On the chemical compositions of disks, stars and planets

On the chemical compositions of disks, stars and planets

Tristan Guillot (OCA, Nice) & Shigeru Ida (Tokyo Tech)

See Owen et al. 1999; Atreya et al. 2003 Solar reference: Lodders 2003

Explaining the noble gases in Jupiter

gas (mostly H+He) evaporates from the disk atmosphere

grains carry noble gases to the

midplane

growing giant planets

progressive

enrichment of the disk

noble gases evaporate

from the grains but not from the disk Continuing

accretion onto the Sun

Evaporation FUV externe

Explaining the noble gases in Jupiter

8

Disk mass

Disk

enrichment

Planet mass

Planet enrichment Jupiter: plain Saturn: dashed

Guillot & Hueso (MNRAS, 2006)

Observation II: The Sun’s abundance

Ramirez, Melendez & Asplund (A&A 2009)

see also Ramirez et al. (2010), Melendez et al. (2012)

Explaining the Sun vs. solar twin abundances

•

Chambers (2010) shows that the difference between the Sun and solar twins amounts to 4 earth masses less of Earth-like +

chondritic material accreted in the Sun.

• This assumes a present-day outer CZ.

•

If planet-formation is ubiquitous, difference between the Sun and other stars must be due to its giant planets

Evolution of the dust and gas

dust migrates due to gas drag

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

disk gets colder ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

first (rocky) planetesimals

form

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

suppression of accretion of rocky material onto the star

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

suppression of accretion of rocky material onto the star

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

filtering becomes 100% efficient

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

filtering becomes 100% efficient

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

ice grains condense onto planetesimals

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

ice grains condense onto planetesimals

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

filtering of ice becomes 100% efficient

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

the star accretes mostly metal-free gas

ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Evolution of the dust and gas

dust migrates due to gas drag

the ice line has moved beyond 1 AU but planetesimals there

contain no water ice line

accretion onto

the Sun «ices»

«rocks»

1 AU 10 AU

Guillot & Ida, in preparation

Filtering efficiency

0.1 1.0 10.0 100.0

10^-4 10^-2 10⁰ 10² 10⁴

perfect filtering by a MMSN protoplanet disk R_p,max=100 km and dust density=10⁰ g/cm³

0.1 1.0 10.0 100.0

Orbital distance [AU]

10^-4 10^-2 10⁰ 10² 10⁴

filtering efficiency

1.00 x MMSN gas disk

10^-4 cm

10^-2 cm 10⁰ cm 10² cm 10⁴ cm

Guillot & Ida, in preparation see Ormel & Klahr 2010,

Sekiya & Takeda 2003

Evolution of the planetesimal formation front

0.001 0.01 0.1 1 10 100 1000 10000

0.1 1 10 100

Surface Desnity [gcm-2 ]

r [AU]

1e-20 1e-18 1e-16 1e-14 1e-12 1e-10

0.1 1 10 100

g

r [AU]

100 1000 10000 100000 1e+06 1e+07 1e+08

0.1 1 10 100

t [yr]

Planetesimal Formation Front [AU]

100 1000 10000 100000 1e+06 1e+07 1e+08

0.1 1 10 100

t [yr]

Planetesimal Formation Front [AU] Guillot & Ida, in preparation

Compositions of exoplanets: global

0.0 0.5 1.0 1.5 2.0 2.5 3.0 10^[Fe/H]

-0.2 0.0 0.2 0.4 0.6 0.8 1.0

M Z/M tot

1

2 3

4 5

6

8

9

10

11 12

13

14 16

17

18 19

20

21 23

Moutou et al. (Icarus 2013) see also Guillot et al. (2006), Guillot (2008), Burrows et al. (2007), Laughlin (2011),

Miller & Fortney (2011)...

Compositions of exoplanets: atmospheres

Conclusion

•

Rich confrontation between Solar System, exoplanetary science and general astronomy

•

We have the building blocks for planet formation but are missing some crucial pieces

•

We have the possibility to directly image planets, including when they are being formed!

•

Measurements of compositions of stars, planets, protoplanetary disks are becoming possible.