Luminosity of the Rigel star in the Orton constellation is 17000 times that of our sun. If the surface temperature of the sun is 6000 K, calculate the temperature of the star.
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- 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.A star has a peak output at 440 nm and has a luminosity of 3 solar luminosities. What is its radius? (LS=3.826 X 1026 J/s)Betelgeuse is a nearby supergiant that will eventually explode into a supernova. Let's see how awesome it would look. At peak brightness, the supernova will have a luminosity of about 10 billion times the Sun. It is 600 light-years away. All stellar brightnesses are compared with Vega, which has an intrinsic luminosity of about 60 times the Sun, a distance of 25 light-years, an absolute magnitude of 0.6 and an apparent magnitude of 0 (by definition). a) At peak brightness, how many times brighter will Betelgeuse be than Vega? b) Approximately what apparent magnitude does this correspond to? c) The Sun is about -26.5 apparent magnitude. What fraction of the Sun's brightness will Betelgeuse be?
- Calculate the luminosity of the star with an apparent magnitude of 2. Given the Sun has an apparent magnitude of -26.57 and 3.9 × 1026 W luminosity.I need the answer as soon as possible(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.
- Question A4 a) A star has a temperature T = 15000K, mass M = 0.25M and luminosity L = 0.02L. Sketch the position of this star on the Hertzsprung-Russell diagram relative to the main sequence. b) Using the given properties of the star, derive expressions for the star's radius R and mean density p. Calculate values for these in units of R. and kg m-³, respectively. c) Starting from the equation for hydrostatic equilibrium, derive an approximate expression for the central pressure Pc of the star in terms of its density p and radius R, assuming uniform ρ density. d) Assuming that the star is made of ordinary gas material such as the Sun, calculate an estimate of the central temperature of the star. From this value and the luminosity, briefly explain what can be inferred about the nuclear processes in the star. Discuss very briefly why your estimate for the central temperature may be too large.The star Rigel has a radial velocity r = 20.7km s-1, parallax 700 = 4.22mas, and proper motion components la= 1.67mas yr'in right ascension and us = 0.56mas yr1 in declination. What are its total proper motion, %3D %3D %3D tangential velocity, and space motion?(Answer don't copy with hand written please)As a star runs out of hydrogen to fuel nuclear fusion in its core, changes within the star usually cause it to leave the main sequence, expanding and cooling as it does so. Would a star with a radius 12 times that of the Sun, but a surface temperature 0.5 times that of the Sun, be more, or less luminous than the Sun? Show and explain your reasoning. You may assume the surface area of a sphere is A = 4πr2.