1 / 33

The formation of stars and planets

The formation of stars and planets. Image credit: Michael Sherick. Lecture by C.P. Dullemond Max-Planck-Institute for Astronomy Heidelberg. Sorry about:. Topic of Star- and Planet Formation is too vast to cover completely, and in sufficient depth, in 15 hours.

henrietta
Télécharger la présentation

The formation of stars and planets

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The formation of stars and planets Image credit: Michael Sherick Lecture by C.P. Dullemond Max-Planck-Institute for Astronomy Heidelberg

  2. Sorry about: • Topic of Star- and Planet Formation is too vast to cover completely, and in sufficient depth, in 15 hours. • We will have to gloss over many things... • Many important topics not included, for example: • Origin of ‘metal’-enriched matter from which we are built • Star formation on galactic scale (e.g. star-burst galaxies) • Chemistry of star formation, photodissociation of molecules • Pre-main sequence stellar evolution • High-mass star formation (unless voluntary extension!)

  3. Literature: • S.W. Stahler & F. Palla, “The formation of stars” • L. Hartmann, “Accretion processes in star formation” • The review ‘bibles’ of star and planet formation: • Protostars and Planets II • Protostars and Planets III • Protostars and Planets IV • (next year) Protostars and Planets V

  4. Thanks to ...... for material • Ewine van Dishoeck • Carsten Dominik • Christian Fendt • Anders Johansen • Klaus Pontoppidan • Frithjof Brauer • Sascha Quantz • *Many others* The field of star and planet formation is quite a large field. I have received lots of very valuable information and material from the following people, to whom I am indebted:

  5. Technical notes on the lecture: • Target group: • PhD students and advanced undergraduate students • Physics and astrophysics • Goals: • Half overview, half in depth • Mostly theory, but strong link to observations • Powerpoint material will be put on my web site: • www.mpia.de/homes/dullemon/lectures/starplanet/

  6. Technical notes on the lecture: • Style of lecture : • Working out simple analytical models (of cloud cores, of disks, of particle motion, particle agglomeration etc.) • Discussion of state-of-the-art models with physical explanation. • Comparison of models with observations • We need solid basis in the physics of astrophysics (hour 2+3) • But first a quick overview... in pictures and movies

  7. The formation of stars and planets Day 1, Topic 1: Introduction and Overview Lecture by: C.P. Dullemond

  8. Birthplace of stars: Molecular Clouds Ophiuchus Giant Molecular Cloud (by Loke Tan)

  9. Birthplace of stars: Molecular Clouds Ophiuchus Giant Molecular Cloud (by Loke Tan)

  10. Forming stars from Molecular Clouds M. Bate Exeter UK Very dense Molecular Cloud: very aggressive star formation

  11. ‘Isolated’ Star Formation M.Hogerheijde1998, after Shu et al. 1987

  12. In the beginning... Stars are born deep in very cold dark (optically thick) clouds. Their birth is ‘secret’: not visible at optical wavelength. Infrared telescopes can penetrate through these clouds and witness the first signs of life from a protostar

  13. Feeding the infant star... • Infall of matter onto protostar is energetic: lots of radiation • In above image some radiation escapes via cavity. • Most of radiation escapes at long wavelength (infrared), because cloud is transparent at those wavelength. • Far-IR wavelength telescopes have low resolution so far, so what’s really happening down there is still difficult to study. McNeal’s Nebula

  14. Not all ‘food’ is welcome: outflows...

  15. Not all ‘food’ is welcome: outflows...

  16. Zoom-in M16 (Eagle) M17 (Horseshoe) Milky Way M8 (Lagoon) Hale-Bopp Jupiter A zoom-in to a massive star forming region Picture credit: W. Keel

  17. A zoom-in to a massive star forming region Eagle Nebula (M16) Picture credit: T.A. Rector & B.A. Wolpa

  18. A zoom-in to a massive star forming region Eagle Nebula (M16) Picture Credit: J. Hester & P. Scowen

  19. A zoom-in to a massive star forming region Eagle Nebula (M16) Picture Credit: J. Hester & P. Scowen

  20. size of our solar system A zoom-in to a massive star forming region Eagle Nebula (M16) Picture Credit: J. Hester & P. Scowen

  21. Clearing of the remnant birth cloud

  22. A star+disk appears...

  23. A star+disk appears... HST image of AB Aurigae by Carol Grady

  24. Planets form in the disk (?) Artist’s impression of planet formation...

  25. Grinding asteriods back to dust...

  26. Grinding asteriods back to dust... Planets and asteroids have formed, some asteroids get destroyed and produce the dust you observe in the image. Can the dust trace the location of (invisible) planets?

  27. The early life of a newly formed star

  28. star mass Zero-age main sequence (ZAMS) O B Oh, Be AFine Girl, Kiss Me A (Right Now Sweety!) F G K M The Harvard classification. Annie Jump Cannon, Henry Draper

  29. Pre-main-sequence: the infancy of a star Palla & Stahler

  30. Pre-main-sequence: the infancy of a star • Protostar = self-gravitating hot ball of gas, continuously being fed by accreting matter • At first: no internal nuclear heat production • Star cools by radiation: • Kelvin-Helmholz time scale • Star contracts, central density and temperature increases (!) • Deuterium ignites as soon as Tc >= 1x106 K • Thermostat: ds/dTc<0, i.e. too hot: star swells, Tc goes down, and deuterium burning slows • Star becomes fully convective • Stellar radius inflates: can reach 3...5 R.

  31. Pre-main-sequence: the infancy of a star • (We are now in the T-Tauri star phase) • Star contracts slowly • with constant temperature for low mass stars, i.e. they move vertically downward in the HR diagram • Tc and c increase until: • Hydrogen ignition • Prolonged hydrogen burning starts • This is the start of the ‘adult’ life of the star • Star reached the ZAMS

  32. Age and mass determination of PMS stars Testi et al. Martin et al.

  33. Overview of the lecture • Day 1: • Introduction • Radiation physics • Hydrodynamics and Magnetohydrodynamics • Day 2: • Giant Molecular Clouds • Self-gravitating hydrostatic spheres • Collapsing clouds • Day 3: • Viscous evolution of protoplanetary disks 1+2 • Irradiated protoplanetary disks, SEDs, observations • Day 4: • Magnetospheric accretion, jets, outflows • Motion of particles in disks • Agglomeration of particles in disks • Day 5: • The solar system and extrasolar planets • Formation of planets • Migration of planets and outlook

More Related