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Photometric Binaries - Coggle Diagram
Photometric Binaries
Modeling
mass fraction :explode: important
Normalized
Roche Potential
leads to Roche lobes
Circular orbits
Sync rotation
forms due to RL
Algol type = no mass transition
exeeds L_1
the eclipses are wider
Overfill RL = stars touch each other
WUMA system
eclipses interpertation
phase 1:
going down gradually due to the smaller star covers bigger one
ingress
Phase 2:
smaller star is in the area of bigger one
phase 3:
gradually goes out - Smaller star
degress
reflection effect
if T_1>> T_2
irradiation
usually moddeled as simple reflection
but not good enough
Space is not good either
limiting factors
cosmic radiation degradation
Balloon EXP
data transfer
Crowding
Unfocused images
redistribute the light
to get as many photons as we can
rich fields
When the stars of very larg
santrigugal force
T_pole> T_equator
grabity darkening
???
limb effects
gray atmospheric models
Roche lobe doen't fell
cause 2 periods in one phase
Reletevistic effects of light curves
Gravitational MicroLensing
Can be applied to binaries
brightening the stars
it's not resolvable but we can see the magnifications
used for
DM (dark matter)
???
We can have it in R_dot distance too
They are observed
Anti-ransit event
G-lensing of binary not planet like WD
By the flux of transits we can have mass
after take into account the GR correction in modelling
