Stars Luminous gaseous celestial body – spherical in shape held by its own gravity
How do we study stars? Light!!
Stellar Radiation H fusion occurs in star’s interior converting mass to E (mass deficit). T must be ~ 10 7 K, for nuclei to overcome Coulomb force & fuse. Interior of the star is so hot it is plasma.
BE of He higher than BE 4 H. H isotopes. He - 4.
Excess E is carried away by photons & neutrinos. Some E gets absorbed in star heats interior more & exerts outward pressure.
Stellar Equilibrium- outward P from radiation balances gravity inward in stable stars.
Stable Stars maintain size. The sun is stable
Ex 1. The sun is losing mass at 4.26 x 10 9 kg/s. At what rate does the sun emit energy? Assuming the mass is converted to E. E = mc 2. (4.26 x 10 9 kg/s)(3 x 10 8 m/s) x J each second.
Luminosity (L) = total power output of a star W or J/s. As we just calculated the sun converts mass to Energy Sun L = 3.9 x W. Star Power
Luminosity (W) depends on: -Surface Area - Temperature -Which equation relates power to A & T?
-L – Watts J/s -A surface A m 2 -T Kelvin = 5.67 x W/ m 2 K 4. -L = AT 4. -L = 4 r 2 T 4. Stars are regarded as black bodies
Apparent Brightness (b): how bright stars appear. What we see from Earth depends on L & distance from Earth
Def. Apparent brightness radiation from star that is incident on the Earth per m 2.
Calculation of Apparent Brightness (b): L = luminosity in W d = distance to Earth m b = apparent brightness W/m 2. Intensity
Ex 2: The apparent brightness of a star is 6.4 x 10 8 W/m 2. If its distance to Earth is 50 LY, find its luminosity.
b4 d 2 = L (6.4 x 10 8 W/m 2 ) (4 )(4.73 x m) x W d = (9.46 x m/LY)(50 LY) = 4.73 x m
Finding Star Temperature Remember Black Bodies?
Wein’s Displacement Law relates peak & surface temp for black body. Star’s spectra similar to black body. T in Kelvin in meters
as T inc. Tot intensity increase for all Peak changes to shorter higher f.
Ex 3: A star has a surface temp of K and L = 6.1 x W. a. What is the peak ? b. Find its radius.
Use Stephen Boltzmann to find R.
Solar Spectrum Some radiation absorbed by outer layers. Can identify elements in outer layers. If H is present, H will absorb = to dif between Bohr orbit levels. Form black lines.
Motion & Speed of Stars Doppler Effect/Red or Blue shift gives info. Absorption lines shift toward longer or shorter, depending on motion.
Red Shift Spectrum – stars moving away from us show dark line shift. Find v, direction by shift of line spectra.
Blue Shift – moving toward us Amount of Shift relates to speed of motion
List 3 observations we can make using light to get information about stars. State what we can learn from each type of observation.
Use Spectrum to find: Chemical composition surface (absorption spectrum) Motion toward or away from Earth Red/blue shift Surface temp Peak (color)
Ex 4: Our sun has T = 6000 K and L = 3.9 x W. If star Z has T = 4000 K, &L = 5.2 x W would expect: It to be larger or smaller to our sun? Calculate its radius in terms of our sun’s radius. Larger 26 x R sun.
Early Star Classification Spectral Class Color Temperature Composition.
Sun
Stellar spectra qbCkhttp:// qbCk From 4:48
Star Types
Types of Stars Single – not bound to another. Sun. Binary – 2 stars appear close. Most bound together by grav. Cepheid – varies in brightness on regular cycle of days – changing size. Red Giant – Old star. H burning is over. Low surface T. High L, lg area. Supergiant – very heavy star fuses elements beyond carbon. White dwarf – solar mass but planetary size no more fusion.
Binary Stars – Optical binary – appear together but not physically near each other.
Visual binaries orbit together around center of mass. Can be distinguished visually. Mass can be determined from period of revolution & separation.
Eclipsing Binary – Cannot see separate stars but 1 passes in front of the other so observed brightness varies with regular period.
Animation of eclipsing binary mfjIhttp:// mfjI
Why is there a larger dip in intensity for 1 position? Brighter/hotter star blocked bigger dip in light curve.
Spectroscopic Binary too close to distinguish eclipse but can see doppler shift
Red & Blue Shifted w/motion
Binary Star Types 4 min. kxBiIhttp:// kxBiI
Star Classification
Spectral Classes. Stars characterized by temperature, absorption lines & color. OBAFGKM Oh be a fine girl – kiss me. Then subdivided in 10 smaller groups 0-9. Sun – G2.
H-R diagram graphs temp against luminosity – Not Linear Be able to identify general regions of star types on the H-R diagram 90% Stars on Main sequence.
H-R Diagram MS Low Mass MS High Mass Small, Hot Cool, Large Cool, Super-Large Fast Burners Long Lives
HR Diagram start at 1:24
Black body radiation 12 min AI_9mk&autoplay=1&app=desktophttps:// AI_9mk&autoplay=1&app=desktop