Astronomy college course/Sizes of white dwarfs, neutron stars, quasars
Redshift and blueshift can be associated with the Doppler effect
This unit explores how know the sizes of white dwarfs, neutron stars, and quasars. In the process of answering these questions, we shall learn about the doppler effect in astronomy, the gravitational redshift, energy conservation, the cosmic redshift, and causality.
White dwarfs and the gravitational redshift[edit | edit source]
Review white dwarf stars:
- The fate of stars with less than 1.4 solar masses (includes sun)
- Radius of 0.01R☉ (i.e. 0.01 Solar radii) can be deduced from its position on the HR diagram.
- We know the luminosity because we know the apparent magnitudes and the distance, which allows us to apply the inverse square law to deduce total power output (also called luminosity). But how do we know the distance? That was easy, the first discovered white dwarf was observed as a companion to a well known star.
- And because we know the distance to the companion star, we also know that mass of the white dwarf (if we believe in gravity)
- But are we really sure about the temperature? The equations for luminosity, color, temperature, distance and relative magnitude all assume that the star is a black body. How do we know that it is a black body?
- The figure to the right shows the actual spectrum of the type A0V star Vega. Stars don't really have a unique temperature because we see through several layers that are semi-transparent, allowing light from a variety of temperatures to reach our eyes (telescope). By convention, astronomers have devised an "effective temperature", and for Vega, it is 9500K. Reality is complicated. Even humans have different temperatures for different parts of the body.
Gravitational redshift[edit | edit source]
- Another verification of the white dwarf's size comes from General Relativity (which is much more advanced than special relativity because it demands that Euclidean geometry be abandoned).
Time dilation is one of the bewildering features of relativity.
An intuitive understanding of the gravitational redshift comes from the photon picture of light and conservation of energy. When a particle of mass m is ejected from a massive planet (of mass M), the particle loses kinetic energy, KE =mv2 , where v is speed. By Einstein's theory of special relativity, the speed of the particle, v, never exceeds the speed of light, c (where c≈ 3×108m/s). But a photon has zero mass and a speed equal to c (if it is in a vacuum). Since the energy of a photon is given by E=hf, the only way a photon can lose energy is to reduce it's frequency, f (since h is a universal constant called Planck's constant).
Time dilation is one of the bewildering features of relativity. The light clock shown illustrates how Einstein deduce that a moving clock seems to travel slowly. The "tick" of this clock is the time it takes for light to bounce from one mirror to the other. If all observers perceive light to travel from one mirror to the other, and if a stationary and moving observer both perceive light to be travelling at the same speed, then the "tick" of the clock seems slower to an observer watching a moving clock. (This would not be a paradox, for example of people tossing a ball back and forth on a train, since the two observers perceive different speeds for the ball.)
- Identified in 1731 by John Bevis; independently rediscovered in 1758 by Charles Messier as M1 (who was hunting comets and eventually made a catalog of things that are not comets (things comet hunters should ignore). (See Messier objects)
- Blue color produced by synchrotron radiation, which is radiation given off by the curving motion of electrons in a magnetic field.
- Even though the Crab Nebula is the focus of much attention among astronomers, its distance remains an open question, owing to uncertainties in every method used to estimate its distance. In 2008, the consensus was that its distance from Earth is 2.0 ± 0.5 kpc (6.5 ± 1.6 kly). Note: It is best to remember percent uncertainty: 0.5/2.0 = 0.25/1 = 0.25 =25%.
- One method of calculating the distance to compare the angular expansion with the spectroscopically determined expansion velocity.
- The "fingers" seen in close-up images are caused by a low density gas pushing against a high density gas that is essential "above". Such a combinations of fluids is unstable. See also Bill Blair's page.
How we know neutron stars are small[edit | edit source]
- The plasma surrounding the neutron star is far too unstable to model it as a simple black body. The position on the HR diagram tells us nothing. As far as I can tell, we have three reasons for believing the small size:
- The size can be calculated using an advanced version of Quantum Theory. This calculation is less reliable than for the white dwarf because nuclear physics and relativity play a greater role. Is the theoretical calculation just slightly less reliable or much less reliable? Few people have the knowledge to answer that question with any authority.
- The rapid rotation of the pulsar renders it impossible for it to be a white dwarf (remember white dwarfs are simpler to model -- they would certainly fly apart if they rotated that fast, or so the experts say)
- A very simple energy calculation confirms the theoretical radius of a neutron
- Begin with the theoretical mass and radius of a neutron star.
- Use the observed rotation rate.
- Matter that is in motion has "kinetic energy". In the non-relativistic theory, the kinetic energy, KE=½mv2, where m is the mass of each atom and v is the speed. The relativistic calculation is almost as simple. Using calculus, one can take a solid spinning object (such as a bowling ball) and calculate the total kinetic energy, even though not all the atoms are moving at the same speed (the ones near the center have much less kinetic energy). The result of this calculation is the total kinetic energy of a pulsar. FYI, the formula is, , where M is mass, R is radius, and P is period.
- Another observable fact about pulsars is the rate at which they are slowing down. In other words we know how much energy is being lost by the pulsar every second. This energy has to go somewhere, and the spinning magnet delivers this power (mostly to to the electrons) in the surrounding Crab nebula.
- Finally, the total radiated energy of the Crab nebula has been measured. The Crab is emitting light at all wavelengths. And, it roughly matches the theoretical prediction.
Quasars (supermassive black holes?)[edit | edit source]
A very big universe[edit | edit source]
- There are 7 billion people on earth
- If you are "one in a million", there are 7,000 people on Earth just like you.
- If you divided up all the stars in the Milky way among all people alive today, each person on Earth would get about 40 stars.
- There at least half as many galaxies in the universe as there are stars in the Milky Way.
A surprisingly young universe[edit | edit source]
- One in 2.75×1045 are the odds that a monkey typing randomly on a typewriter (lock in capital letters) would type the sentance: "TO BE OR NOT TO BE, THAT IS THE QUESTION."
- Suppose there were 7 billion monkeys for every star in the universe. That would be 4.2×1032 monkeys. If these monkeys typed at a rate of one sentence every second for the age of the universe (13 billion years), then this sentence will get typed approximately 60 times.
- How did life evolve in this short time?
Hubble's Law[edit | edit source]
Recall that the standard candle is an object of known luminisoty, which permits distance to be calculated from the relative magnitude (i.e. light intensity as seen from Earth).