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Astrophysics Flashcards

1
Q

Intensity Ratio

A

1A/1B = 2.512MB-MA

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2
Q

Magnitude Difference

A

MA-MB = 2.5log(1A/1B)

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3
Q

Small Angle Formula

A

angular diameter-arcseconds/206265 = linear diameter/distance

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4
Q

Circular Velocity

A

VC = squareroot(GM/r-meters)

M = mass of central body (kg)

G = 6.67x10-11 m3/s2kg

* Answer in m/s

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5
Q

Compare LGP

A

LGPA/LGPB = (DA/DB)2

D = diameter

* Answer in times (x)

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6
Q

Resolving Power

A

a = 11.6/D(cm)

D = diameter (cm)

* Answer in arcseconds

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7
Q

Magnification

A

M = FO/FE

FO = focal length of objective

FE - focal length of eyepiece

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8
Q

Wien’s Law

A

~max = 3,000,000/T-degrees Kelvin

* Answer in nm

~max = .2987/T x 108Å

T = 2.9x108Å/peak ~

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9
Q

Stefan-Boltzmann Law

A

E = σT4(J/s/m2)

T = K

σ = 5.67 x 10-8J/m2s degree4

* Answer in J

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10
Q

Doppler Formula

A

Vr/c = triangle~/~o

Vr = radial velocity

c = 300,000 km/s

triangle~ = change in ~

~o = observed ~

(lmaoo you’re prob laughing when u see this)

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11
Q

Fusion Explained

A

E = mc2

m = kg

c = 3x108 m/s

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12
Q

Distance to Star

A

d = 206,265/p-arcseconds

p=parallax

* Answer in AU

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13
Q

F Ratio

A

focal length(mm)/objective diameter(mm)

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14
Q

Distance Modulus

A

mv - Mv = -5 + 5log(d)

d = 10 mV-MV+5/5 = pc

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15
Q

Luminosity of Star

A

L/Lo = (R/Ro)(T/To)

* Answer in times (x)

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16
Q

Mass of Binary System

A

MA + MB = a3/p2

M= solar masses

p = orbital period (yrs)

a = AU

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17
Q

Kepler’s 3rd Law

A

p2 = a3

p = orbital period (yrs)

a = distance (AU)

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18
Q

Mass-Luminosity Relation

A

L = M3.5

M = star mass in Mo

* Answer in times (x)

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19
Q

Life Expectancy

A

T = 1/M2.5

M = star mass in Mo

* Answer in O lifetimes x 10 billion = years

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20
Q

Schwarzschild Radius

A

RS = 2GM/C2

G = 6.67 x 10-11 m3/s2kg

C = 3 x 108 m/s

M = mass (kg)

* Answer in m

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21
Q

Hubble Law

A

Vr = Hd

Vr = velocity of recession of galaxy (km/s)

H = 20km/s/Mpc

d = distance (Mpc)

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22
Q

Redshift

A

Z = triangle~/~o

triangle~ = change in ~

~o = unshifted ~

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23
Q

Age of Universe

A

TU = 1/H x 1012years

H = 70 km/s/Mpc

* Answer in years

24
Q

Distance-Rate-Time

A

d = rt

r = d/t

t = d/r

25
Q

Newton’s Law of Gravity

A

F = Gm1m2/r^2

G = 6.67 x 10-11 m3/s2kg

m1m2 = masses of objects in kg

r = distance between the two masses (m)

F = the strength of the gravitational force (N)

26
Q

Kepler’s 1st Law (Eccentricity)

27
Q

Ratio

A

distance/(size/separation)

28
Q

Frequency

29
Q

1 AU

A

1.495979 x 1011m

30
Q

1 parsec (AU)

A

206,265 AU

31
Q

1 parsec (m)

A

3.085678 x 1016m

32
Q

1 parsec (light years)

A

3.261633 light years

33
Q

1 light year

A

9.46053 x 1015m

34
Q

c, or the speed of light

A

2.997925 x 108m/s

35
Q

G, or the gravitational constant

A

(6.67 x 10(-11)) + (m3/s2)/kg

36
Q

M+

A

5.976 x 1024kg

37
Q

R+

A

6,378.164 km

38
Q

Mo

A

1.989 x 1030kg

39
Q

Ro

A

6.9599 x 108m

40
Q

Lo

A

3.826 x 1026kg

41
Q

M of the Moon

A

7.350 x 1022 kg

42
Q

R of the Moon

43
Q

M of H atom

A

1.67352 x 10-27 kg

44
Q

1 arc minute (1’)

45
Q

1 arc second (1”)

46
Q

1 Megaton

A

1,000k000 of TNT = 4.5 x 1015 J

47
Q

Gravity

A

6.67x10^-11Nm2/kg2

48
Q

Force

A

F = G x m1m2/r2

49
Q

Eccentricity

A

e2 = 1 -b2/a2

50
Q

Barycenter

A

ma/mb = rb/ra

m = mass

r = distance

51
Q

Keplar’s 3rd Law

A

p2 = (4π2/GM)a3

G = gravitational constant

M = mass of centeal object

P = solar years

52
Q

Keplar’s 2nd Law

A

rotation of the a planet around a focal point results in the same time lapse passed over two opposite, but similar given areas. This proves acceleration as we near the focal point

53
Q

1a supernovae

A

caused by white dwarves gaining mass of over 1.4 solar masses from its companion in a binary system

all 1a supernovaes have the same brightness and can determine intergalatic distances. They are brighter than type II

54
Q

Type II supernovae

A

stars must be 8+ solar masses. Iron production because as elements run out for fusion. Heavy elements > atomic #26 are created in supernovae

55
Q

Pulsars

A

stars core must be 1.4-3.2 solar masses. Emits beans of radiation at magnetic poles.

56
Q

H-R Diagram

A

relates the absolute magnitudes and luminosities of stars with spectral types and temps. Can reveal characteristics in stars and predict locations of new stars. Measured in kelvin or spectral class (O B A F G K M)

Astrophysics (1 decks)

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