeru K Suzuki ◽  
Shu-ichiro Inutsuka
Keyword(s):  
Protoplanetary Discs

scholarly journals MRI-active inner regions of protoplanetary discs. I. A detailed model of disc structure

2021 ◽  
Vol 504 (1) ◽  
pp. 280-299
Author(s):  
Marija R Jankovic ◽  
James E Owen ◽  
Subhanjoy Mohanty ◽  
Jonathan C Tan
Keyword(s):  
Energy Transport ◽  
Threshold Temperature ◽  
Mass Star ◽  
Dust Grains ◽  
Solar Mass ◽  
Detailed Model ◽  
Short Period ◽  
Pressure Maximum ◽  
Ion Emission ◽  
Protoplanetary Discs

ABSTRACT Short-period super-Earth-sized planets are common. Explaining how they form near their present orbits requires understanding the structure of the inner regions of protoplanetary discs. Previous studies have argued that the hot inner protoplanetary disc is unstable to the magnetorotational instability (MRI) due to thermal ionization of potassium, and that a local gas pressure maximum forms at the outer edge of this MRI-active zone. Here we present a steady-state model for inner discs accreting viscously, primarily due to the MRI. The structure and MRI-viscosity of the inner disc are fully coupled in our model; moreover, we account for many processes omitted in previous such models, including disc heating by both accretion and stellar irradiation, vertical energy transport, realistic dust opacities, dust effects on disc ionization, and non-thermal sources of ionization. For a disc around a solar-mass star with a standard gas accretion rate ($\dot{M}\, \sim \, 10^{-8}$ M⊙ yr−1) and small dust grains, we find that the inner disc is optically thick, and the accretion heat is primarily released near the mid-plane. As a result, both the disc mid-plane temperature and the location of the pressure maximum are only marginally affected by stellar irradiation, and the inner disc is also convectively unstable. As previously suggested, the inner disc is primarily ionized through thermionic and potassium ion emission from dust grains, which, at high temperatures, counteract adsorption of free charges on to grains. Our results show that the location of the pressure maximum is determined by the threshold temperature above which thermionic and ion emission become efficient.

scholarly journals Composition of early planetary atmospheres – II. Coupled Dust and chemical evolution in protoplanetary discs

2017 ◽  
Vol 469 (4) ◽  
pp. 3910-3927 ◽  
Author(s):  
A. J. Cridland ◽  
Ralph E. Pudritz ◽  
Tilman Birnstiel ◽  
L. Ilsedore Cleeves ◽  
Edwin A. Bergin
Keyword(s):  
Chemical Evolution ◽  
Planetary Atmospheres ◽  
Protoplanetary Discs

scholarly journals Structure of protoplanetary discs with magnetically driven winds

2018 ◽  
Vol 475 (4) ◽  
pp. 5059-5069 ◽  
Author(s):  
Fazeleh Khajenabi ◽  
Mohsen Shadmehri ◽  
Martin E Pessah ◽  
Rebecca G Martin
Keyword(s):  
Protoplanetary Discs

scholarly journals Gas and multispecies dust dynamics in viscous protoplanetary discs: the importance of the dust back-reaction

2018 ◽  
Vol 479 (3) ◽  
pp. 4187-4206 ◽  
Author(s):  
Giovanni Dipierro ◽  
Guillaume Laibe ◽  
Richard Alexander ◽  
Mark Hutchison
Keyword(s):  
Back Reaction ◽  
Dust Dynamics ◽  
Protoplanetary Discs

scholarly journals Inclinations of Circumbinary Planets: Assembly of Protoplanetary Discs and Secular Binary-Disc Interaction

2012 ◽  
Vol 8 (S293) ◽  
pp. 146-151
Author(s):  
Dong Lai ◽  
Francois Foucart
Keyword(s):  
Binary Stars ◽  
Outer Region ◽  
Orbital Plane ◽  
Close Binary ◽  
Back Reaction ◽  
Star Forming ◽  
Transiting Planets ◽  
Close Binary Stars ◽  
Mutual Inclination ◽  
Protoplanetary Discs

AbstractThe Kepler satellite has discovered a number of transiting planets around close binary stars. These circumbinary systems have highly aligned planetary and binary orbits. In this paper, we explore how the mutual inclination between the planetary and binary orbits may reflect the physical conditions of the assembly of protoplanetary discs and the interaction between protostellar binaries and circumbinary discs. Given the turbulent nature of star-forming molecular clouds, it is possible that the infalling gas onto the outer region of a circumbinary disc rotates around a different axis compared to the central protostellar binary. Thus, the newly assembled circumbinary disc can be misaligned with respect to the binary. However, the gravitational torque from the binary produces warp and twist in the disc, and the back-reaction torque tends to align the disc and the binary orbital plane. We present a new, analytic calculation of this alignment torque, and show that the binary-disc inclination angle can be reduced appreciably after the binary accretes a few percent of its mass from the disc. Since mass accretion onto the proto-binary is very likely to occur, our calculation suggests that in the absence of other disturbances, circumbinary discs and planets around close (sub-AU) stellar binaries are highly aligned with the binary orbits, while discs and planets around wide binaries can be misaligned.

scholarly journals The JCMT Gould Belt Survey: low-mass protoplanetary discs from a SCUBA-2 census of NGC 1333

2014 ◽  
Vol 447 (1) ◽  
pp. 722-727 ◽  
Author(s):  
P. Dodds ◽  
J. S. Greaves ◽  
A. Scholz ◽  
J. Hatchell ◽  
W. S. Holland ◽  
...  
Keyword(s):  
Gould Belt ◽  
Low Mass ◽  
Protoplanetary Discs

scholarly journals MBM 12: young protoplanetary discs at high galactic latitude

2009 ◽  
Vol 497 (2) ◽  
pp. 379-392 ◽  
Author(s):  
G. Meeus ◽  
A. Juhász ◽  
Th. Henning ◽  
J. Bouwman ◽  
C. Chen ◽  
...  
Keyword(s):  
Galactic Latitude ◽  
High Galactic Latitude ◽  
Protoplanetary Discs
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