With a 14 solar mass star example. Describe how its position on an H-R diagram will change as it leaves the main sequence.
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With a 14 solar mass star example. Describe how its position on an H-R diagram will change as it leaves the main sequence.
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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.. 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.Match each statement with the appropriate item (If the first corresponds to B and the next 4 to C, enter BCCCC) 1) stars that have evolved off the main sequence and are growing in luminosity due to a hydrogen burning shell 2) young, spread out star cluster 3) cooler stars in a cluster that have not yet evolved off the main sequence 4) stars that are burning helium in their core 5) old, dense star cluster A. red-giant branch B. open cluster C. lower main sequence D. horizontal branch stars E. globular cluster
- A red giant that was originally a 9.5MSun main-sequence star loses a solar mass in 100,000 years via a superwind. What is this mass loss rate in units of solar masses per year? (the answer is not 0.000095 solar masses per year). Additionally, at this mass loss rate, what will the red giant's mass be after 0.5 million years? (Enter your answer as a multiple of MSun.)Match each characteristic below of a one-solar-mass star to its appropriate phase. Answer M for Main-sequence Star, or P for Protostar. If the first is M and the rest P, enterMPPPPPP). A) energy generated by nuclear fusion B) pressure and gravity are NOT precisely balanced. C) surface radiates energy at same rate that core generates energy D) radius much larger than the Sun E) energy generated by gravitational contraction F) lasts about 10 billion years G) luminosity much greater than the SunI need the answer as soon as possible
- In the star clusters shown, which one is younger and why?How often can a star go supernova? Group of answer choices Many times, depending on the size of its companion star. Twice, the first time when it runs out hydrogen, and the second time when it runs out of iron. Once, early in its evolution. Once, late in its evolution. At various times, depending on the composition of the star.Suppose 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. ]