Practical Numerical Training UKNum

Transcription

1 Practical Numerical Training UKNum Conclusions Dr. H. Klahr & Dr. C. Mordasini Max Planck Institute for Astronomy, Heidelberg Programm: 1) Weiterführende Vorlesungen 2) Fragebogen 3) Eigene Forschung 4) Bachelor/Masterarbeiten

2 1 Weitereführende Vorlesungen

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8 2 Fragebogen

9 3 Eigene Forschung

10 Galaxies, stars and planets 10 billion galaxies How many harbor life? 100 billion stars how many planets? How frequent? Life? First generation of human beings with technology to answer this.

11 Ways to understanding Herschel s 1789 For many centuries Cloud collapse Hertzsprung Russel Nuclear Fusion Stellar Mass Funct. Sun Stars Solar System La Silla Obs. ESO Darwin ESA For a decade In a decade? Formation in disks Collisions Gas accretion Migration Exoplanets Astrobiology Habitable Zone Biomarkers Complex Life Life Extraterrestrial Life?

12 Planet formation: The paradigm Gravitational Core - remote observations - in-situ measurements - sample returns - laboratory analysis - theoretical modeling Minority line Party line Accretion Instability A satisfactory theory should explain the formation of planets in the solar system as well as around other stars.

13 Planet formation: Sequential picture in presence of gas in absence of gas dust 10 7 years 10 7 years Star & protoplanetary disk planetesimals protoplanets migration giant planets giant impacts 10 8 years type I type II terrestrial planets dynamical rearrangement

14 Quantitatively, planet formation is a complex process Huge dynamical range in size/mass: grains to giant planets Multiple input physics: gravity, hydrodynamics, radiative transport, [ thermodynamics, magnetic fields, impact physics, material properties,... Strong non-linear mechanisms (e.g. runaway growth) Feedbacks and interactions (e.g. protoplanetary disk-planet: orbital migration) dσ dt = 3 r r [ ] r 1/2 ) r νσr1/2 + Σ w (r) + Q planet (r). dm dr =4πr2 dp ρ dr = Gm ρ r ( ) 2 dl dr =4πr2 ρ ϵ T S dt t dr = T dp P dr = d ln T d ln P =min( ad, rad ) rad = 3 0 = q h 2 2 p r 2 p 2 p dr p dt = 2r p tot J p 64πσG d P dt κlp T 4 m = (3M ) 1/3 dm Z 6 a 2 B L M 1/3 dt 3 4 H R H + 50 qr 1 dm Z dt ρ(p )=ρ 0 + cp n. = p R 2 captf G (e, i) 1/3 Mp r H = r p 3M H Planet formation and evolution difficult to understand from first principles alone.

15 Magnetohydrodynamic disk models around young stars

16 Instabilities in disks

17 Orbital migration of planets

18 High mass star formation models

19 Fig. III.1.1: Two of the most important statistical observational constraints for planet formation theory. The left panel shows the semimajor axis mass diagram of the extrasolar planets. The different colors indicate the observational detection technique. mass-radius lines for planets of different compositions. In both panels, the planets of the Solar System are also shown. Note that these figures are not corrected for the various observational biases, which favor for the radial velocity and the transit tech- Exoplanets: statistical tests for theory Mass Mass [Earth [M mass] ] Jupiter Saturn Neptune Uranus 5 Radial velocity Venus Earth & Transits Earth 1 Microlensing Venus Direct imaging Neptune , Semimajor axis [AU] Mass [Earth masses] Radius [R Earth ] Uranus Saturn Jupiter ice rocky jovian Credit: C. Mordasini

20 Extrasolar planet population synthesis

21 Bachelorarbeit Kai Salm

22 4 Verfügbare Bachelor/ Masterarbeiten

23 Current Batchelor/Master projects

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