1. Binary Star Evolution Cevin Kroxall Stellar Atmosphere’s à la Pilachowski

2. Binaries To zeroth order all stars are members of multiple systems! Really makes a difference when stars are interacting binaries  30-50% of all stars  i.e. one of the stars fills its Roche lobe More likely to encounter this after the main sequence phase  Half the stars in the sky have yet to experience this  Half of those stars will be interacting binaries in the future

3. Binary Stars

4. Binary Origins At least 50% of PMS objects are multiple systems Binaries are created before the disks clear and bonafide PMS stars are revealed Start with a molecular cloud  No B-field  Lots of physics  And 1 key assumption: its similar to single star formation

5. Are Formation Times Related to Periods? Tohline, J 2002 ARAA, 40, 349 A)Collapse starts B)Gas becomes opaque C)Ionization D)Total Ionization of H E)Quasi Equilibrium

6. Formation Mechanisms Capture  Need favorable three body encounters  Very improbable (maybe in globular cores) Prompt Fragmentation  Only homologous collapses work No scrambling of mass, proportionally collapsed  Does NOT occur before at least 1 free-fall time  Can occur in rotating clouds on the 1 st quasi equilibrium state  Mixed Results… very dependant on initial conditions and resolution in models… fragments but binaries?

7. Formation Mechanisms Delayed Break-Up  Free-fall and formation of a massive accretion disk which becomes unstable  Get Dumb-bells and pears We assume!!! No one has actually done it! Rely on stability tests Leave out viscosity and get compressible ellipsoids  Doesn’t seem to lead to binaries

8. Binary Formation Summary “In conclusion… binary formation is the primary branch of the star formation process. Obviously nature knows how to form binary star systems. Hopefully, in the coming decade [we] will find one or more fully convincing ways to do so as well.” Tohline, J 2002 ARAA, 40, 349

9. Binary Evolution “The theory of binary star evolution relies heavily on … models of single stars” “The theory of binary star evolution has a much different character then does the theory of single star evolution.” “There are no beautiful sequences of mathematically impeccable binary star models to which one can point with pride and compare successfully with observations.” Iben, 1991, ApJSS, 76, 55

10. Roche Lobes First basic concept in binary evolution theory  A unique surface of constant potential which consists of two separate lobes, each enclosing on of the stellar components  A particle inside a lobe experiences a force in the direction of the enclosed star  Assumptions: Centrally concentrated star Rotation is synchronous with orbit Circularized orbit Iben, 1991, ApJSS, 76, 55 Irradiated Roche Lobe - Podsialdlowskix http://www- astro.physics.ox.ac.uk/~podsi/podsiadl owski1.html VV Cephei systems e  0.5 L2

11. Roche Lobe Overflow How to fill your lobe Growth of a component due to internal changes Orbital shrinkage due to loss of angular momentum Swelling due to rejection of accreated matter or nuclear ignition A hardening collision between the binary and another star

12. Remnant Mass & Composition Second major concept/assumption in binary evolution  The remnant of the of the donor will have the same mass and composition as the core of the donor when it first fills its Roche lobe Iben, 1991, ApJSS, 76, 55

13. Mass Transfer & Mass Conservation 3 rd Concept - Function of the structure of the component at the moment of overflow, the degree of mass & angular momentum conservation, and the response of the companion dM/dt ~ -M/  th  If the donor does not posses a deep convective envelope, then mass & angular momentum conservation is acceptable

14. Common Envelope 4 th Concept - Secondary may form a hot expanding layer which then fills its Roche lobe Provides a frictional interaction between embedded cores and shedding material Leads to a tighter bound orbit One of the least understood phases of binary evolution One of the most important phases of binary evolution

15. Common Envelope Problems Donor has a mass larger than 70% of the accretor Theoretically most red giant donors should experience this phase  Observationally this is not true  Mass loss by stellar wind prior to mass transfer? When can the CE be ejected? When do we get a complete merger?

16. Orbital Angular Momentum Loss 5 th Concept - Angular momentum loss can drive or sustain Roche Lobe filling (keep a component in conact with its Roche lobe despite it shrinking) Mechanisms to get rid of angular momentum  Magnetic stellar wind  Gravitational wave radiation  Tidal torques  3-body interactions What happens to magnetic breaking when a donor becomes fully convective? (dynamo is killed)

17. General Classification Based upon the evolutionary stage of the mass donor at the beginning of mass transfer  Case A - main-sequence  Case B - post-main-sequence, pre-helium-ignition  Case C - post-helium-buring Two modes of mass transfer  Quasi-conservative donor has a radiative envelope, orbital periods increase  Dynamical Donor is giant with a deep convective envelope, orbits shrink  Either an ejection of the common envelope leaving a tight binary or tidal destruction of binary components leading to a merger SN 1987A over production? - Mass loss w/o spiral in? - radiative common envelope?

18. The Summary Iben Figures The adventure begins The most likely end The CV sequence

19. The Summary Iben Figures

20. Blue Stragglers (BS) Found above the turnoff Found in both (and nearly all) open and globular clusters from 10 8 - 10 13 years old First seen in M3 by Sandage (1953) Some are almost definitely NOT binaries Often centrally concentrated in clusters Li under abundant Slow rotators All are at least slightly evolved 4% are eclipsing binaries!!!!  Only 0.1% of main sequence stars in globulars are eclipsers

21. More BS Johnson & Sandage 1955, ApJ, 121, 616 UBIQUITOUS BUT RARE Only a few percent of the stars that previously populated that area of the HR diagram “Blue staggler-hood afflicts relatively few stars in a typical cluster”

22. Creating BS Stellar Merger Remnants Contraction of longer period binaries into contact binaries from angular momentum loss Related to timescales which we don’t know Stellar Collision Remnants Requires binary - binary collisions Could be responsible for 10-20% High numbers of eclipsers? BOTH REQUIRE MANY PRIMORDIAL BINARIES

23. Future BS Better statistics  Constrain ages More BS are binaries in open clusters  Is this real? (  - mergers;  - collisions) Radial distributions Why are they slow rotators? Need masses Faint main sequence proto-BS?

24. Short Period Tidally Locked Binaries Preserve fragile elements like Li by freezing mixing in surface layers due to tidal torques

25. Binary Summary “Even though a star may be single now, it may well have been a member of a binary system in the past. Indeed, whenever one is confronted with a new stellar phenomenon, it is probably adviable to first thoroughly explore the possibility of a binary interaction as a cause of the phenomenon before starting to adjust the input physics in the stellar calculation.” P. Podsiadlowski (emphasis added)