5) A nova can occur when a white dwarf, which is the dense core of a once-normal star, "steals" gas from its nearby companion star. When enough gas builds up on the surface of the white dwarf it triggers an explosion of rapid hydrogen fusion (think of this as a hydrogen flash). Assuming Enova - 1038 joules and all this energy is coming from hydrogen fusion, estimate how much mass used in this process.
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- 1) a) Calculate the Jeans length for the dense core of a giant molecular cloud with T=10 K, n = 1010/m³, and µ=2. b) Estimate the adiabatic sound speed for this core, using y=5/3. c) Use this speed to find the amount of time required for a sound wave to cross the cloud t3=2Rj/vs. d) Compare your answer with the free-fall scale and comment your results.A main sequence star of mass 25 M⊙has a luminosity of approximately 80,000 L⊙. a. At what rate DOES MASS VANISH as H is fused to He in the star’s core? Note: When we say “mass vanish '' what we really mean is “gets converted into energy and leaves the star as light”. Note: approximate answer: 3.55 E14 kg/s b. At what rate is H converted into He? To do this you need to take into account that for every kg of hydrogen burned, only 0.7% gets converted into energy while the rest turns into helium. Approximate answer = 5E16 kg/s c. Assuming that only the 10% of the star’s mass in the central regions will get hot enough for fusion, calculate the main sequence lifetime of the star. Put your answer in years, and compare it to the lifetime of the Sun. It should be much, much shorter. Approximate answer: 30 million years.The Local Bubble is: a. a region of low density intersteller gas extending several hundred LY around the Sun b. a region around any exploding star where material is expanding from the explosion c. the region around very hot stars where hydrogen is ionized
- What is the average density of a neutron star that has the same mass as the sun but a radius of only 20.0 km if the radius of the neutron star is 57.999 km?(a) Estimate the Eddington luminosity of a 0.072 M, star and compare your answer to the main-sequence luminosity given in Problem 21. Assume k = 0.001 m² kg¯'. Is radia- tion pressure likely to be significant in the stability of a low-mass main-sequence star? (b) If a 120 Mo star forms with log1o T. = 4.727 and log1o(L/Lo) = 6.252, estimate its Eddington luminosity. Compare your answer with the actual luminosity of the star.1: Briefly explain what are neutron stars and then estimate the escape velocity of a neutron star.
- (Astronomy) Neutron Star Escape Velocity. What is the escape velocity at the surface of a 2.80-solar-mass neutron star that has a typical radius for this type of star? Express your answer in units of km/s.8) A neutron star is found with a radius of 10 km and has a surface temperature of 1,000,000 K. Calculate its luminosity with respect to that of the Sun. nts)2) How does the mean density of a 1.5 Mo neutron star compare to a carbon nucleus? Assume the carbon nucleus has a radius r=3 x 10–15 m.
- When the Sun becomes a red giant, it's luminosity will be 2000 times its current value. The solar flux at Earth will also increase by a factor of 2000. Neglecting the greenhouse effect, the surface temperature of the earth is determined by thermal equilibrium: the flux of radiation absorbed equals the flux of radiation emitted. This means the Earth's surface flux must also increase by a factor of 2000. If the current average surface temperature is 58 degrees F, what will the average surface temperature be when the Sun is a red giant. Express your answer in units of degrees Fahrenheit. [Hint: Recall that the Stefan-Boltzmann law says that the flux F emitted by a blackbody is related to its surface temperature T (measured in Kelvins) is F=σT4 . Use this law in the form of a ratio, expressing T in Kelvins. Then convert back to Fahrenheit.]c) Derive the Schwarzschild criterion for the onset of convection in an ideal gas, namely d ln T d ln P 7-1 Y Explain all steps in your derivation, and justify any assumptions that you make. d) In a region of convective instability near the surface of a solar-type star of total mass M, the temperature and pressure are related approximately by the expression P KT5/2. Show that the temperature gradient for an ideal gas in hydrostatic = equilibrium in this convection zone is given by dT dr 2Gm(r)μ 5Rr² Further, assuming that the mass in the convection zone is small compared to M, show that at a depth h measured from the top of the convection zone, the temperature is approximately given by T = Ts + 2GMμ -h₂ 5RR² when his small compared to R, and Ts is the temperature at the top of the convection zone.