Alexander Krivov, Sebastian Müller, Torsten Löhne, Harald Mutschke

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From observations of debris dust to properties of planetesimals Alexander Krivov, Sebastian Müller, Torsten Löhne, Harald Mutschke Astrophysical Institute and

1 From observations of debris dust to properties of planetesimals Alexander Krivov, Sebastian Müller, Torsten Löhne, Harald Mutschke Astrophysical Institute and University Observatory Friedrich Schiller University Jena Germany Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

2 A planetary system and its debris disk Planets Planetesimal belt + Debris dust = Debris disk Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

3 Outline Approach Application to unresolved disks Application to resolved disks Summary Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

4 Outline Approach Application to unresolved disks Application to resolved disks Summary Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

5 Idea of this work Traditional approach Planetesimal belt? Collisional model Our approach Dust disk Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Observables Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3, Thermal emission model

6 Collisional model: ACE Initial planetesimal belt Analysis of Collisional Evolution Debris disk at subsequent time instants Features: - statistical code in an (m,a,e)-mesh - accurate photogravitational dynamics - collisions (mergers, cratering, disruption) - diffusion by P-R and stellar wind - distributed parallel computing Authors: Krivov & Sremčević ( ), Löhne ( ) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

7 Results: dust distributions Distance-dependent size distribution Size-dependent radial distribution cf. Krivov, Löhne, & Sremčević, AAp 455 (2006) Thébault & Augereau, AAp 472 (2007) Löhne, PhD thesis (2008) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

8 Thermal emission model: SEDUCE & SUBITO SED Utility for Circumstellar Environment Size and spatial distribution of dust, its optical properties SUrface Brightness Investigation TOol Features: - NextGen stellar photosphere models - Mie calculations for arbitrary (n,k) - Thermal emission (no scattered light) SED radial brightness profile Author: Müller ( ) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

9 Results: dust temperatures Absorption Efficiency Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

10 Outline Approach Application to unresolved disks Application to resolved disks Summary Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

11 Input and output Model parameters Star: stellar mass M * stellar luminosity L * stellar age t * Planetesimal belt: initial mass M 0 location r width dr excitation <e>,<i> known (fixed) poorly known (fixed) unknown (free) SED Observables All solids: Collisions: bulk density mechanical properties optical properties critical fragmentation energy fragments size distribution cratering efficiency Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

12 Reference disks 3AU 10AU 30AU 100AU 200AU G2V star Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

13 Scaling rules F (M 0, r, t) F (xm 0, r, t) = x F(M 0, r, xt) Löhne, Krivov, & Rodmann, ApJ 673 (2008) F (M 0, r, t) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

14 Results: SEDs for reference disks Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

15 Application to selected debris disks Stars : G2V Dust data: from various surveys with IRAS, ISO, Spitzer, Keck II, JCMT Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

16 Comparison of observed SEDs to modeled SEDs F (M 0, r, t * ) Belt mass, from SED s height Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Belt location, from SED s peak wavelength Age, assumed known Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

Derived masses and locations of (outer) planetesimal belts System [HD] 377 70573 72905 107146 141943 ~130AU Belt mass [M earth ] 32 2.5 Ardila et al. ApJ 624, L141-142 (2005) 0.23 47 6.

17 Derived masses and locations of (outer) planetesimal belts System [HD] ~130AU Belt mass [M earth ] Ardila et al. ApJ 624, L (2005) Belt location [AU] ~200 ~200 ~100 ~200 ~100 Dust mass [M earth ] 3.1x x x x x10-3 Large ( AU) and massive ( earth masses) Kuiper belt analogs But: results sensitively depend on assumed dust properties Krivov, Müller, Löhne, & Mutschke, ApJ 687 (2008) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

18 Outline Approach Application to unresolved disks Application to resolved disks Summary Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

19 Input and output Model parameters Star: stellar mass M * stellar luminosity L * stellar age t * Planetesimal belt: initial mass M 0 location r width dr excitation <e>,<i> All solids: bulk density mechanical properties optical properties known (fixed) poorly known (fixed) unknown (free) SED Observables Brightness profiles in different colors Collisions: critical fragmentation energy fragments size distribution cratering efficiency Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

20 Application to the Vega disk Su et al., ApJ (2005); Marsh et al., ApJ (2006) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

21 The first-guess model Star: L * =37L sun Belt: AU, <e>=0.1 Material: astrosil Collisonal outcome model: nominal Müller, Löhne, & Krivov, in prep. Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

22 The best model Star: L * =25L sun Belt: AU, <e>=0.1 Material: astrosil Collisonal outcome model: flat size distribution of fragments Müller, Löhne, & Krivov, in prep. Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

23 Outline Approach Application to unresolved disks Application to resolved disks Summary Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

Summary We suggest a constructive way of using debris disk observations to constrain planetesimal properties Unresolved cases: application

2-50 earth masses) Kuiper belt analogs Resolved cases: application to the Vega disk showed it to be compatible to a steady-state

24 Summary We suggest a constructive way of using debris disk observations to constrain planetesimal properties Unresolved cases: application to five G2V excess stars revealed large ( AU) and massive ( earth masses) Kuiper belt analogs Resolved cases: application to the Vega disk showed it to be compatible to a steady-state collisional evolution scenario, contrary to previous claims Herschel Open Time Key Program DUNES (DUst around NEarby Stars) Planet Formation and Evolution: The Solar System and Extrasolar Planets Tübingen, March 3,

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