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#norelated
* ߥʡ2020 [#zbb5ecca]

ߥʡϸ§Ȥ轵14:00鳫ŤƤޤϢ ,  , Ų ,  ~
astro-phߥʡ轵12:00鳫ŤƤޤϢCarol Kwok

// ߥʡȯɽ
// 

** Schedule & History [#vfafd1d8]

[[2019ǯ>Planet2019]]
[[2018ǯ>Planet2018]]
[[2017ǯ>Planet2017]]
[[2016ǯ>Planet2016]]
[[2015ǯ>Planet2015]]
[[2014ǯ>Planet2014]]

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||ȯɽ|ȥ|Remarks|ô|h
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|[[ 1 4/9 15:00->#planet0409]]|All members| Self-introduction |15:00||
|[[ 2 4/16 14:00->#planet0409]]|Haruka Hoshino, Hirotaka Hohokabe| Small ASJ meeting |||
|[[ 3 4/23 14:00->#planet0409]]|Yuki Yoshida, Eiichiro Kokubo| Small ASJ meeting |||
|[[ 4 5/14 14:00->#planet0409]]|Sota Arakawa| Thermal history and tidal evolution of trans-Neptunian satellite systems ||Ų|
|[[ 5 5/28 14:00->#planet0528]]|Takuya Takarada (ABC)| Radial-velocity search and statistical studies for short-period planets in the Pleiades open cluster |||
|[[ 6 6/4 16:00->#planet0606]]|Beibei Liu (Lund Univ)| Pebble-driven planet formation around very low-mass stars and brown dwarfs |16:00||
|[[ 7 7/9 14:00->#planet0606]]|Yuka Fujii||||


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//ݤIshigaki(ISAS)
//ڤ(), Sakuraba(칩), Liu(Lund)
//ܴ(D1)
//ŲȡŤ() 
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//礵



//:&aname(planet1107){5/21}; ̾ȥ|
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//:&aname(planet0418){4/18}; Carina Heinreichsberger, Terrestrial or Gaseous? A classification of exoplanets according to density, mass and radius|
//When looking at Exoplanet Archives the class of a planet is not given. Therefore I tried to find an easy and fast way to classify exoplanets using only density, mass and radius. In this talk I will discuss the formation theory of Planets to explain the boundaries between the different classes (gas, terrestrial) and show the results of my empirical study.

:&aname(planet0604){6/4}; Beibei Liu, Pebble-driven planet formation around very low-mass stars and brown dwarfs|
We conduct a pebble-driven planet population synthesis study to investigate the formation of planets around very low-mass stars and brown dwarfs, in the (sub)stellar mass range between 0.01 M⊙ and 0.1 M⊙. Based on the extrapolation of numerical simulations of planetesimal formation by the streaming instability, we obtain the characteristic mass of the planetesimals and the initial masses of the protoplanets (largest bodies from the planetesimal size distributions), in either the early self-gravitating phase or the later non-self-gravitating phase of the protoplanetary disk evolution. We find that the initial protoplanets form with masses that increase with host mass, orbital distance and decrease with disk age. Around late M-dwarfs of 0.1 M⊙, these protoplanets can grow up to Earth-mass planets by pebble accretion. However, around brown dwarfs of 0.01 M⊙, planets do not grow larger than Mars mass when the initial protoplanets are born early in self-gravitating disks, and their growth stalls at around 0.01 Earth-mass when they are born late in non-self-gravitating disks. Around these low mass stars and brown dwarfs, we find no channel for gas giant planet formation because the solid cores remain too small. When the initial protoplanets form only at the water-ice line, the final planets typically have ≳15% water mass fraction. Alternatively, when the initial protoplanets form log-uniformly distributed over the entire protoplanetary disk, the final planets are either very water-rich (water mass fraction ≳15%) or entirely rocky (water mass fraction ≲5%).