Abstract
We use resistive magnetohydrodynamical (MHD) simulations with the nested grid technique to study the formation of protoplanetary disks around protostars from molecular cloud cores that provide the realistic environments for planet formation. We find that gaseous planetary-mass objects are formed in the early evolutionary phase by gravitational instability in regions that are decoupled from the magnetic field and surrounded by the injection points of the MHD outflows during the formation phase of protoplanetary disks. Magnetic decoupling enables massive disks to form and these are subject to gravitational instability, even at ∼10 AU. The frequent formation of planetary-mass objects in the disk suggests the possibility of constructing a hybrid planet formation scenario, where the rocky planets form later under the influence of the giant planets in the protoplanetary disk.
| Original language | English |
|---|---|
| Pages (from-to) | L58-L62 |
| Journal | Astrophysical Journal Letters |
| Volume | 718 |
| Issue number | 2 PART 2 |
| DOIs | |
| Publication status | Published - Aug 1 2010 |
| Externally published | Yes |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Emergence of protoplanetary disks and successive formation of gaseous planets by gravitational instability. / Inutsuka, Shu Ichiro; Machida, Masahiro N.; Matsumoto, Tomoaki.
In: Astrophysical Journal Letters, Vol. 718, No. 2 PART 2, 01.08.2010, p. L58-L62.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Emergence of protoplanetary disks and successive formation of gaseous planets by gravitational instability
AU - Inutsuka, Shu Ichiro
AU - Machida, Masahiro N.
AU - Matsumoto, Tomoaki
PY - 2010/8/1
Y1 - 2010/8/1
N2 - We use resistive magnetohydrodynamical (MHD) simulations with the nested grid technique to study the formation of protoplanetary disks around protostars from molecular cloud cores that provide the realistic environments for planet formation. We find that gaseous planetary-mass objects are formed in the early evolutionary phase by gravitational instability in regions that are decoupled from the magnetic field and surrounded by the injection points of the MHD outflows during the formation phase of protoplanetary disks. Magnetic decoupling enables massive disks to form and these are subject to gravitational instability, even at ∼10 AU. The frequent formation of planetary-mass objects in the disk suggests the possibility of constructing a hybrid planet formation scenario, where the rocky planets form later under the influence of the giant planets in the protoplanetary disk.
AB - We use resistive magnetohydrodynamical (MHD) simulations with the nested grid technique to study the formation of protoplanetary disks around protostars from molecular cloud cores that provide the realistic environments for planet formation. We find that gaseous planetary-mass objects are formed in the early evolutionary phase by gravitational instability in regions that are decoupled from the magnetic field and surrounded by the injection points of the MHD outflows during the formation phase of protoplanetary disks. Magnetic decoupling enables massive disks to form and these are subject to gravitational instability, even at ∼10 AU. The frequent formation of planetary-mass objects in the disk suggests the possibility of constructing a hybrid planet formation scenario, where the rocky planets form later under the influence of the giant planets in the protoplanetary disk.
UR - http://www.scopus.com/inward/record.url?scp=78349288920&partnerID=8YFLogxK
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U2 - 10.1088/2041-8205/718/2/L58
DO - 10.1088/2041-8205/718/2/L58
M3 - Article
AN - SCOPUS:78349288920
VL - 718
SP - L58-L62
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 2 PART 2
ER -