Describe why numerical modelling of stellar structure requires both outward and inward integration calculations. Also, describe an iterative method to minimize the difference in the values of both outward and inward calculations.
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Describe why numerical modelling of stellar structure requires both outward and
inward integration calculations. Also, describe an iterative method to minimize the
difference in the values of both outward and inward calculations.
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- What is the life expectancy (in years) of a 10 M⊙ main-sequence star? What is the life expectancy (in years) of a 70 M⊙ main-sequence star?What is the relationship between the color of a reflection nebula and the color of the star that illuminates it?. The radius of the nebula is about 0.401 light-years. The gas is expanding away from the star at a rate of about 37 kilometers/second . Considering that distance = velocity x time, calculate how long ago the gas left the star if its speed has been constant the whole time. Make sure you use consistent units for time, speed, and distance. Answer in years.
- How can we know that the sun will “die” in about 5 billion years? Choose the correct answer. A. We can see the evolution and death in the spectra B. We can see the entire process as it plays out in a star C. We look at thousands of stars like the sun and can see them in all stages of developmentI need the answer as soon as possibleSuppose a protostar has a luminosity of 39,473 L⊙ and a surface temperature of 4,130 K (Kelvins). What is the radius of this protostar? [Enter your answer as a multiple of the Sun's radius. I.e., if you find R = 20 R⊙ , enter 20. This problem is easier if you start with the relevant equation and create a ratio using the Sun's values. Recall that the Sun has a surface temperature of 5778 K. ]