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more than half of all stars have companions
in small percentage of these, two stars are sufficiently close to affect each other
Lecture 14: Binary Stars
Observational Classifications
visual binaries: components can be individually detected
Sirius A & B
white dwarf
AI
Astrometric Binaries
Spectroscopic Binariessingle-lined (only one star’s spectral lines observed) and double-lined (both stars observed)
Eclipsing Binaries hotter star
Visual Doubles Alcor
Mizar
Alcor
Mizar A & B : visual binary
Mizar A: spectroscopic binary
Mizar B : spectroscopic binary
Deriving Stellar Masses
for visual binaries if orbit shape and distance known
double-lined spectroscopic and eclipsing binary with known light and velocity curve
visual binary with known orbital shape and radial velocities for both components (less common)
Roche Lobes & Lagrangian Points
equipotential surfaceLagrangian pt
co-rotating frame
Classification of Close Binaries
1) detached binaries
2) semi-detached binaries
Mass Transfer
one example
3) contact binaries
extreme example is common envelope evolution
what do you expect light curve to look like?
Evolution of Semi-Detached Binaries1) if detached component is normal star, slow mass transfer: evolved, less massive star dumps on unevolved, smaller, more massive star
Algol-like systems
0.81 solar mass star (G or K type) dumping on 3.7 solar mass B star
deep eclipse when?
2) if detached component is white dwarf --> cataclysmic variables
nova: fusion of accreted H on WDdwarf nova: accretion disk instability
3) if detached component is NS or BH --> X-ray binaries
low mass (LMXBs) : evolved low mass star overflowing Roche lobe
high mass (HMXBs) : young, massive star dumping through stellar winds
all sorts of exotic bursting scenarios
Some interesting binaries...
Cyg X-1 (first X-ray source discovered in Cygnus)
B supergiant, 8K light years, 5.6 day orbit
B supergiant --> ~30 solar masses
X-ray source compact (tens of millisecond variability)
orbit implies >6 solar masses
too much for WD or NS