photometric bin Flashcards

1
Q

what are photometric bin?

A
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2
Q

role of inclination

A
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3
Q

EA, EB, EW

A

eclipsing ALgol type: no contact
eclipsing beta lyrae type: contact
eclipsing W Ursae Majoris type: contact bin w CE

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4
Q

prob with ground based obs?

A

AM
reddening

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5
Q

advantage of ground based obs?

A

cheap

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6
Q

solution to AM?

A

comparison star see if variablity is same

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7
Q

conditions fro comparison star?

A

close by
similar temp
same color (to same reddening effect)

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8
Q

other uses of photometric analysis

A

exoplanet
asteriod

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9
Q

telescopes observing for photometric analysis?

A
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10
Q

problem w space based obs.

A

expensive (data transfer, fewer missions)
light reflection
cosmic rays

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11
Q

parameters derived

A

roche potential from mass ratio

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12
Q

types od attachment

A

detached
contact
overcontact

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13
Q

effect of tidal interactions?

A

circular orbits
synchronised rotation

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14
Q

how different lightcurve effects help derive orbital parameters?

A
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15
Q

lc variation w orbital period fro ref, ellipsoid?

A

ref– sine– orbital period
ellipsoid sine– orbital period / 2

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16
Q

parametres info from ellipsoid

A

ellipsoid deformation is based on tidal forces, roche geometry:
q– deformation (obs in lc) propotional to mass ratio
a– semi major axis inv propotional to distortion
R

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17
Q

what is Gravity darkening

A

tidal forces or fastrotation can make equator more stretched out, T_pole> T_equator

18
Q

what do limb darkening and gravity darkening look like in lc?

A

limb darkening – rounded curve in eclipse minima

19
Q

what lc effect grav darkenig can be obs with?

A

ellipsoidal effect

20
Q

what is Gravitational lensing & Gravitational self-lensing ?

A
21
Q

gravitational lensing, why flux inc? why lc top curve rounded?

A
22
Q

ellipsoid– why sinosidal variations are asymmteric?

A
23
Q

relatistiv beaming

A

in space based missions– flux amplified for blue-shifted. asymmetric amp–
sd + wd

24
Q

which lc variation effect produces diagnostic parameters ?
which dont?

A

Do:
eclipses: R
relatistic beaming: lc -> R_V
ellipsoid (q, R/a)

Don’t:
grav lensing?
reflection?

25
Q

effcts that cause change in eclipses?

A

romers delay
rositter mc laugllin effect

26
Q

romers delay

A

diff masses– slight different dist to observer- slight shift in time light reaches us

27
Q

rositter mclauglin effect

A

brcause of rotation– some part of star is blushifted and other red– eclipses in blue n red shifted part– effects spectra– radial velocity

28
Q

when is rositter mclaughlin effect more prominent?

A

fast rotation– far from the center

29
Q

use of rositter mclaughlin effect

A

more useful for eclipse not at the center
when eclipses are not in the orbital plane (misaligned) eclipse not in the center –
discovery of exoplanets (un aligned, retrogate)
young massive stars otherwise are difficult to find paramters because of rotatinal broadening

30
Q

identify rositter mclaughlin effect in radial vel curve?

A

for: blueshifted
redshifted
retrograde

31
Q

can you measure mass ratio from romers delay? how?

A

yes, del t = cont. x K (1- m2/m1)

32
Q

parameters observable for eclipsing binaries?

A

info of all parameters –
inclination, distance = astrometry
mass = spectra
radius = eclipse

33
Q

how are double line eclipsing binaries amazing?

A
34
Q

sine lc?

A

ref or ellipsoid?

35
Q

diff between ref or ellipsoid?

A

period
ref vary by p
ellipsoid vary by p/2

36
Q

how does romer delay help identify masses?

A
37
Q

how does ellipsoidal help put constraints on inclination?

A

lc dependednt on R/a, q and inclination

38
Q

how are gravitational lensing and self gravitational lensing identified in lightucurves?

A

anti transit or shallower eclipses than estimated

39
Q

use of gravitational lensing?

A

flux ratio proportional to M2/R1?

40
Q

use of relativistic doppler beaming?

A

lc –> radial velocity curve –> orbital parameters
cheaper than spectra

41
Q
A