1. Neutron Star Observation Facts
The mass of a neutron star is generally between 1.35 and 2.1 times the mass of the sun, but its diameter is only about 10 kilometers. Neutron stars have some significant characteristics: high density, high rotation speed, strong magnetic field, and strong radiation. Many neutron stars exist in the form of pulsars and regularly emit electromagnetic waves outward. This phenomenon is because the rotation axis of the neutron stars does not coincide with their magnetic axis, causing their powerful magnetic field to continuously accelerate the charged particles, thus forming radiation. The most famous pulsars, such as those in the Crab Nebula, can send hundreds of signals per second.
In 1932, James Chadwick discovered neutrons, and in the same year, Soviet physicist Lev Landau predicted neutron stars. In 1934, Bard and Zwicky believed that supernova explosions could transform an ordinary star into a neutron star, and pointed out that this process could accelerate particles and produce cosmic rays. In 1939, Oppenheimer and Volkov established the first quantitative neutron star model. In 1967, Joselene Bell, a graduate student at Professor Hueysh of Cambridge University, first discovered the pulsar. Pulsars are generally observed by radio telescopes. The largest radio telescope in the world is the 500-meter aperture spherical radio telescope (FAST) located in Guizhou, China. As of November 2024, the number of pulsars discovered by FAST has exceeded 1,000. Some scholars estimate that the total number of neutron stars in the Milky Way should be at least more than 200,000. As of August 2023, there have been more than 3,000 pulsars discovered by humans in the Milky Way. One of the more famous ones is a pulsar in the center of the Crab Nebula. In 2007, astronomers used the European Aviation Agency (ESA) Gamma Ray Telescope to discover the fastest-rotating neutron star to date. This neutron star is numbered XTE J1739-285 and can rotate 1122 turns along its axis per second. The neutron star has a diameter of about 10 kilometers, but its mass is similar to that of the sun, and its density is as high as 100 million tons per cubic centimeter. Its huge gravity continuously captures a large amount of hot gas from adjacent stars and continuously induces a thermal nuclear explosion. On October 27, 2010, the British Daily Telegraph reported that astronomers discovered the largest neutron star in the universe to date, with a mass almost twice that of the sun. This neutron star is named PSR J1614-223.
The basic principles of general relativity tell us that large-mass objects will cause the bending of space and time. The mass of a neutron star is usually 1-2 times the mass of the sun, and the radius is about 10-20 kilometers, which will form an extremely strong gravitational field near it. When light passes near neutron stars, it should bend to form a gravitational lens. Currently, the observations involving curved light of neutron stars mainly include the following points:
(1) Self-luminous bending: When the light emitted by the neutron star itself escapes the surface, it will also bend due to a strong gravitational field. This causes the observer to see both its front and part of its back area, making the visual size of the neutron star larger than the actual physical size. This is just a situation of speculation by traditional theory, and no specific case reports have been found.
(2) X-ray halo:
Figure 1 is a photo of the ring structure composed of a bright X-ray source found by the Chandra
X-ray Observatory in galaxy AM0644. This structure is inferred by the gravitational lensing effect of neutron stars or black holes. AM 0644-741 is a special ring galaxy observed by the Hubble Space Telescope. It is located in the direction of the Constellation Flying Fish in the South. It is about 300 million light-years away from us and has a diameter of 150,000 light-years, about 1.5 times that of the Milky Way. Through multi-band observation data, it was shown that the celestial body was originally a normal spiral galaxy, and was later formed by a violent galaxy collision. When galaxies collide, they will pass through each other, but the stars inside rarely come into contact, and interstellar clouds and dust will be compressed, triggering the birth of wavy stars, and gradually spreading outward with the impact as the starting point, forming a landscape similar to the ripples of ponds expanding outward. The bright ring-like structure of blue star clusters in the picture orbits the central yellow nuclear sphere. Obviously, the brilliant ring-like structure formed by the blue star cluster is related to the central yellow nuclear sphere. There is no observational evidence of neutron stars or black holes here.
(3) Companion star orbit attenuation: Observation examples of neutron stars bending space-time can be verified by observing the interaction between neutron stars and companion stars. For example, scientists observed the interaction between the neutron star PSRJ0348+0432 and its companion star white dwarf. The neutron star is about twice the mass of the Sun, wrapped in a sphere with a diameter of less than 13 miles (20.92 kilometers) and rotates very quickly, 25 turns per second. PSRJ0348+0432 and its companion star, the white dwarf, form a binary galaxy, and the period of mutual orbit is 144 minutes. By observing the orbital motion of binary galaxies, scientists found that the orbits were attenuating, and their energy loss was consistent with the gravitational wave radiation predicted by general relativity, indirectly confirming the space-time bending effect. This is just the attenuation of the orbits of neutron stars and companion stars, and there is no direct evidence that neutron stars bend light.
(4) Gravitational time delay effect: Pulsars are fast-rotating neutron stars with very stable rotation periods and strong electromagnetic radiation. Their signal cycle accuracy can even exceed the atomic clock, making pulsars an ideal tool for studying strong gravitational field effects. When the signal emitted by a pulsar passes through a strong gravitational field during propagation, it will be bent and lead to a delay in propagation time. This phenomenon is the gravitational time delay effect. Here is the pulsar signal being bent, not the neutron star being bent.
(5) The large sway of the rotation axis of the neutron star. The double-pulse galaxy J1906 is about 25,000 light-years away from the Earth, and the frequency of radio waves is once every 144 milliseconds. Pulsars rotate around their companion stars and rotate around within 4 hours. Each neutron star in a double neutron galaxy is larger than the Sun, but the distance between the two neutron stars is very short, 100 times shorter than the distance between the Earth and the Sun. The two neutron stars have very large mass, are very close to each other, and have extremely strong gravitational effects, causing the rotation axis of the neutron stars to sway greatly. This swing phenomenon shows that the two neutron stars rotate along each other’s orbits. Under the action of the gravitational well, neutron stars or pulsars actually travel along the curved space-time, and the curved space-time affects the rotation axis of the neutron stars. The gravitational well has a huge gravitational dragging effect on neutron stars, and the rotation axis of neutron stars or pulsars has swung greatly. The prediction of gravity on space-time bending in general relativity is further confirmed. This is just the role between two neutron stars, not the direct evidence of the curved light of neutron stars.
(6) Gamma ray bursts around neutron stars: Because of their super high mass and rotation speed, neutron stars will periodically radiate powerful energy into the universe (gamma ray burst). By analyzing these gamma-ray bursts, scientists were able to determine the location of neutron stars and further study the space-time bending phenomenon around them. This is not direct evidence of neutron stars’ curved light.
(7) Companion star rotation acceleration: PSR B1937+21 is a millisecond pulsar discovered in the constellation Fox in 1982 by the team of American astronomer Donald Baker. The rotation period of the celestial body is 1.558 milliseconds, and it rotates about 642 turns per second. As a neutron star wreck, PSR B1937+21 generates periodic electromagnetic pulse signals through a high-speed rotating magnetic field, with an upper mass limit of 1,000 times that of the earth. Its rotation stability is close to the atomic clock accuracy, and its periodic deceleration rate reaches the order of milliseconds for a billion years, and can be used as a reference for long-term cosmic timing. Observations show that its accretion of substances with its companion star may cause acceleration of rotation, and the magnetic field intensity is about 4 orders of magnitude lower than that of conventional pulsars. This is just the acceleration of rotation of the neutron star companion star, and it is not direct evidence of the curved light of the neutron star.
Generally, neutron stars have particularly high density. A neutron star with a diameter of 10km has a mass greater than the sun. According to Newton’s law of universality, gravity is proportional to mass. The gravity of a neutron star with a 10km is also greater than that of the sun. According to Einstein’s gravitational lens, the degree of gravitational bending light is proportional to the planet’s gravity. Therefore, the degree of bending light of neutron stars should be greater than that of the sun. At present, more than 3,000 neutron stars have been found, and it should be easy to observe the bending light of neutron stars. However, the fact is that there is no direct evidence of bending light of neutron stars so far.