Luminosity and Colour of Stars Michael Balogh Stellar Evolution (PHYS 375)
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Transcript of Luminosity and Colour of Stars Michael Balogh Stellar Evolution (PHYS 375)
Luminosity and Colour of StarsLuminosity and Colour of Stars
Michael BaloghStellar Evolution (PHYS 375)
The physics of starsThe physics of stars
A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it’s own pressure.
To understand how this simple system behaves, however, requires an understanding of:1. Fluid mechanics2. Electromagnetism3. Thermodynamics4. Special relativity5. Chemistry6. Nuclear physics7. Quantum mechanics
X-ray ultraviolet infrared radio
Course OutlineCourse Outline
Part I (lectures 1-5) Basic properties of stars and electromagnetic radiation Stellar classification Measurements of distance, masses, etc.
Part II (lectures 6-13) Chemical composition of stars (interpretation of spectra) Stellar structure (interiors and atmospheres) Energy production and transport
Part III (lectures 14-22) Stellar evolution (formation, evolution, and death) White dwarfs, neutron stars, black holes
The nature of starsThe nature of stars
• Stars have a variety of brightnesses and colours
• Betelgeuse is a red giant, and one of the largest stars known
• Rigel is one of the brightest stars in the sky; blue-white in colour
Betelgeuse
Rigel
Apparent brightness of starsApparent brightness of stars
Star nameRelative brightness
Distance (light years)
Sirius 1 8.5
Canopus 0.49 98
Alpha Centauri
0.23 4.2
Vega 0.24 26
Arcturus 0.25 36
Capella 0.24 45
Star nameRelative brightness
Distance (light years)
Proxima Centauri
0.0000063
4.2
Alpha Centauri
0.23 4.2
Barnard’s star
0.000040 5.9
Wolf 359 0.000001 7.5
Lalande 21185
0.00025 8.1
The apparent brightness of stars depends on both:• their intrinsic luminosity• their distance from us
Their colour is independent of distance
The five brightest stars The five nearest stars
The Astronomical UnitThe Astronomical Unit
Astronomical distance scale: Basic unit is the Astronomical Unit (AU), defined as the
semimajor axis of Earth’s orbit
How do we measure this? Relative distances of planets from sun can be
determined from Kepler’s third law:
E.g. given Pearth, Pmars:
32 aP 32
Mars
Earth
Mars
Earth
a
a
P
P
1AU = 1.49597978994×108 km
The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit
This defines the unit 1 parsec = 206265 AU = 3.09×1013 km ~ 3.26 light years
ParallaxParallax
1 AU
p
d
Measuring ParallaxMeasuring Parallax
The star with the largest parallax is Proxima Centauri, with p=0.772 arcsec. What is its distance?
A star field with 1” seeing
These small angles are very difficult to measure from the ground; the atmosphere tends to blur images on scales of ~1 arcsec. It is possible to measure parallax angles smaller than this, but only down to ~0.02 arcsec (corresponding to a distance of 1/0.02 = 50 pc). Until recently, accurate parallaxes were
only available for a few hundred very nearby stars.
HipparcosHipparcos
The Hipparcos satellite (launched 1989) collected parallax data from space, over 3 years
120,000 stars with 0.001 arcsec precision astrometry
More than 1 million stars with 0.03 arcsec precision
The distance limit corresponding to 0.001 arcsec is 1 kpc (1000 pc). Since the Earth is ~8 kpc from the Galactic centre it is
clear that this method is only useful for stars in the immediate solar neighbourhood.
Parallax: summaryParallax: summary
1. A fundamental, geometric measurement of distance
2. Can be measured directly3. Limited to nearby stars4. Is used to calibrate other, more indirect distance
indicators. Ultimately even our estimates of distances to the most remote galaxies rests on a reliable measure of parallax to the nearest stars
BreakBreak
The electromagnetic spectrumThe electromagnetic spectrum
• The Earth’s atmosphere blocks most wavelengths of incident radiation very effectively. It is only transparent to visual light (obviously) and radio wavelengths.
• Observations at other wavelengths have to be made from space.
U B V R I
Different filters transmit light of different wavelengths. Common astronomy filters are named:
BlackbodiesBlackbodiesThe energy radiated from a surface element dA is given by:
dddAdTBddAdTB sincos)(cos)(
Units of B(T): W/m2/m/sr
BlackbodiesBlackbodies
Energy quantization leads to a prediction for the spectrum of blackbody radiation:
1
2)(
4)(
5
2
kT
hc
e
hcTu
cTB
The energy radiated from a surface element dA is given by:
dddAdTBddAdTB sincos)(cos)(
Units of B(T): W/m2/m/sr
Planck’s lawPlanck’s law
Calculate the luminosity of a spherical blackbody: Each surface element dA emits radiation isotropically Integrate over sphere (A) and all solid angles ()
2
0
2/
0
sincosA
dddAdBdL
dBA
Properties of blackbody radiationProperties of blackbody radiation
1. The wavelength at which radiation emission from a blackbody peaks decreases with increasing temperature, as given by Wien’s law:
K cm 290.0max T
424 eTRL 2. The total energy emitted (luminosity) by a
blackbody with area A increases with temperature (Stefan-Boltzmann equation)This defines the effective temperature of a star with radius R and luminosity L
ExamplesExamples
The sun has a luminosity L=3.826×1026 W and a radius R=6.96×108 m. What is the effective temperature? At what wavelength is most of the energy radiated?
K cm 290.0max T424 eTRL
ExampleExample
Why does the green sun look yellow?
The human eye does not detect all wavelengths of light equally
ExamplesExamples
Spica is one of the hottest stars in the sky, with an effective temperature 25400 K. The peak of its spectrum is therefore at 114 nm, in the far ultraviolet, well below the limit of human vision. We can still see it, however, because it emits some light at longer wavelengths
K cm 290.0max T
424 eTRL
Apparent magnitudesApparent magnitudes
The magnitude system expresses fluxes in a given waveband X, on a relative, logarithmic scale:
Note the negative sign means brighter objects have lower magnitudes
Scale is chosen so that a factor 100 in brightness corresponds to 5 magnitudes (historical)
refrefX f
fmm log5.2
The magnitude scaleThe magnitude scale
refrefX f
fmm log5.2
One common system is to measure relative to Vega By definition, Vega has m=0 in all bands. Note this does not mean Vega
is equally bright at all wavelengths!
Setting mref=0 in the equation above gives:
X
XVegaX
mf
ffm
,0
,
log5.2
log5.2log5.2
• Colour is defined as the relative flux between two different wavebands, usually written as a difference in magnitudes
Apparent magnitudesApparent magnitudes
Object Apparent mag
Sun -26.5
Full moon -12.5
Venus -4.0
Jupiter -3.0
Sirius -1.4
Polaris 2.0
Eye limit 6.0
Pluto 15.0
Reasonable telescope limit (8-m telescope, 4 hour integration)
28
Deepest image ever taken(Hubble UDF)
29
The faintest (deepest) telescope image taken so far is the Hubble Ultra-Deep Field. At m=29, this reaches more than 1 billion times fainter than what we can see with the naked eye.
95/465.2/)629( 101010
refrefX f
fmm log5.2