Warning: foreach() argument must be of type array|object, bool given in /var/www/html/web/app/themes/studypress-core-theme/template-parts/header/mobile-offcanvas.php on line 20

Fate of an \(X\) -Ray Binary. The X-ray bursts that happen on the surface of an accreting neutron star are not powerful enough to accelerate the exploding material to escape velocity. Predict what will happen in an X-ray binary system in which the companion star eventually feeds over 3 solar masses of matter into the neutron star's accretion disk.

Short Answer

Expert verified
The neutron star will collapse into a black hole after accreting over 3 solar masses.

Step by step solution

01

Understanding X-ray Binary Systems

An X-ray binary is a system in which a normal star orbits a compact object like a neutron star or black hole. As matter from the star is drawn towards the compact object, it forms an accretion disk and emits X-rays as it is heated.
02

Comprehending the Effects of Accretion

In X-ray binaries, the neutron star can accumulate, or 'accrete', matter from its companion star. This increases the total mass of the neutron star. Typically, neutron stars have a mass slightly above 1.4 solar masses, known as the Chandrasekhar limit.
03

Analyzing Mass Increase

If the neutron star accumulates 3 solar masses of matter, this would increase its total mass significantly. Neutron stars have an upper mass limit, known as the Tolman–Oppenheimer–Volkoff (TOV) limit, which is around 2 to 3 solar masses.
04

Predicting the Outcome

When the accreted mass causes the neutron star to exceed the TOV limit, it can no longer remain stable. The gravitational force will overwhelm the neutron degeneracy pressure, leading to the collapse of the neutron star into a black hole.
05

Conclusion

Extra 3 solar masses can lead the neutron star to surpass its stability threshold, transforming it into a black hole. This process follows the fundamental principles of stellar evolution and gravitational physics.

Unlock Step-by-Step Solutions & Ace Your Exams!

  • Full Textbook Solutions

    Get detailed explanations and key concepts

  • Unlimited Al creation

    Al flashcards, explanations, exams and more...

  • Ads-free access

    To over 500 millions flashcards

  • Money-back guarantee

    We refund you if you fail your exam.

Over 30 million students worldwide already upgrade their learning with Vaia!

Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Neutron Stars
Neutron stars are incredibly dense remnants of massive stars that have undergone supernova explosions. These celestial objects are known for their extreme density and are primarily composed of neutrons, subatomic particles found in atomic nuclei. After a supernova explosion, if the core of the star has a mass between approximately 1.4 and 3 solar masses, it will collapse into a neutron star. This threshold is defined by the Chandrasekhar limit, which is the maximum mass a white dwarf star can have before collapsing under its gravity.

Neutron stars have a radius of about 10 kilometers but hold a mass greater than that of our Sun. This leads to extremely high gravitational and magnetic fields. Their extreme density means a sugar-cube-sized amount of neutron-star material would weigh the same as a mountain on Earth.

In X-ray binary systems, neutron stars play a crucial role due to their ability to accrete matter from a companion star. This accreting matter forms an accretion disk, eventually emitting X-rays. Understanding how these systems evolve helps scientists explore not only the properties of neutron stars but also fundamental aspects of general relativity and high-energy astrophysics.
Accretion Disks
Accretion disks form around massive celestial objects like neutron stars and black holes in processes involving the gravitational pull of matter. When a star in a binary system loses material to its massive companion, this material orbits the dense object, forming a flattened disk that spirals inwards.

Accretion disks are fascinating due to their role in the conservation of angular momentum. As matter spirals closer to the neutron star, it speeds up, creating friction and therefore heat, which causes the disk to glow, often emitting X-rays. This makes them prominent in the study of X-ray binary systems, as these emissions are critical for observing and understanding these complex systems.

The exact structure and dynamics of an accretion disk can provide insight into the characteristics and behaviors of both the disk itself and the central neutron star, helping astronomers determine factors like size, mass, and rotation speeds. This ongoing study assists in piecing together the lifecycle of stars and the evolution of galaxies.
Tolman–Oppenheimer–Volkoff Limit
The Tolman–Oppenheimer–Volkoff (TOV) limit defines the maximum mass a neutron star can have before collapsing under its gravity into a black hole. Named after physicists Robert Oppenheimer, and George Volkoff, this limit is a crucial concept in astrophysics and helps explain the formation of black holes.

Neutron stars hold themselves up against gravitational collapse with a quantum force known as neutron degeneracy pressure. The TOV limit is reached when this pressure can no longer counterbalance the gravitational force due to the star's large mass. Current estimates place the TOV limit between 2 and 3 solar masses.

Surpassing this limit in an X-ray binary system, as seen when a neutron star accretes excess matter, leads to catastrophic consequences. The ensuing collapse is not a gradual process; it happens rapidly when a neutron star's mass increases beyond the limit. This results in the transformation of the star into a black hole, a process connected to extreme gravitational physics and fundamental stellar evolution principles.

One App. One Place for Learning.

All the tools & learning materials you need for study success - in one app.

Get started for free

Most popular questions from this chapter

Each story should be detailed and scientifically correct but also creative. That is, it should be entertaining while at the same time showing that you understand stellar evolution. Be sure to state whether "you" are a member of a binary system. You are a neutron star of \(1.5 M_{\text {Sun }}\)

Describe the mass, size, and density of a typical neutron star. What would happen if a neutron star came to your hometown?

Surviving the Plunge. The tidal forces near a black hole with a mass similar to that of a star would tear a person apart before that person could fall through the event horizon. Black hole researchers have pointed out that a fanciful "black hole life preserver" could help counteract those tidal forces. The life preserver would need to have a mass similar to that of an asteroid and would need to be shaped like a flattened hoop and placed around the person's waist. In what direction would the gravitational force from the hoop pull on the person's head? In what direction would it pull on the person's feet? Based on your answers, explain in general terms how the gravitational forces from the "life preserver" would help to counteract the black hole's tidal forces.

Be sure to show all calculations clearly and state your final answers in complete sentences. Schwarzschild Radii. Calculate the Schwarzschild radius (in kilometers) for each of the following. a. \(10^{8} M_{\text {Sun }}\) black hole in the center of a quasar b. \(5 M_{\text {Sun }}\) black hole that formed in the supernova of a massive star c. \(A\) mini-black hole with the mass of the Moon d. A mini-black hole formed when a superadvanced civilization decides to punish you (unfairly) by squeezing you until you become so small that you disappear inside your own event horizon

Choose the best answer to each of the following. Explain your reasoning with one or more complete sentences. Which of these binary systems is most likely to contain a black hole? (a) an X-ray binary containing an O star and another object of equal mass (b) a binary with an X-ray burster (c) an X-ray binary containing a G star and another object of equal mass

See all solutions

Recommended explanations on Physics Textbooks

View all explanations

What do you think about this solution?

We value your feedback to improve our textbook solutions.

Study anywhere. Anytime. Across all devices.

Sign-up for free