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ASTC25 Lecture 7

Useful books: Carroll and Ostlie “Intro To Modern Astrophys”, Prialnik “Intro to Stellar Stuct. & Evol.”. Hayashi, Jeans, and the necessity of disks. ASTC25 Lecture 7. Jeans instability & the collapse of molecular clouds. James Hopwood Jeans (1877-1946). How Do Stars Form?. Oph.

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ASTC25 Lecture 7

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  1. Useful books: Carroll and Ostlie “Intro To Modern Astrophys”, Prialnik “Intro to Stellar Stuct. & Evol.” Hayashi, Jeans, and the necessity of disks ASTC25 Lecture 7

  2. Jeans instability & the collapse of molecular clouds James Hopwood Jeans (1877-1946)

  3. How Do Stars Form?

  4. Oph Giant Molecular Cloud, 160 pc away contains numerous dark clouds

  5. GMCs contain: dark clouds, cores, Bok globules GMC mass / solar mass ~ 105 V380 Ori + NGC1999 Oph

  6. Dark clouds L57 Barnard 68

  7. Jeans mass

  8. Jeans mass

  9. Following the fragmentation history, and tracking the way M_Jeans changes w.r.t. the fragment mass, Hoyle (1953) arrived at a concept of opacity-limited fragmentation. When heat gets trapped by opacity, Jeans mass increases because T raises. The smalles mass of fragment is ~0.01 M_sun = 10 m_jup

  10. Chushiro Hayashi (1920-2010 ) Hayashi tracks and thePre-Main Sequenceevolution of stars

  11. Hayashi theory gives a nice explanation for ~vertical tracks of PMS objects in the H-R diagram, however we need to make certain assumptions/guesses Log L Log T_eff H-R diagram

  12. Hayashi phase of protostar contraction Star formation in reality is a bit different: e.g., no spherical symmetry!

  13. Which regions of a star are convective and which radiative? That depends on mass... M/M_sun Sun is radiative except for a thin subsurface layer 10 solar mass star has convctive core and radiative envelope

  14. UKAFF (UK Astroph. Fluids Facility) supercomputer (parallel computer) Stars are forming in… these boxes.

  15. Matthew Symmetric initial conditions Bate (1998)

  16. Realistic star formation simulations using Smoothed Particle Hydrodynamics became possible several years ago. (Up to) millions of particles represent a moving, irregular, 3-D grid, and can be thought of as gas clouds that partially overlap. Each particle interacts with 10…50 neighbors to represent pressure forces with good accuracy. A somewhat ad hoc treatment also endows gas with viscosity. The gas is self-gravitating.

  17. Matthew Bate (2003), Bate and Benz (2003) SPH, 1.5M particles starting from turbulent gas cloud collapse starts after turbulence dies down and Jeans mass drops below the cloud mass.

  18. Brown dwarfs - a failedattempt at stardom As seen in the simulation of molecular cloud fragmentation, brown dwarfs (smallest objects simulated as white points) form in large numbers, and are mostly dispersed throughout the Galaxy afterwards. Sometimes, they are found as orbital companions to stars (not frequently, hence the term “brown dwarf desert” by comparison with the large numbers of planetary companions to stars.) And there is even one BD with it’s own companion of only 5 Jupiter masses!

  19. A strange system discovered in 2003 (among other by Ray Jayawardhana from UofT) : 5 M_jup planet around a 25 M_jup Brown Dwarf in 2MASS1207 BD image has been removed by observational technique ESO/VLT AO HST/NICMOS, 1.6um

  20. Disks - a natural way to stardom As seen in the simulation of molecular cloud fragmentation, star formation is very non-spherical and not even very axisymmetric: it is 3-D and leads to protostars surrounded by accretion disks. The main physical reason is the angular momentum (L) conservation: before L is transferred outward (e.g. by viscosity), the gas cannot approach the rotation axis; but it has no such restriction on approaching the equatorial plane (or midplane), where it gathers in the form of a rotationally-supported thin disk.

  21. disk

  22. R ~ 200 AU

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