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Chapter 16: Problem 29

T Coronae Borealis is a well-known recurrent nova. a. Is it a single star or a binary system? Explain. b. What mechanism causes a nova to flare up? c. How can a nova flare-up happen more than once?

Short Answer

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a) T Coronae Borealis is a binary system. b) It flares up due to hydrogen accumulation and nuclear fusion. c) Recurrent flare-ups occur because mass transfer continues.

Step by step solution

01

- Identify the Type of System

T Coronae Borealis is a recurrent nova. A nova is a type of stellar explosion that occurs within a binary star system, involving a white dwarf and a companion star.
02

- Determine the Flare-Up Mechanism

A nova flare-up occurs when hydrogen from the companion star accumulates on the surface of the white dwarf. As the hydrogen layer grows thicker, it eventually reaches high temperatures and pressures, leading to nuclear fusion and a sudden release of energy, causing the nova to flare up.
03

- Explain Recurrent Flaring

A nova can flare up more than once because the process of mass transfer from the companion star to the white dwarf can continue. As new hydrogen accumulates over time, the conditions for another nova event can be met again, leading to recurrent nova outbursts.

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Key Concepts

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

Binary Star Systems
T Coronae Borealis is part of a binary star system, which means it consists of two stars orbiting a common center of mass. These systems can contain various types of stars, but in the case of recurrent novae like T Coronae Borealis, they usually include a white dwarf and a companion star:
  • The companion star can be a main-sequence star, a red giant, or even another white dwarf.
  • The two stars are gravitationally bound, meaning they are in a continuous orbital interaction.
Binary star systems are essential for the phenomena of novae because the interaction between the two stars leads to the transfer of material. This material transfer is crucial for the occurrence of novae and other explosive events.
White Dwarf Accretion
White dwarf stars are remnants of stars that have exhausted their nuclear fuel. They are incredibly dense and have strong gravitational fields. In a binary star system, the white dwarf can pull material from its companion star in a process known as accretion:
  • Material, primarily hydrogen, is pulled from the companion star and forms an accretion disk around the white dwarf.
  • This material gradually spirals inward and accumulates on the surface of the white dwarf.
  • The growing layer of hydrogen on the white dwarf's surface eventually becomes hot and dense enough to ignite nuclear fusion.
The build-up of this material is what can lead to the explosive events we observe as novae.
Nuclear Fusion in Novae
The flare-ups observed in recurrent novae like T Coronae Borealis are the result of nuclear fusion. This process takes place under extreme conditions:
  • As hydrogen accretes onto the white dwarf, the pressure and temperature in the hydrogen layer increase.
  • When the conditions are right, thermonuclear fusion of hydrogen into helium ignites explosively.
  • This fusion releases a tremendous amount of energy in a very short time.
  • The sudden release of energy causes the brightness of the star system to increase dramatically, which is observed as a nova flare.
Because the mass transfer from the companion star can continue, hydrogen can accumulate again after a flare, leading to subsequent nova events. This cyclical process explains why some novae, such as T Coronae Borealis, are recurrent.

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