TY - JOUR
T1 - Pebble accretion in Class 0/I YSOs as a possible pathway for early planet formation
AU - Tanaka, Yuki A.
AU - Tsukamoto, Yusuke
N1 - Funding Information:
We thank the anonymous referee for their useful reports that greatly improved the manuscript. This work was supported by Ministry of Education, Culture, Sports, Science and Technology (MEXT) Leading Initiative for Excellent Young Researchers and Japan Society for the Promotion of Science (JSPS) KAKENHI grant number JP18K13581.
Publisher Copyright:
© 2019 The Author(s).
PY - 2019/4/1
Y1 - 2019/4/1
N2 - Recent theoretical works suggest that the pebble accretion process is important for planet formation in protoplanetary discs, because it accelerates the growth of planetary cores. While several observations reveal axisymmetric sharp gaps in very young discs, which may be indicative of the existence of planets. We investigate the possibility of planet formation via pebble accretion in much earlier phases, the gravitationally unstable discs of Class 0/I young stellar objects. We find that under the conditions of the Class 0/I discs, the pebble accretion time-scales can be shorter compared to the typical protoplanetary discs due to larger gas and dust accretion rate, but also find that the accretion time-scale is not always a decreasing function of the gas accretion rate. By using estimated accretion time-scales, we give a required initial mass to form cores of gas giants within the lifetime of Class 0/I phases under several parameters, such as radial distances from the host star, gas accretion rates, and dust-to-gas mass ratio. In the most optimistic case, for example the dust-to-gas mass ratio is f = 3fsolar, ∼10−4 M objects at 10 au can grow to 10 M cores during the typical lifetime of the Class 0/I phases, 0.5 Myr.
AB - Recent theoretical works suggest that the pebble accretion process is important for planet formation in protoplanetary discs, because it accelerates the growth of planetary cores. While several observations reveal axisymmetric sharp gaps in very young discs, which may be indicative of the existence of planets. We investigate the possibility of planet formation via pebble accretion in much earlier phases, the gravitationally unstable discs of Class 0/I young stellar objects. We find that under the conditions of the Class 0/I discs, the pebble accretion time-scales can be shorter compared to the typical protoplanetary discs due to larger gas and dust accretion rate, but also find that the accretion time-scale is not always a decreasing function of the gas accretion rate. By using estimated accretion time-scales, we give a required initial mass to form cores of gas giants within the lifetime of Class 0/I phases under several parameters, such as radial distances from the host star, gas accretion rates, and dust-to-gas mass ratio. In the most optimistic case, for example the dust-to-gas mass ratio is f = 3fsolar, ∼10−4 M objects at 10 au can grow to 10 M cores during the typical lifetime of the Class 0/I phases, 0.5 Myr.
KW - Planet-disc interactions
KW - Planetary systems
KW - Planets and satellites: formation
KW - Planets and satellites: physical evolution
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U2 - 10.1093/mnras/stz069
DO - 10.1093/mnras/stz069
M3 - Article
AN - SCOPUS:85063372569
SN - 0035-8711
VL - 484
SP - 1574
EP - 1588
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -