stellar properties distance trig parallax d(pc) = 1/p (arcsec)
DESCRIPTION
Stellar Properties Distance trig parallax d(pc) = 1/p (arcsec) Velocity (V space ) 2 = (V rad ) 2 + (V tan ) 2 Brightness mag = -2.5 log (flux) + constant; L Temperature B-V; spectral class Mass spectroscopic binary; K, P, i Radius eclipsing spectroscopic binary. - PowerPoint PPT PresentationTRANSCRIPT
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Stellar Properties
1) Distance trig parallax d(pc) = 1/p (arcsec)
ü Velocity (Vspace)2 = (Vrad)2 + (Vtan)2
1) Brightness mag = -2.5 log (flux) + constant; L
2) Temperature B-V; spectral class
3) Mass spectroscopic binary; K, P, i
4) Radius eclipsing spectroscopic binary
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pd
1 AU
tan p = 1AU / d (AU)
for small angles p =1 AU/ d(AU)
d (AU) = 1/p where p is in radians
1 radian = 206265 arcsec
d (AU) = 206265 / p (arcsec) (define 1pc = 206265 AU)
d (pc) = 1 / p (arcsec)
1. Distance
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Parallax measurements
nearest star ~ 0.8” (d~ 1.3 pc)
ground limit ~ 0.01” (d~ 100 pc)
HST limit ~ 0.001” (d~ 1000pc)
Hipparcos (1989-1993) [120,000 stars to 0.001”; 1 million stars to 0.02”]
GAIA (2013-2018) [1 billion stars] to 0.000020”
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2. Velocity
proper motion
(Space V)2 = (Radial V)2 + (Tangential V)2
Radial V from Doppler:
/ = v/c
Tangential V from proper motion arcsec/yr :
Vt = 4.74 /p km/s
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Proper Motion
d
Vt
Vr
sin = = Vt/d
Vt = d = /p pc/yr
rad arcsec, pc km, yr sec
Vt = 4.74 /p km/s
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depends on d, speed and direction
Barnard’s star (d=1.85pc) has largest =10”/yr
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http://youtu.be/yxPPDDP5kyQ
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3. Brightness - T, size, dMagnitude scale: backwards, logarithmic
Energy scale: luminosity, flux L=4R2T4 ergs/s
Magnitudes: each mag is factor of 2.5 fainter
1 mag = 2.5
5 mag = 100
10 mag = 10,000
Apparent mags (m) as seen from Earth
Absolute mags (M) if object at 10 pc
mag = -2.5 log flux + constant
m2 - m1 = -2.5 log f2 / f1
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Sun -26.5 +5
moon -12.5 +19
Venus -4 +27.5
Sirius -1.4 +1.4
Vega 0 0.5
eye 6
30in 15
5m 20
faintest 28
m M
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apparent mags absolute mags
5 pc
10 pc
15 pc
5 pc
10 pc
-26.5
1.3
2.0
3.3
4.2
5.06.0
2.0 2.00.0
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Absolute mag M: if star were viewed at 10pc
Apparent mag: star as viewed from earth
m-M = -2.5 log (E/d2) - (-2.5 log (E/102))
= -2.5 log E + 5 log d + 2.5 log E - 5
m-M = -5 + 5 log d distance modulus
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Color Index
mb - mv = Mb - Mv = B-V
mv - mr = V-R
B-V gives temperature
Common filters: U,B,V,R,I,J,H,K Johnson
ugriz Sloan
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Hot star looks blue B-V ~ - 0. 5
Cool star looks red B-V ~ 1. 5
visual filter
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T
B-V
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Bolometric Magnitude:
Brightness over all ~ L
Mbol = Mv + BC
Mbol* - Mbol = -2.5 log L*/L
Mbol ~ 4.74, L ~ 4x1033 ergs/s
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Brightness - depends on T, R, d
Magnitudes (backwards, logarithmic)= -2.5 log(flux) + C or m2 - m1 = -2.5 log (f2/f1)
• m (apparent mag - as seen from earth - includes d)
• M (absolute mag - object at 10 pc - eliminates d)
• m-M = -5 + 5 log d (distance modulus)
• MBOL (bolometric mag - over all ) = MV + BC
• B-V (color index) - gives T
Energy (luminosity, flux)
• L= total energy from star/sec = 4R2T4 ergs/s
• Flux = energy received at earth at = L/4d2 ergs/cm2/s/Å
• MBOL* - MBOL(sun) = -2.5 log (L*/Lsun)
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4. Temperature (B-V, Spectral Class)
-6 O(5-9) HeII >30,000K -0.3
B(0-9) He 11-30,000 -0.1
+1 A H strong 7500-11000 0.0
F CaII 6000-7500 0.3
+5 G metals 5000-6000 0.6
K metals,bands 3500-5000 1.0
+15 M TiO 2000-3500 1.5
R K with C
N M with C
S ZrO
L hydrides <2000
T methane <1300
Mv Class Lines Temp B-V
Luminosity Class: I, II=SG, III, IV=Giant, V=dwarf (main sequence)
sun = G2V
B-V=-0.865 + 8540/T
T~ 9000/[(B-V)+0.93]
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Spectral Class Mnemonics
Oh, Be A Fine Girl(Guy), Kiss Me Right Now Smack
Oh Brother, Astronomy Finally Gruesomely Killed Me Right Now *Slump*
Oven Baked Ants, Fried Gently, Kept Moist, Retain Natural Succulence (Largely True)
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He
H
metals
molecules
Sun
Vega
Betelgeuse
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Jacoby atlas
1984, ApJS,
56, 257
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Info from Spectra:
• abs= normal star, emission = disk or jet
• composition of outer layers (if line present, element present
• temperature of outer layers (from knowledge of energy levels of element)
• density (narrow lines imply low density)
• pressure (wide lines imply high pressure)
• rotation (high rotation makes wider lines)
• binarity (see spectra of two different stars)
• wind (strange P Cygni line profiles with absorption + emission)
• magnetic field (Zeeman splitting of lines)
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WD spectrum
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Spectra of giants
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P Cygni features
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Spectroscopic parallax:
1. Use stars < 100pc to calibrate MV for spectral classes
2. For unknown star:
a) use CCD to measure mV
b) use spectrograph to find spectral class
c) use calibration from (1) to get MV
d) use distance modulus to calculate d
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Different Kinds of Temperature
Type From Observe
Brightness Planck fctn F
Color Planck fctn B-V
Effective (T4) Stefan-Boltzman L & R
Excitation Boltzman Ratio of lines
Ionization Saha Ratio of lines
Kinetic Thermal Doppler Width of lines
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5. Mass (double - lined spectroscopic binaries)
m1/m2 = v2/v1
m1 + m2 = 42a3/GP2 (a=vP/2)
v1 sin i, v2 sin i, P
come from radial velocity curve of binary
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Alcor and Mizar are just neighbors but Mizar itself is a visual binary and Mizar A and Mizar B are each binaries
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xm1m2
d1 d2 m1d1 = m2d2
v = 2d/P so d=vP/2
m1v1P/2 = m2v2P/2
m1v1 = m2v2
m1/m2 = v2/v1
center of mass physics
Kepler’s 3rd law
Fg = Fc
GmM/r2 = mv2/ r v = 2r/P
GM/r = 42r2/P2
M = 42r3/GP2
.r. Mm
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Mass - from spectroscopic binaries need K1, K2, P, i)
m1/m2 = v2 / v1= K2 / K1
m1 + m2 = 42(a1 + a2)3 /GP2
K1 = v1 sin i = 2a1sin i / P
a1 = PK1 / 2 sin i
a1 + a2 = P (K1 + K2) / 2 sin i
m1 + m2 = (42 / GP2)P3(K1+K2)3/83sin3i = P(K1+K2)3/2G sin3i
for double-lined binary
(m1+ m2)P2 = (a1+ a2)3 = a13(1+ a2/a1)3
a2/a1 = m1/m2
(m1+ m2)P2 = a13(1+ m1/m2)3 = a1
3(m1+ m2)3/m23
f(m1, m2) = m23sin3i/(m1+m2)2 = a1
3/P2 = K13P/83
For single-lined binary with solar mass units
mass function gives a lower limit to m2
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Mass of Sun (from planet orbits) = 2 x 1033 g
Star masses range from 0. 07 M to 100 M
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Which is star 1 and which star 2?
Which star is more massive?
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K2K1
m2/m1 = K1/K2 ~ ?
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6. Radius
• from lunar occultation
• from interferometry (for supergiants)
• from T, L (R = [L/4T4]1/2)
• from eclipsing, spectroscopic binaries (need eclipse times, K1, K2)
D1 = (K1+ K2) ta-b where a-b is ingress or egress time
D2 = (K1+ K2) ta-c where a-c is ingress/egress + eclipse time
Radii of stars range from 1/100 R to 400 R
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a
b c
d
a b cd
primary eclipse secondary eclipse
a-b or c-d moves diameter of small star Ds
a-c or b-d moves diameter of large star DL
Ds = V x ta-b DL = V x ta-c where V = Ks + KL
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1 5 10 15 20 25
P=?
e=?
i=?
Rs/RL= ?
Ms/ML=?
a =?
Ds=?
DL=?
Ms=?
ML=?
Ls/LL=?
Ts/TL=?
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1 5 10 15 20 25
P=24 hr
e=0
i=90
Rs/RL= 1/3
Ms/ML=2
a= 3x106=.02AU
Ds=8.1x105=0.6Dsun
DL=2.4x106=1.7Dsun
Ms=0.4Msun
ML=0.8Msun
Ls/LL=1.51
Ts/TL=1.9
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radius
density
0.01R
400 R
10-6 g/cm3
106 g/cm3
mass
100 M
0.07M
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Location depend on:
Mass
Age
Composition
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uses ~20,000 stars
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Mass - Luminosity Relation