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Formation of Planets around M & L dwarfs D.N.C. Lin University of California with AAS Washington Jan 11th, 2006 S. Ida, H. Li, S.L.Li, E. Thommes, I. Dobbs-Dixon,

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Presentation on theme: "Formation of Planets around M & L dwarfs D.N.C. Lin University of California with AAS Washington Jan 11th, 2006 S. Ida, H. Li, S.L.Li, E. Thommes, I. Dobbs-Dixon,"— Presentation transcript:

1 Formation of Planets around M & L dwarfs D.N.C. Lin University of California with AAS Washington Jan 11th, 2006 S. Ida, H. Li, S.L.Li, E. Thommes, I. Dobbs-Dixon, S.T. Lee,P. Garaud, M. Nagasawa Doug Lin: 17 slides

2 Disk properties Hillenbrand Calvet 1 Disk life time is independent of M * :similar available time 2 Disk accretion rate varies as M * 2 : Less gas content 3 Disk heavy element mass varies as M * 1-2 ?Less metals

3 Preferred locations Meteorites: Dry, chondrules & CAI’s Icy moons Enhancement factor > 4

4 Stellar mass dependence T(snow line) ~160K, L ~ M 2 a(snow line) ~ (L) 1/2 /T 2 ~2.7(M * /M o ) AU V k (snow)~(M/a) 1/2 ~Const ; H/a ~Const Similar aspect ratio and Keplerian speed! But shorter time scales (a/V k ) for lower M * Water-rich planets form near low-mass stars

5 Feeding zones:  10 r Hill Isolation mass: M isolation ~   a 3 M * -1/2 From planetesimals to embryos Initial growth: (runaway) Shorter growth time scale at the snow line

6 M * dependence M isolation ~1.3  a/1AU) 3/4 (M * /M o ) 3/2 M earth less massive embryos  embryos ~0.033  a/1AU) 59/20 (M * /M o ) -16/15 Myr longer growth time Can form >3M earth embryos outside 5AU within 10Myr Scaling disk models with M * : a)Solar system: Minimum-mass nebula b)Other stars:  (a) =  SN (a) h d where h d = (M * /M sun ) 0,1,2 c)Embryos with M p >M earth are formed outside snow line Importance of snow line: Interior to it: growth limit due to isolation Exterior to it: long growth time scale Outside the snow line:

7 type-II migration planet’s perturbation viscous diffusion type-I migration disk torque imbalance Disk-planet tidal interactions viscous disk accretion Goldreich & Tremaine (1979), Ward (1986, 1997), Tanaka et al. (2002) Lin & Papaloizou (1985),....

8 Low-mass embryo (10 Mearth) Cooler and invisic disks

9 (Mass) growth vs (orbital) decay Loss due to Type I migration Embryos’ migration time scale Outer embryos are better preserved only after significant gas depletion Critical-mass core:M p =5M earth

10 Flow into the Roche potential Equation of motion: Bondi radius (R b =GM p /c s 2 ) Hill’s radius (R h =(M p /3M * ) 1/3 a) Disk thickness (H=c s a/V k ) R b / R h =3 1/3 (M p /M * ) 2/3 (a/H) 2 decreases with M * If R b > R h,, a large decline in  (+ve r gradient) would be needed to overcome the tidal barrier. A small  at the Hill’s radius would quench the accretion flow.

11 Reduction in the accretion rate Growth time scales: Embryos’ emergence time scale: ~  a/1AU) 59/20 (M * /M o ) -16/15 Myr KH cooling/contraction of the envelope: ~ (M p /M earth ) -(3-4) Myr Uninhibited Bondi accretion: ~(H/a) 4 (M * 2 /M p M d  k ~ yr(M J /M p ) Uninhibited accretion from the disk: ~M p /(dM/dt)~ yr(M p /M J ) Reduction due to Hill’s barrier: >  disk depletion Tidal barriers suppress the emergence of gas giants around low-mass stars

12 Gap formation & type II migration Viscous and thermal conditions Lower limiting mass for gas giants around low-mass stars Neptune-mass planets can open up gaps and migrate close to the stars

13 Hot Neptunes around low-M * stars Radial extent is determined by V k > V escape

14 Migration-free sweeping secular resonances Resonant secular perturbation M disk ~M p (Ward, Ida, Nagasawa) Ups And Transitional disks

15 Dynamical shake up (Nagasawa, Thommes) Bode’s law: dynamically porous terrestrial planets orbits with low eccentricities with wide separation

16 Formation of water worlds Jupiter-Saturn secular interaction & multiple extrasolar systems Sweeping secular resonance may be more intense in low-mass stars. But the absence of gas or ice giants would leave behind dynamically-hot earth-mass objects

17 Summary 1.Snow line is important for the retention of heavy. Around low-mass stars, planets with mass greater than that of the earth are formed outside the snow line. 2. Planet-disk interaction can lead to depletion of first generation planetesimals, especially around low-mass stars 3.Self regulation led to the stellar accretion of most heavy elements, the late emergence of planets, and perhaps the inner holes inferred from SED’s. 4. Around low-mass stars, gas accretion rate onto proto gas giants is also suppressed by a tidal barrier. 5. Neptune-mass embryos can open up gaps and migrate to the stellar proximity. 6.Residual planetesimals may have modest eccentricities. 7 There will be a desert of gas giants and an oasis of terrestrial planets, including short-period water worlds around dwarfs.


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