UNDERSTANDING THE UNIVERSE(LL)-W/CODE
3rd Edition
ISBN: 9780393869903
Author: PALEN
Publisher: NORTON
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 13, Problem 44QAP
To determine
To show size of Earth will be roughly the size of football field if it converted into a neutron star.
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solution
Students have asked these similar questions
How much energy would be released if a star with a mass of 25 Msun and a radius of 10 Rsun detonates as a supernova explosion in 1 second? (Hint: think about the definition of binding energy). Express your answer in terms of solar luminosities.
If Earth's moon were replaced by a neutron star with a radius of 13 km, what would the angular diameter of the neutron star be as seen from Earth? (Hint: Use the small-angle formula, angular diameter (in arc seconds) / 2.06 ✕ 105 arc seconds = linear diameter/distance, where the linear diameter and the distance both have the same units.)
If a neutron star has a radius of 11 km and rotates 1,366 times a second, what is the speed at which a point on the surface at the neutron star's equator is moving? Express your answer as a fraction of the speed of light. (Note: The speed of light is 3 x 10° km/s.)
Chapter 13 Solutions
UNDERSTANDING THE UNIVERSE(LL)-W/CODE
Ch. 13.1 - Prob. 13.1CYUCh. 13.2 - Prob. 13.2CYUCh. 13.3 - Prob. 13.3CYUCh. 13.4 - Prob. 13.4CYUCh. 13.5 - Prob. 13.5CYUCh. 13.6 - Prob. 13.6CYUCh. 13 - Prob. 1QAPCh. 13 - Prob. 2QAPCh. 13 - Prob. 3QAPCh. 13 - Prob. 4QAP
Ch. 13 - Prob. 5QAPCh. 13 - Prob. 6QAPCh. 13 - Prob. 7QAPCh. 13 - Prob. 8QAPCh. 13 - Prob. 9QAPCh. 13 - Prob. 10QAPCh. 13 - Prob. 11QAPCh. 13 - Prob. 12QAPCh. 13 - Prob. 13QAPCh. 13 - Prob. 14QAPCh. 13 - Prob. 15QAPCh. 13 - Prob. 16QAPCh. 13 - Prob. 17QAPCh. 13 - Prob. 18QAPCh. 13 - Prob. 19QAPCh. 13 - Prob. 20QAPCh. 13 - Prob. 21QAPCh. 13 - Prob. 22QAPCh. 13 - Prob. 23QAPCh. 13 - Prob. 24QAPCh. 13 - Prob. 26QAPCh. 13 - Prob. 27QAPCh. 13 - Prob. 28QAPCh. 13 - Prob. 29QAPCh. 13 - Prob. 30QAPCh. 13 - Prob. 31QAPCh. 13 - Prob. 32QAPCh. 13 - Prob. 33QAPCh. 13 - Prob. 35QAPCh. 13 - Prob. 36QAPCh. 13 - Prob. 37QAPCh. 13 - Prob. 38QAPCh. 13 - Prob. 39QAPCh. 13 - Prob. 40QAPCh. 13 - Prob. 41QAPCh. 13 - Prob. 43QAPCh. 13 - Prob. 44QAPCh. 13 - Prob. 45QAP
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- H II regions can exist only if there is a nearby star hot enough to ionize hydrogen. Hydrogen is ionized only by radiation with wavelengths shorter than 91.2 nm. What is the temperature of a star that emits its maximum energy at 91.2 nm? (Use Wien’s law from Radiation and Spectra.) Based on this result, what are the spectral types of those stars likely to provide enough energy to produce H II regions?arrow_forwardwhat is the answer for sub-item (b) if the radius of the neutron star is 90.651 km? (express your answer in the proper SI unit and without scientific notation)arrow_forwardA 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.arrow_forward
- What is the answer below if the radius of the neutron star is 29.894 km? (express your answer in the proper SI unit and without scientific notation) 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?arrow_forwardIn a star of 1 solar mass (M☉), the core hydrogen burning phase, also known as the main sequence phase, lasts for approximately 10 billion years. Suppose there's a star of 15 solar masses (M☉). Stars of higher mass burn through their hydrogen at a faster rate, following an approximate relation that the lifetime of a star on the main sequence (T) is proportional to its mass (M) raised to the power of -2.5 (T ∝ M^-2.5). Calculate approximately how long this 15 solar mass star would remain in the main sequence phase, compared to the 1 solar mass star.arrow_forwardwhat is the answer for sub-item (b) if the radius of the neutron star is 84.66 km?arrow_forward
- A molecular cloud is 22 pc in diameter and is located 303 pc from Earth. What is its angular size on the sky (in arc seconds)? The cloud has a density of n = 8,500 hydrogen molecules/cm³. What is the total mass of the cloud in solar masses? (Approximate the molecular cloud as spherical.)arrow_forwardFor a main sequence star with luminosity L, how many kilograms of hydrogen is being converted into helium per second? Use the formula that you derive to estimate the mass of hydrogen atoms that are converted into helium in the interior of the sun (LSun = 3.9 x 1026 W). (Note: the mass of a hydrogen atom is 1 mproton and the mass of a helium atom is 3.97 mproton. You need four hydrogen nuclei to form one helium nucleus.)arrow_forwardAssume that the mass of the core of a star that just went Supernova type II is $2.5 \mathrm{M}_{\odot}$ before and after the collapse, while the Radius changes from $10^3 \mathrm{~km}$, before the collapse, to 12 km , after the collapse respectively.(a) What is the change in potential energy of the core between the two stages before and after the collapse?(b) Knowing that the luminosity of the Sun is $4 \times 10^{26} \mathrm{~W}$ how many years would it take the Sun to release the same amount of energy?arrow_forward
- Use t = 1 M2.5 to compute the life expectancy of a 0.8-solar-mass star. (A solar lifetime is approximately 10 billion years.)arrow_forwardCalculate the total number density ( ntot ) and the density ( ρ ) at a depth in a star composed of pure hydrogen where T = 9500 K and 35 % of the atoms are ionized (assume UI = 2). What percentage of hydrogen atoms are in the energy level n = 2?arrow_forwardA star is transited by a planet. From the measured period T and the transit duration t alone, show that one can obtain an upper bound on the density of the transited star : rhomax= 3T/(G(pi2)(t3)). Hint: Combine Kepler's Law [(omega2)(a3)=GMstar and the equation t=((rstarT)/(pi*a))*(1-b2)1/2 to eliminate a, and then extract the density of the spherical star. The upper bound is obtained by assuming an impact parameter b=0.arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
Foundations of Astronomy (MindTap Course List)PhysicsISBN:9781337399920Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
Stars and Galaxies (MindTap Course List)PhysicsISBN:9781337399944Author:Michael A. SeedsPublisher:Cengage Learning
Stars and GalaxiesPhysicsISBN:9781305120785Author:Michael A. Seeds, Dana BackmanPublisher:Cengage Learning
AstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Foundations of Astronomy (MindTap Course List)
Physics
ISBN:9781337399920
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Stars and Galaxies (MindTap Course List)
Physics
ISBN:9781337399944
Author:Michael A. Seeds
Publisher:Cengage Learning
Stars and Galaxies
Physics
ISBN:9781305120785
Author:Michael A. Seeds, Dana Backman
Publisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax