Neutron stars rotate rapidly due to their conservation of angular momentum. When a massive star collapses into a neutron star, its core spins faster as it contracts. Since angular momentum is conserved, the neutron star continues to rotate rapidly as a remnant of the collapsed star.
The true statement is: "A pulsar requires that a neutron star rotates rapidly." Pulsars are rapidly rotating neutron stars with strong magnetic fields, which emit beams of electromagnetic radiation along their magnetic poles, leading to their characteristic pulsed signals as they rotate. The other conditions mentioned are not essential for a neutron star to become a pulsar.
Some neutron stars that emit pulses of radiation are known as pulsars. Pulsars rotate rapidly and emit beams of electromagnetic radiation from their magnetic poles, which are observed as regular pulses when they sweep across the Earth.
Neutron stars are born from massive stars collapsing, which conserves the original star's angular momentum. Since the original star had a slow rotation, the neutron star that forms from it will have a faster spin due to the conservation of angular momentum.
Rapid rotation: Neutron stars can spin incredibly fast, with some completing hundreds of rotations per second. Strong magnetic fields: Neutron stars have extremely powerful magnetic fields, magnitudes stronger than any other object in the universe, which can influence their behavior and emit radiation.
The connection between pulsars and neutron stars is explained by the generally accepted model that pulsars are rapidly rotating neutron stars that emit beams of radiation from their magnetic poles, causing periodic signals to be observed when the beams cross our line of sight. This emission of radiation is what gives rise to the pulsed nature of pulsar signals.
They rotate with an amazingly stable rotation rate.
The true statement is: "A pulsar requires that a neutron star rotates rapidly." Pulsars are rapidly rotating neutron stars with strong magnetic fields, which emit beams of electromagnetic radiation along their magnetic poles, leading to their characteristic pulsed signals as they rotate. The other conditions mentioned are not essential for a neutron star to become a pulsar.
Some neutron stars that emit pulses of radiation are known as pulsars. Pulsars rotate rapidly and emit beams of electromagnetic radiation from their magnetic poles, which are observed as regular pulses when they sweep across the Earth.
All young neutron stars spin rapidly. You might be confused with a pulsar. See related questions.
A pulsar is a rapidly spinning neutron star that releases regular pulses of electromagnetic radiation from its magnetic field
Revolve means they have to have something to revolve around. Do you mean rotate? [See related question] All neutron stars rotate due to the conservation of momentum. At birth they move incredibly quickly - sometimes a thousand times a second but as they age, they will slowly slow down.
Pulsars. They are very dense neutron stars that rotate quickly and very regularly, emitting radiation pulses towards the earth like a lighthouse.
Neutron stars are born from massive stars collapsing, which conserves the original star's angular momentum. Since the original star had a slow rotation, the neutron star that forms from it will have a faster spin due to the conservation of angular momentum.
A neutron star is the "end of the line" for a giant star that exploded as a supernova. The material in a neutron star is packed so densely that a chunk of it the size of a cigarette package would weigh thousands of tons. It spins rapidly, at a steady rate (they are sometimes called "radio beacon stars").
Stars actually do rotate.
Pulsars are rapidly rotating neutron stars that emit beams of electromagnetic energy. Neutron stars form when the core of a massive star collapses and goes supernova leaving behind a neutron star which will begin rotating and releasing energy.
Some massive stars will become neutron stars. When massive stars die they will either become neutron stars or black holes depending on how much mass is left behind.