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Please either hand me solutions in class- or email them- Legibly handw.docx

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Please either hand me solutions in class- or email them- Legibly handw.docx

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Please either hand me solutions in class, or email them. Legibly handwritten or word- processed are fine. 1. Explain what is meant by the \'Chandrasekhar mass\' 2. State which is the odd one out from type la supernova, \'type II supernova\', \'classical nova, and \'X-ray burst, and explain why 3.State the three igredients necessary for a neutron star to appear as a radio pulsar. 4. Explain how planetary nebulae become so colorful. 5. Describe the main differences between an open cluster and a globular cluster.
Solution
Problem 1)
The Chandrasekhar mass limit is the maximum mass of a stable white dwarf star . The currently accepted value of the Chandrasekhar limit is about 1.4 times of solar mass (mass of our sun) and it is equal to approximately 2.765×10^30 kg.
White dwarfs resist gravitational collapse primarily through electron degeneracy pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star\'s core is insufficient to balance the star\'s own gravitational self-attraction. Consequently, a white dwarf with a mass greater than the limit is subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole. Those with masses under the limit remain stable as white dwarfs.
I hope this would be helpful. According to Chegg guidelines I can answer one question at a time so please post other questions separately ..
.

Please either hand me solutions in class, or email them. Legibly handwritten or word- processed are fine. 1. Explain what is meant by the \'Chandrasekhar mass\' 2. State which is the odd one out from type la supernova, \'type II supernova\', \'classical nova, and \'X-ray burst, and explain why 3.State the three igredients necessary for a neutron star to appear as a radio pulsar. 4. Explain how planetary nebulae become so colorful. 5. Describe the main differences between an open cluster and a globular cluster.
Solution
Problem 1)
The Chandrasekhar mass limit is the maximum mass of a stable white dwarf star . The currently accepted value of the Chandrasekhar limit is about 1.4 times of solar mass (mass of our sun) and it is equal to approximately 2.765×10^30 kg.
White dwarfs resist gravitational collapse primarily through electron degeneracy pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star\'s core is insufficient to balance the star\'s own gravitational self-attraction. Consequently, a white dwarf with a mass greater than the limit is subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole. Those with masses under the limit remain stable as white dwarfs.
I hope this would be helpful. According to Chegg guidelines I can answer one question at a time so please post other questions separately ..
.

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Please either hand me solutions in class- or email them- Legibly handw.docx

  1. 1. Please either hand me solutions in class, or email them. Legibly handwritten or word- processed are fine. 1. Explain what is meant by the 'Chandrasekhar mass' 2. State which is the odd one out from type la supernova, 'type II supernova', 'classical nova, and 'X-ray burst, and explain why 3.State the three igredients necessary for a neutron star to appear as a radio pulsar. 4. Explain how planetary nebulae become so colorful. 5. Describe the main differences between an open cluster and a globular cluster. Solution Problem 1) The Chandrasekhar mass limit is the maximum mass of a stable white dwarf star . The currently accepted value of the Chandrasekhar limit is about 1.4 times of solar mass (mass of our sun) and it is equal to approximately 2.765×10^30 kg. White dwarfs resist gravitational collapse primarily through electron degeneracy pressure. The Chandrasekhar limit is the mass above which electron degeneracy pressure in the star's core is insufficient to balance the star's own gravitational self-attraction. Consequently, a white dwarf with a mass greater than the limit is subject to further gravitational collapse, evolving into a different type of stellar remnant, such as a neutron star or black hole. Those with masses under the limit remain stable as white dwarfs. I hope this would be helpful. According to Chegg guidelines I can answer one question at a time so please post other questions separately ..

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