A neutron star is a type of star that forms from the collapse of a larger star's material. Neutron stars form when the material of a larger star undergoes a gravitational collapse after a supernova, which causes the star's material to become very dense and generates enormous pressure. This pressure causes the atoms in the star to become very dense, so that the electrons are forced to move into the atomic nucleus. These atomic nuclei then turn into neutron nuclei, which form a neutron star.
Neutron stars are approximately 20 km in diameter, neutron stars can have a mass of up to 1-3 times greater than the mass of the sun. Its diameter is only tens of kilometers, making this star only the size of the Metropolitan city or Jakarta. Neutron stars have several types, namely Magnetars and Pulsars.
Neutron stars have a very large mass, but very small size. Neutron stars are also known as compact stars, because of their very small size. Neutron stars are also known as pulsars, because they periodically emit radio and X-rays.
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[“TYPES of Neutron Stars”]
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1. SINGLE STAR: A neutron star that forms after a star dies, has a mass of 1.4 or more and is less than 20 kilometers in diameter. It is a well-known neutron star because it is often used in time-jumping processes.
A single neutron star is a type of star consisting only of neutrons. Single neutron stars form when a star loses all of its outer mass in a supernova or other stellar mass jump. As a result, all that remains of the top of the star is high-pressure, largely invisible neutron matter.
Single neutron stars vary from relatively tiny to more than 20 times the mass of the sun. They also vary in properties and significant stress which causes them to be very compact and strong.
2. DOUBLE STAR: A double neutron star is made up of two types of neutron stars that usually revolve around each other around the center of the earth or a system called “orbitals”.
A double neutron star is a star consisting of two rotating neutron stars. A double neutron star is formed when two neutron stars collapse and then gravitationally pull on each other.
Multiple neutron stars usually have a mass greater than a single neutron star. In some cases, double neutron stars are even heavier than regular stars, although heavier does not mean bigger double neutron stars.
Double neutron stars are also considered as efficient sources of energy, namely through a process called proton-proton fusion. This process generates heat that helps prevent the double neutron star from collapsing.
3. PULSAR: is a type of neutron star which may be the result of a supernova or a single neutron star. Unlike other neutron stars, pulsars generate radio vibrations caused by their extremely fast rotation around the star. With a pulsar, you can see radio transmitters producing energy in the form of X-ray waves.
Pulsar is a star with a very high density. Pulsars have a super fast rotation period so that their speed can be said to be close to the speed of light
Pulsars can rotate tens to hundreds of times in just 1 second. Usually the names of Pulsars are abbreviated as PSR. For example, PSR B0329+54.
4. MAGNETAR: A magnetar is a type of neutron star that has a very strong magnetism. Their magnetism can be stronger than that of our planet. This allows them to release powerful magnetic energy, which can cause symptoms such as X-ray flares. Magnetars are also known for storing more magnetic energy than any other neutron star can create.
Magnetar names are shortened to SGR. For example, SGR 1806-20.
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[ "FORMATION 🛠️" ]
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The formation of a neutron star starts from the beginning when matter condenses in space through which the mass passes. This causes a new protoss star to form. This new star was formed from several initial layers, the outermost being the large hydrogen layer that surrounds the star. This layer is shifted by the force of gravity, forming a rather thin layer of helium around it. The energy released by the condensation of matter produces a second layer of plasma within it.
When the energy produced exceeds the amount of energy available, the high pressure in the plasma pushes the star to elongate. As plasma moves through the star's outer layers, it repairs the structure of the surrounding layers. This causes the helium layer to turn rather thinah becomes a stronger and thicker layer known as the AGB (Asymptotic Giant Branch) layer.
Once the star is in the AGB layer, the hydrogen and helium molecules will react with each other and turn the star into a neutron star. Then, the pressure due to the competition of protons and neutrons in the star will cause a supernova explosion which will send the material previously hidden in the star into space.
After a supernova explosion, the star will disappear from view, but contained within it is an object called a neutron star. This object is the end result of this process, a very compact neutron star and may contain black matter which is dark energy.
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[ “STRUCTURE & COMPOSITION 💧” ]
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The structure and composition of a Neutron Star is vast and complex. A neutron star is a compact and very dense astrophysical object with a mass of about 1.4 to 3 times that of the sun. Finally, most of its mass is concentrated at a much shorter distance than the diameter of a normal star like the Sun.
The nucleus of a neutron star is the compact part of the star, and is the driving force behind its main structure. The core consists of matter consisting of available and charged protons and neutrons by means of atomic forces. This matter dominates the gravitational physics and core dynamics of a neutron star, exposing the core to high pressures of neutron radiation and is called a neutron plasma.
The neutron star shell is the layer outside the core that controls the energy balance. It consists of successive dense layers containing atoms of heavy elements, each layer reducing the amount of positive charge of the nucleus through the decay of neutrons. This layer serves to maintain the internal fuzi balance of the neutron star and regulate its growth and stability.
The mantle of a neutron star is the layer between the core and shell which regulates the process of neutron decay and the electron diode system which synchronizes the neutron shell with deformation. This deformation creates the insulation of the wires so that the neutron star can trap light and float through space as a black object. About 5% of the mass of a neutron star is in this layer.
The neutron star envelope is the outer layer produced by the light and gas from the core. It includes a fraction of the star's mass up to 1.2 × 10^27 kilograms. It also has the beneficial application of mechanical stress to help maintain the neutron star's equilibrium.
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[ “ROTATION” ]
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The rotation of a neutron star refers to the rotational motion that is considered to be a feature of the mass distribution or called the inner seashore of a neutron star. This motion is responsible for the stability of the neutron star through a complex internal energy transfer mechanism into the gravitational stability. Usually, using the estimation of the general theory of relativity, it is assumed that the rotation of a neutron star rotates at a constant speed and is not disturbed by time throughout its lifetime. This rotation has a direct effect on the internal structure of the neutron star, including its contractility, mass distribution, and the star's gravitational pull. This also affects the emission and absorption patterns of the neutron star. In addition, there are several hypotheses that suggest that the population trend of neutron stars can be determined by the fiscality of rotation.
Neutron stars generally spin very fast after they form because of conservation of angular momentum; in analogy to the spinning ice skaters tugging at their arms, the slow rotation of a star's core usually speeds up as it contracts. A newborn neutron star can rotate many times in one second.
1. SLOW TURN: P - P-point (or P-Dot) diagrams for known rotational powered pulsars (red), anomalous X-ray pulsars(green), high energy emission pulsars (blue), and binary pulsars (pink)
Over time, the spin of the neutron star slows down, because the rotating magnetic field basically emits energy associated with rotation; older neutron stars may take a few seconds for each revolution. This is called a spin down. The slow rate of rotation of a neutron star is usually constant and very small.
The periodic time (denoted P) is the rotation period or time for one rotation of a neutron star. The spin-down rate, the rotational deceleration rate, is then given the symbol (P-dot), a derivative of P with respect to time. It is defined as the periodic increase in time per unit time; it is a dimensionless quantity, but it can be given in units of s⋅s−1 (seconds per second).
The spin-down rate (P-dot) of a neutron star is typically in the time range 10 l−22 to 10−9 s⋅s−1, with a shorter period (or faster rotation), observed neutron stars usually have a smaller P-dot. As a neutron star ages, its rotation continues to slow down (as it increases P); eventually, the rotational speed would become too slow to drive the radio emission mechanism, and the neutron star would no longer be detectable.
The P and P-dot allow an estimate of the minimum magnetic field of a neutron star. The P and P-dots can also be used to calculate the characteristic age of pulsars, but provide a somewhat larger estimate of their actual age when applied to young pulsars.
P and P -dot can also be combined with the moment of inertia/number of neutron stars to estimate a quantity called spin-down luminosity , which is given the symbol (E -dot). It is not the luminosity that is measured, but rather the calculated rotational energy loss rate which will calculate it in terms of radiation. For neutron stars in which the spin-down luminosity is proportional to the actual luminosity, the neutron star is said to be "rotation-driven". The observed luminosity of the Crab Pulsar is comparable to the spin-down luminosity, which supports the model that rotational kinetic energy drives radiation from it. With neutron stars such as magnetars, where the actual luminosity exceeds the spin-down luminosity by about a factor of one hundred, it is assumed that the luminosity is powered by magnetic dissipation, rather than being powered by rotation.
P and P -dots can also be plotted for a neutron star that makes a P - P- dot diagram. It encodes a large amount of information about the pulsar population and its properties, and has been likened to the Hertzsprung-Russell diagram in its importance to neutron stars.
2. SPIN: The rotational speed of a neutron star can increase, a process known as a spin up. Sometimes a neutron star absorbs orbiting material from a companion star, which can increase its rotation rate and reshape the neutron star like an oblate ball. This causes the rotation rate of the neutron star to increase to more than a hundred times per second in the case of millisecond pulsars.
The fastest rotating neutron star currently known, is PSR J1748-2446ad, with a rotation of 716 revolutions per second. However, a 2007 paper reported the detection of X-ray burst oscillations, which revealed an indirect number of spins, of 1122 Hz ( or 1122 spins) of the neutron star XTE J1739-285,which exhibits 1122 rotations per second. However, at present, this signal has only been seen once, and should be considered tentative until another outburst from the star is confirmed.
3. GLITCHES AND STARQUARQES: Occasionally, a neutron star will experience a glitch (glitch), which is a sudden small increase in its rotational speed or spin up. This disturbance is thought to be the effect of starquakes (or starquakes) — as the rotation of the neutron star slows down, it becomes more rounded in shape. Because the "neutron" crust is too rigid, this event causes the crust to fracture known as a discrete event, which creates starquakes that are similar to earthquakes. After a starquake, the star will have a much smaller equatorial radius, and because its angular momentum is conserved, its rotational speed increases.
Starquakes usually occur in a neutron magnetar star, which is thought to be the resulting fault, although the main hypothesis for the gamma-ray source is known as a soft gamma repeater.
A neutron star with a starquake, usually indicating that the starquake will not release enough energy to fault the neutron star; some suggest that this disturbance may be caused by the eddy transition in the theoretical superfluid core of the neutron star from a metastable to a lower energy state, thereby releasing energy that appears as the rotation rate increases.
4. ANTI-GLITCHES: small sudden drops in the rotational speed, or spin down, of a neutron star have also been reported. It so happened with magnetar 1E 2259+586, that in this one case, the process resulted in an increase in the X-ray luminosity by a factor of 20, and a significant change in the spin-down rate. Current models of neutron stars do not predict this behavior. If the cause is internal, it indicates a differential rotation of the dense outer crust and the superfluid component of the magnetar's inner layer structure.
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[ "RADIATION ☢️" ]
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Neutron star radiation is a type of radiation produced by a neutron star. A neutron star is an astrospheric object consisting of a frozen mass of neutrons at a high temperature. Neutron stars are the result of supernovae which cause the end product to be a neutron star. The radiation produced by a neutron star is in the form of electromagnetic waves consisting of X rays, radio waves, and gamma.
The radiation that stars produce g neutrons are an important part of the knowledge of cosmology, astrophysics, and astronomy. X-rays are the first generation of radiation produced by neutron stars. Other electromagnetic waves produced by neutron stars are radio and gamma waves. These two rays also play an important role in the process of fusion of neutron stars.
Neutron star radiation can also help illuminate the solar system, with X and gamma rays being emitted to the Earth's surface. In addition, the radiation produced by neutron stars can also be used to understand the physical mechanisms around neutron stars and outside the solar system.
1.PULSARS:
Neutron stars can be detected by their electromagnetic radiation. Neutron stars are usually observed in pulsed radio waves and other electromagnetic radiation, and neutron stars observed with pulses are called pulsars.
The pulsar's radiation is thought to be caused by the acceleration of particles near its magnetic poles, which do not need to be aligned with the neutron star's axis of rotation. It is thought that a large electrostatic field is generated near its magnetic poles, which causes the emission of electrons. These electrons are accelerated magnetically along field lines, causing curvature radiation, with radiation highly polarized toward the curvature plane. In addition, high-energy photons can interact with photons of lower energy and the magnetic field produces an electron − positron pair, which through electron-positron annihilation causes a further higher-energy photon.
The radiation originating from the magnetic poles of a neutron star can be described as magnetospheric radiation, referring to the magnetosphere of a neutron star. However, the magnetosphere with magnetic dipole radiation is often confused, magnetic dipole radiation is an emission of radiation with a frequency equal to the rotational frequency of the neutron star because the axis of the magnet is not parallel to the axis of rotation.
If the neutron star's axis of rotation were different from that of the magnet, researchers would only see these beams of radiation whenever the magnetic axis pointed toward it during the neutron star's rotation. Therefore, periodic pulsations are observed, at the same speed as the rotation of the neutron star.
2. A NON-pulsing NEUTRON STAR:
Pulsating non-pulsing neutron stars have also been identified, although they may have much smaller periodic luminosity variations. This appears to be a characteristic of X-ray sources known as Central Compact Objects in Supernova remnants, which are thought to be young , an isolated neutron star with a radio-quiet pulse.
3. RADIATION SPECTRUM:
This electromagnetic radiation spectrum includes visible light, near infrared, ultraviolet, X-rays and gamma rays. Pulsars observed in X-rays are known as X-ray pulsars if they are accretion-driven, whereas those identified in visible light are known as optical pulsars. The majority of detected neutron stars, including those identified in optical, X-ray, and gamma rays, also emit radio waves, an example that emits radio waves is the Crab Pulsar which produces electromagnetic emissions across the spectrum. However, there are neutron stars called quiet radio neutron stars, with no detectable radio emission.
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[ "POPULATION 👥" ]
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Currently, there are about 2,000 known neutron stars in the Milky Way and Magellanic Clouds, most of which have been detected as radio pulsars. Most of the discovered neutron stars are concentrated along the disk of the Milky Way, although the perpendicular scattering of the large disk due to supernova explosion processes can impart high translational speeds (400 km/s) to newly formed neutron stars.
Some of the closest known neutron stars are RX J1856.5−3754, which is about 400 light years from Earth, and PSR J0108−1431 about 424 light years. RX J1856.5-3754 is a member of a close group of neutron stars called The Magnificent Seven. Another nearby neutron star detected at the location of the constellation Ursa Minor has been nicknamed Calvera by its Canadian and American discoverers, after the name of the villain in the 1960 film The Magnificent Seven . This fast-moving object was found using the ROSAT/Bright Source Catalog.
Neutron stars are detectable only with modern technology during the very early stages of their life (almost always less than 1 million years) and are outnumbered by older neutron stars which can only be detected through black body radiation and gravitational effects on other stars.
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[ “OBSERVATION 🔭 ” ]
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A neutron star is a star consisting of a neutron nucleus with a very large relative mass. Neutron stars are in the final stages of evolution star and has a small radius of about 10 km. The presence of neutron nuclei in a neutron star makes it much denser than the air stars that have been observed. Neutron stars are also known to have high space speeds, so they can produce gravitational waves called panquation.
Observations and observations of neutron stars are carried out using available detection technology. This technology includes radiotelescopes, gamma shields, and X-ray detectors. Similar instrumentation can be used to detect jumping neutron beams as well as neutron stars. Observations can also reveal the location of the neutron star in the galaxy and the composition of its core. Knowledge about neutron stars can also be expanded by carrying out a spectroscopic analysis of the light they emit.
Observations made scientists take several examples of neutron stars, including:
1. The Black Widow Pulsar - a very massive millisecond pulsar. LGM-1 - the first known radio-pulsar.
2. PSR B1257+12 - the first neutron star found with a planet (millisecond pulsar).
3. PSR B1509−58 - source photo of "Hand of God" taken by Chandra X-ray Observatory.
4. PSR J0108−1431 - nearby neutron star. The Magnificent Seven, a group of dim isolated X-ray neutron stars nearby.
5. PSR J0348+0432 - the most massive neutron star with a limited mass, 2.01 ± 0.04M.
6. RX J0806.4-4123 - a source of infrared radiation neutron stars.
7. SWIFT J1756.9-2508 - a millisecond pulsar with a star-type companion with a planetary-distant mass (below the brown dwarf).
8. Swift J1818.0-1607 - the youngest neutron.
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[ “HISTORY 📖” ]
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At the meeting of the American Physical Society in December 1933 (proceedings published in January 1934), Walter Baade and Fritz Zwicky proposed the existence of a neutron star, less than two years after the discovery of the neutron by James Chadwick. In seeking an explanation for the origin of supernovas, they tentatively proposed that in a supernova explosion, an ordinary star turns into a star composed of very dense neutrons which they call a neutron star. Baade and Zwicky rightly proposed at the time that there was a release of the gravitational binding energy of the neutron star driving the supernova: "In the process of a supernova, a large amount of mass is annihilated". Neutron stars were thought to be too faint to be detected and little sighting was made of them until November 1967, when Francisco Pacini showed that neutron stars were rotating and had a strong magnetic field, so they would emit electromagnetic waves. Unbeknownst to him, radio astronomer Antony Hewish and his research assistant Jocelyn Bell in Cambridge immediately detected radio pulses from a star now believed to have a high magnetic field, a fast rotating neutron star, known as a pulsar.
In 1965, Antony Hewish and Samuel Okoye discovered "an unusual high-brightness radio temperature source in the Crab Nebula". This source turned out to be the Crab Pulsar which resulted from the massive supernova of 1054.
In 1967, Josif Shklovsky examined the X-ray and optical observations of Scorpius X-1 and correctly concluded that the radiation came from a neutron star in the accretion stage.
In 1967, Jocelyn Bell Burnell and Antony Hewish discovered regular radio pulses from PSR B1919+21. This pulsar is then interpreted as an isolated fast-spinning neutron star. The pulsar's energy source comes from the rotational energy of a neutron star. The majority of known neutron stars (about 2000, as of 2010) have been found to be pulsars, emitting ordinary radio waves.
In 1971, Riccardo Giacconi, Herbert Gursky, Ed Kellogg, R. Levinson, E. Schreier, and H. Tananbaum discovered a 4.8 second pulse in an X-ray source in the constellation Centaurus, Cen X-3. They interpreted this as a result of a hot rotating neutron star. The energy source is gravitational and is produced from a rain of gas that falls onto the surface of the neutron star from a companion star or the interstellar medium.
In 1974, Antony Hewish was awarded the Nobel Prize in Physics "for his decisive role in the discovery of the pulsar" without Jocelyn Bell participating in the discovery.
In 1974, Joseph Taylor and Russell Hulse discovered the first binary pulsar, PSR B1913+16, which consists of two neutron stars (one is seen as a pulsar) orbiting around its center of mass. Einstein's general theory of relativity predicted that large objects in short binary orbits should emit gravitational waves, and thus that their orbits should decrease with time. This was actually observed, just as general relativity predicted, and in 1993, Taylor and Hulse were awarded the Nobel Prize in Physics for this discovery. .
In 1982, Don Backer and colleagues discovered the first millisecond pulsar PSR B1937+21. This object rotates 642 times per second, a value that places fundamental limits on the mass and radius of a neutron star. Many millisecond pulsars were later discovered, but PSR B1937+21 remained the fastest rotating pulsar for 24 years, until PSR J1748-2446ad (which rotates more than 700 times per second) was discovered.
In 2003, Marta Burgay and colleagues discovered the first double neutron star system in which both components can be detected as a pulsar, PSR J0737−3039. The system's invention made possible a total of 5 different tests of general relativity, some of them with unprecedented precision.
In 2010, Paul Demorest and colleagues measured the mass of the millisecond pulsar PSR J1614−2230 to be 1.97 ± 0.04 M, using the Shapiro delay. This is substantially higher than the mass of a previously measured neutron star (1.67 M, see PSR J1903 +0327), and places strong limitations on the composition of the neutron star's interior.
In 2013, John Antoniadis and colleagues measured the mass of PSR J0348+0432 to be 2.01 ± 0.04 M, using white dwarf spectroscopy. This confirmed the existence of such a massive star using a different method. Furthermore, it is possible, for the first time, to test the theory of general relativity using such a massive neutron star.
In August 2017, LIGO and Virgo made the first detection of gravitational waves produced by colliding neutron stars.
In October 2018, astronomers reported that GRB 150101B, a gamma-ray burst event detected in 2015, may be directly related to the historic GW170817 and related to the merger of two neutron stars. The similarities between the two events, in terms of gamma, optical and x-ray emission, and the very "striking" nature of the host galaxy, suggest that the two separate events may have been the result of a merger. neutron stars, and both may experience kilonovas, which may be more common in the universe than previously understood, according to researchers.
In July 2019, astronomers reported that a new method for determining the Hubble constant, and resolving differences to previous methods, has been proposed based on the merger of a pair of neutron stars, following the detection of the merger of the neutron star GW170817. Their Hubble constant measurement is about 70.3+5.3−5.0(km/s)/Mpc.
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[ “SUMMARY 📑” ]
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• Neutron stars are stars formed by the death of other, larger stars.
• Neutron stars are stars that are very dense and have great pressure.
• Due to the density, the electrons in the neutron star are pushed into the atomic nucleus, and this nucleus turns into a neutron nucleus, and creates a neutron star.
• Neutron stars have a diameter of 20km.
• Neutron stars have a mass 3x greater than the mass of the sun.
• Neutron stars are very small, but have a greater mass than the sun because of the density between the particles.
• Neutron stars emit radio and X-rays periodically.
• Neutron stars have 4 types, namely "Single", "Double", "Pulsar", "Magnetar" stars.
• A single star is a type of neutron star which has a small size and a type of star which only consists of neutron particles.
• A single neutron star is formed as a result of a supernova phenomenon and a star that experiences a supernova ejects all of its outer mass, and all that's left are the neutrons.
• A double star is a type of neutron star which consists of two neutron stars rotating around an orbital system.
• Double neutron stars have a greater mass than single neutron stars.
• Double neutron stars are referred to as energy efficient sources, namely carrying out a process called proton-proton fusion, this process that produces heat and prevents this star from dying.
• Pulsars are a type of neutron star that generates radio vibrations.
• Pulsars rotate very fast, so fast they are close to the speed of light.
• The pulsar's name is shortened to psr. For example, PSR B0329+54.
• Magnetar is a type of neutron star that has a strong magnetism.
• The name of the magnetar is abbreviated as SGR. For example, SGR 1806-20.
• Neutron stars are created as a result of supernova phenomena from other stars.
• The structure and composition of a neutron star consists of "Core", "Skin", "Mantle", and "Outer Layer".
• The nucleus of a neutron star is made up of neutrons and protons.
• The nucleus of a neutron star becomes dominant over the gravity and dynamics of the star's core, and results in a high pressure of neutron radiation.
• Neutron star skin is a layer that controls the energy balance.
• The shell of the neutron star is outside the core.
• The shell of a neutron star is made up of atoms of heavy elements, and each layer sheds a positively charged nucleus through decay.
• Neutron star mantle is a layer that regulates the decay process.
• The neutron star's mantle is in the layer between the core and the shell.
• 5% of the mass of a neutron star is in the mantle.
• The outermost layer of a neutron star is a stellar covering made of light and gas.
• The envelope of a neutron star includes a star's mass up to 1.2x10^27.
• The star rotates very fast because of the conservation of angular momentum.
• Newly born neutron stars usually spin or rotate many times in one second.
• Neutron star rotation is divided into 4 categories, namely "Slow Spin", "Spin", "Spin Interference", and "Anti Interference".
• Slow spin is the slow rotation of a neutron star over time.
• The spin process is slow because the magnetic field is basically rotating.
• Spin is the process of increasing the speed of rotation by a neutron star.
• The process of rotating a neutron star is known as a spin up.
• The process of rotating the neutron star occurs because this star absorbs other matter.
• Disturbance is a process of rotation of a neutron star that is disturbed in rotation, and causes the rotational speed to decrease.
• These disturbances are known as starquakes.
• Disruption of the rotation of a neutron star is caused by a neutron crust that is too rigid, and causes the crust to crack.
• Anti-disturbance is the rotational process of a neutron star, in which a small instantaneous decrease in the rotational speed.
• Anti-disturbance is known as spin down.
• Neutron star radiation is radiation from a neutron star that produces electromagnetic waves consisting of X rays, radio waves, and gamma.
• Neutron star radiation is divided into 3 types, namely "Pulsars", "Throbbing Neutron Stars, and "Spectral Radiation.
• Pulsar radiation from a neutron star radiation is a type of radiation in which radio waves pulse and the neutron star is observed by its pulse.
• The pulsar's radiation pulse is caused by the acceleration of particles near the magnetic poles.
• Nonpulsating neutron star radiation is radiation in which the neutron star does not produce pulsations unlike pulsar radiation.
• Spectral radiation is a type of radiation from a neutron star, where this radiation produces visible light.
• It is known, the population of neutron stars can reach 2,000 in the Milky Way and early Magellan.
• The closest neutron star to Earth is RX J1856.5-3754, which is 400 light years away.
• Neutron stars can only be detected by modern technology.
• Technologies for observing neutron stars are radiotelescopes, gamma shields, and X-ray detectors.
• Examples of neutron stars are Pulsar Black Widow, and PSR B1257+12.
• Walter Baade and Fritz Zwicky were the first to discover a neutron star in 1934.
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