When to eat your brown dwarf: At breakfast, lunch or dinner? - - PowerPoint PPT Presentation

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When to eat your brown dwarf: At breakfast, lunch or dinner? - - PowerPoint PPT Presentation

Dec 04, 2023 36 likes •297 views

When to eat your brown dwarf: At breakfast, lunch or dinner? Tristan Guillot Observatoire de la Cte dAzur Doug Lin (UCSC), Pierre Morel (OCA) A&A stuff Increase font size (should be the same size as the text) Increase thickness

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When to eat your brown dwarf: At breakfast, lunch or dinner?

Tristan Guillot Observatoire de la Côte d’Azur Doug Lin (UCSC), Pierre Morel (OCA)

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SLIDE 3

A&A stuff

Increase font size (should be the same size as the text) Increase thickness Avoid vector fonts (with IDL: !p.font=0)

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M-Teff relation

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

Bouchy et al. (2011)

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SLIDE 6

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

M-Teff relation

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SLIDE 7

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

CoRoT-11 b CoRoT-15 b CoRoT-2 b CoRoT-3 b OGLE-TR-122 b WASP-30 b CoRoT-14 b WASP-19 b WASP-18 b HAT-P-20 b CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b HD 41004 B b KELT-1 b NLTT 41135C b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b XO-3 b tau Boo b

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

M-Teff relation

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SLIDE 8

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

M-Teff relation

Conjecture: Massive planets and brown dwarfs in this region have been swallowed by their star due to tidal interactions

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SLIDE 9

Probabilities

0.01 0.10 1.00 10.00 100.00 M2 [MJup] 0.0 0.2 0.4 0.6 0.8 1.0 P(Teff>6000K & M2>M2,i) Porb<5 days Porb>5 days

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

Porb<5days Porb>5days

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SLIDE 10

Consequences of tidal interactions

  • Circularization
  • Orbital migration
  • Critically depends on

period and Q parameter

  • Q measures the efficiency of

dissipation

  • Q is determined to be

around 105 to 106 for the circularization of binary stars

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SLIDE 11

4000 5000 6000 7000 Teff [K] 104 106 108 1010 1012 tmigration [years]

tau Boo CoRoT-15 CoRoT-18 CoRoT-2 CoRoT-3 OGLE-TR-122 WASP-30 CoRoT-14 WASP-19 WASP-18 OGLE-TR-123 WASP-33 HAT-TR-205-013 WASP-12 M [Mjup] 1 10 100

Q'

*=106

Q’*=106: migration timescales

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SLIDE 12

Model

Solves the tidal evolution of star +companion in the planar case (assumes Q α n) Stellar evolution models (CESAM2k) are included (radius, moment of inertia, convective zones) Magnetic breaking is taken into account The companion’s radius is fixed = 1Rjup Initial conditions are based on the

  • bserved, present-day population

Guillot, Lin & Morel, in preparation Dynamical equations: Barker & Ogilvie (2009)

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The sources of dissipation in the star

  • Constant Q model
  • Requires Q*>108
  • Cannot explain the tmig-Teff correlation
  • Dissipation of internal gravity

waves(Goodman & Dickson 1998, Barker &

Ogilvie 2010, 2011)

  • Only in stars with a radiative center
  • Only for companions with masses above a

critical mass (>3 Mjup for a 5Ga Sun)

  • Dissipation of inertial waves (Ogilvie &

Lin 2004, 2007)

  • Limited to a narrow frequency range
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The IGWs prescription

The gravity waves break and dissipate near the stellar center if there is a radiative core and if the perturbing amplitude is large enough, i.e., for the present Sun: In that case the tidal dissipation factor is:

Otherwise, we assume

Q’=107 to 1010

Barker & Ogilvie (2010)

0.00 0.01 0.02 0.03 Radius [RSun]

  • 0.0005

0.0000 0.0005 0.0010 0.0015 0.0020 Wave displacement [RSun]

1 Mjup 3 Mjup 10 Mjup 30 Mjup Non-linear

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SLIDE 15

The critical mass for dissipation

0.00 0.01 0.02 0.03 Radius [RSun]

  • 0.0005

0.0000 0.0005 0.0010 0.0015 0.0020 Wave displacement [RSun]

1 Mjup 3 Mjup 10 Mjup 30 Mjup Non-linear

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SLIDE 16

Stellar evolution models

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SLIDE 17

Magnetic braking

We assume a=1, n=1.5 and find Kw=1.5x10-14 yr-1, in agreement with Bouvier et al. 1997 We add a factor Min(1,mcz/m0) where mcz is the mass of the outer convective zone/total mass and m0=6x10-4 to account for the fact that massive stars have a slower braking

4000 5000 6000 7000 8000 Teff [K]

  • 1

1 2 3 Log(vsini) [km/s]

mcz

*=0

mcz

*=10

  • 2

mcz

*=10

  • 3

SPOCS + Nordstrom

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SLIDE 18

Constant dissipation model: Q’*=108

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 lifetime/main sequence age

0.8 0.9 1.0 1.1 1.2 1.3 1.4 Mstar [MSun]

  • 1

1 2 log(Mp) [MJup]

CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b KELT-1 b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b tau Boo b

Q’*=10

8

Pini=3days

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SLIDE 19

Constant dissipation model: Q’*=106

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 lifetime/main sequence age

0.8 0.9 1.0 1.1 1.2 1.3 1.4 Mstar [MSun]

  • 1

1 2 log(Mp) [MJup]

CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b KELT-1 b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b tau Boo b

Q’*=10

6

Pini=3days

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SLIDE 20

Internal gravity wave: full model

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 lifetime/main sequence age

0.8 0.9 1.0 1.1 1.2 1.3 1.4 Mstar [MSun]

  • 1

1 2 log(Mp) [MJup]

CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b KELT-1 b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b tau Boo b

IGW

Pini=3days

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SLIDE 21

Internal gravity wave: full model

0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 lifetime/main sequence age

0.8 0.9 1.0 1.1 1.2 1.3 1.4 Mstar [MSun]

  • 1

1 2 log(Mp) [MJup]

CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b KELT-1 b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b tau Boo b

IGW Close-in, massive companions are lost Too much orbital angular momentum F stars loose angular momentum more slowly and tidal dissipation by IGWs is not possible Low mass companions are below critical limit for IGWs dissipation except at old ages

Pini=3days

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SLIDE 22

3000 4000 5000 6000 7000 Teff [K] 0.01 0.10 1.00 10.00 100.00 M sini [MJup]

CoRoT-11 b CoRoT-15 b CoRoT-2 b CoRoT-3 b OGLE-TR-122 b WASP-30 b CoRoT-14 b WASP-19 b WASP-18 b HAT-P-20 b CoRoT-14 b CoRoT-15 b CoRoT-27 b CoRoT-3 b HAT-P-20 b HAT-TR-205-013 b HD 41004 B b KELT-1 b NLTT 41135C b OGLE-TR-106 b OGLE-TR-123 b TYC 2930-00872 b WASP-14 b WASP-18 b WASP-30 b WASP-89 b XO-3 b tau Boo b

P [days] 1 10 100 [Fe/H]

  • 0.5

0.0 0.5

Is it breakfast or dinner-time for CoRoT

  • 2?
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CoRoT

  • 2
  • CoRoT
  • 2 is a wide binary (Poppenhaeger & Wolk 2014)
  • CoRoT
  • 2A is a G7V with a 3.5 Mjup companion
  • Apparent age: 0.1-0.3 Ga
  • CoRoT
  • 2B is a K9V with a low X ray activity
  • Apparent age: >5 Ga
  • An old age helps putting back CoRoT
  • 2Ab with the
  • ther inflated hot Jupiters

0.001 10.000 1.0 1.8 0.010 0.100 1.000 Age [Ga] 1.2 1.4 1.6 Radius [RJup]

0.8 0.9 1.0 1.1 1.2 Radius [100,000 km] 2x1029 erg s-1 1029 erg s-1 3x1028 erg s-1

  • pacities x 30
  • pacities x 30

1% K.E. (4.6x1027 erg s-1) standard model 3x1029 erg s-1

Guillot & Havel (2011)

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SLIDE 24

Dynamical evolution of CoRoT

  • 2

2000 4000 6000 8000 Age [Ma] 5 10 15 20 25 Period [days]

Orbital period Stellar spin period Planet spin period log(Q*)

2000 4000 6000 8000 Age [Ma] 2 4 6 8 10 12 Period [days]

Orbital period Stellar spin period Planet spin period log(Q*)

CoRoT

  • 2 fiducial

3.5Mjup, Pini=5days, e=0 CoRoT

  • 2 massive

35Mjup, Pini=5days, e=0

Does not agree with the lack of massive planets on close orbits around G dwarfs:

  • Q’* dependence upon Pspin implies weaker dissipation in massive planet case
  • When star & planet are locked, migration is governed by magnetic braking

timescale (see Damiani & Lanza 2015)

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SLIDE 25

Planets for breakfast?

  • Mazeh et al. (2015) show that “cool” KOIs are

more aligned than “hot” KOIs (Teff>6250K)

  • up to Porb=50 days!
  • Matsakos & Königl (2015) propose that this may

be due to an early ingestion of planets

  • Swallowed planets would affect the angular momentum of

cool stars more than hot stars which have a faster rotation

  • This assumes that the stellar rotation axis and the disk with

planets are tilted initially

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SLIDE 26

Conclusions

  • There are very few brown dwarfs & massive planets as close

companions to G dwarfs whereas they are present around F dwarfs

  • This would be naturally explained by their engulfment
  • Would explain the «close-in brown dwarf desert»
  • Source of dissipation are still to be fully accounted for
  • Low magnetic braking in F-dwarfs is a critical factor
  • Internal gravity waves have the interesting properties but are unable to

account for all observations

  • Inertial waves can potentially help
  • Role of eccentricity?
  • We still don’t know when brown dwarfs get eaten…