Star like pulsar and neutron stars

### 300 Types of Stars and Cosmic Objects

Here is a numbered list of 300 astronomical objects, including neutron stars, pulsars, black holes, unusual stars, stellar remnants, and other objects related to stellar evolution. Important: these are not all separate types of stars; the list also includes subtypes, theoretical objects, and related cosmic phenomena.

### 1–50: Main Stars and Stellar Types

* Main-sequence star

* Protostar

* Pre-main-sequence star

* T Tauri star

* Herbig Ae/Be star

* O-type star

* B-type star

* A-type star

* F-type star

* G-type star

* K-type star

* M-type star

* Red dwarf

* Orange dwarf

* Yellow dwarf

* Blue dwarf (hypothetical stellar evolutionary stage)

* White star

* Blue-white star

* Red star

* Brown dwarf

* Sub-brown dwarf

* Ultracool dwarf

* Metal-poor star

* Metal-rich star

* Population I star

* Population II star

* Population III star (first-generation, theoretical)

* High-velocity star

* Hypervelocity star

* Runaway star

* Field star

* Binary star

* Triple star system

* Multiple star system

* Spectroscopic binary

* Eclipsing binary

* Visual binary

* Contact binary

* Detached binary

* Semidetached binary

* Symbiotic star

* Variable star

* Pulsating star

* Rotating variable star

* Eruptive variable star

* Flare star

* BY Draconis variable

* RS Canum Venaticorum variable

* Ellipsoidal variable

* R Coronae Borealis variable

### 51–100: Giant, Supergiant and Massive Stars

* Red giant

* Red-giant-branch star

* Horizontal-branch star

* Red-clump star

* Blue giant

* Blue supergiant

* Red supergiant

* Yellow supergiant

* White supergiant

* Luminous blue variable

* Wolf–Rayet star

* WN-type Wolf–Rayet star

* WC-type Wolf–Rayet star

* WO-type Wolf–Rayet star

* Wolf–Rayet binary

* Hypergiant

* Yellow hypergiant

* Red hypergiant

* Blue hypergiant

* Massive star

* Very massive star

* Extremely massive star

* Chemically peculiar star

* Ap star

* Bp star

* Am star

* HgMn star

* Lambda Boötis star

* Carbon star

* S-type star

* Barium star

* CH star

* CEMP star

* Technetium-rich star

* Lithium-rich giant

* R-type carbon star

* N-type carbon star

* J-type carbon star

* Hydrogen-deficient star

* Helium star

* Extreme helium star

* Subdwarf B star

* Subdwarf O star

* Hot subdwarf

* Blue straggler

* SX Phoenicis variable

* Delta Scuti variable

* Gamma Doradus variable

* Slowly pulsating B star

* Beta Cephei variable

### 101–150: Pulsars, Neutron Stars and Compact Remnants

* Neutron star

* Pulsar

* Radio pulsar

* Millisecond pulsar

* X-ray pulsar

* Gamma-ray pulsar

* Optical pulsar

* Accreting pulsar

* Rotation-powered pulsar

* Recycled pulsar

* Binary pulsar

* Isolated pulsar

* Young pulsar

* Old pulsar

* Magnetar

* Anomalous X-ray pulsar

* Soft gamma repeater

* Central compact object

* Compact central X-ray source

* Accreting neutron star

* Neutron-star merger remnant

* Neutron star with a fallback disk

* Transitional millisecond pulsar

* Black widow pulsar

* Redback pulsar

* Double neutron-star system

* Neutron-star–white-dwarf binary

* Neutron-star–black-hole binary

* Thorne–Żytkow object (hypothetical)

* Strange star (hypothetical)

* Quark star (hypothetical)

* Hybrid star (hypothetical)

* Electroweak star (hypothetical)

* Boson star (hypothetical)

* Gravastar (hypothetical)

* White dwarf

* Carbon–oxygen white dwarf

* Helium white dwarf

* Oxygen–neon white dwarf

* Magnetic white dwarf

* Nonmagnetic white dwarf

* Pulsating white dwarf

* ZZ Ceti star

* V777 Herculis star

* GW Vir star

* Hot white dwarf

* Cool white dwarf

* Crystallized white dwarf

* Merger-produced white dwarf

* White-dwarf binary

### 151–200: Black Holes and Black-Hole Systems

* Stellar-mass black hole

* Intermediate-mass black hole

* Supermassive black hole

* Ultramassive black hole

* Primordial black hole (hypothetical)

* Isolated black hole

* Binary black hole

* Triple black-hole system

* Accreting black hole

* Non-accreting black hole

* Rotating Kerr black hole

* Nonrotating Schwarzschild black hole

* Charged Reissner–Nordström black hole (idealized)

* Charged rotating Kerr–Newman black hole (idealized)

* Black hole with an accretion disk

* Black hole with a relativistic jet

* Dormant black hole

* Wandering black hole

* Recoiling black hole

* Merging black holes

* Black-hole merger remnant

* Black hole in an X-ray binary

* Black hole in a microquasar

* Black hole in an active galactic nucleus

* Quasar-hosting black hole

* Blazar-hosting black hole

* Seyfert-galaxy black hole

* Radio-galaxy black hole

* Tidal-disruption-event black hole

* Black hole in a globular cluster

* Black hole in a nuclear star cluster

* Black hole in a dwarf galaxy

* Black hole in a spiral galaxy

* Black hole in an elliptical galaxy

* Black hole in a galaxy merger

* Seed black hole

* Direct-collapse black hole

* Population III remnant black hole

* Stellar-collapse black hole

* Supernova-produced black hole

* Failed-supernova black hole

* Black hole with a fallback disk

* Black hole with a circumbinary disk

* Black hole with a warped accretion disk

* Black hole with a dusty torus

* Black hole with a magnetized disk

* Black hole in a hierarchical triple

* Black hole–neutron star binary

* Black hole–white dwarf binary

* Black hole–main-sequence star binary

### 201–250: Explosive, Evolved and Unusual Stellar Objects

* Classical nova

* Recurrent nova

* Dwarf nova

* Symbiotic nova

* Type Ia supernova

* Type Ib supernova

* Type Ic supernova

* Type II supernova

* Type IIP supernova

* Type IIL supernova

* Type IIn supernova

* Type IIb supernova

* Superluminous supernova

* Pair-instability supernova

* Pulsational pair-instability event

* Electron-capture supernova

* Fallback supernova

* Failed supernova

* Hypernova

* Kilonova

* Merger-driven transient

* Fast blue optical transient

* Luminous red nova

* Intermediate-luminosity optical transient

* Stellar tidal-disruption event

* Micronova

* Magnetar giant flare

* Gamma-ray burst progenitor

* Long gamma-ray burst source

* Short gamma-ray burst source

* Collapsar

* Supernova shock-breakout source

* Circumstellar-interaction transient

* Wolf–Rayet progenitor

* Supernova progenitor

* Planetary-nebula central star

* Post-AGB star

* Asymptotic giant branch star

* Thermally pulsing AGB star

* OH/IR star

* Mira variable

* Semiregular variable

* RV Tauri variable

* Cepheid variable

* Type II Cepheid

* RR Lyrae variable

* Long-period variable

* Irregular variable

* Luminous red variable

* Yellow dwarf in a post-main-sequence phase

### 251–300: Exotic Stellar Systems and Related Cosmic Objects

* Blue compact dwarf galaxy starburst population

* Population III protostar

* Massive primordial star

* Supermassive star (theoretical)

* Quasi-star (theoretical)

* Dark star (hypothetical dark-matter-powered star)

* First-generation metal-free star

* Pair-instability progenitor star

* Chemically homogeneous massive star

* Rapidly rotating massive star

* Be star

* Oe star

* B\[e\] star

* Herbig Be star

* Classical Be star

* Gamma Cassiopeiae variable

* Magnetic chemically peculiar star

* Ap/Bp magnetic star

* Pulsating subdwarf

* ELM white dwarf (extremely low-mass)

* Extremely low-mass helium white dwarf

* Double-degenerate binary

* Double-white-dwarf merger system

* AM Canum Venaticorum binary

* Cataclysmic variable

* Dwarf nova in quiescence

* Polar (magnetic cataclysmic variable)

* Intermediate polar

* Supersoft X-ray source

* Super-soft accreting white dwarf

* X-ray burster

* Type I X-ray burster

* Superbursting neutron star

* Ultraluminous X-ray source compact object

* Ultraluminous X-ray pulsar

* Microquasar

* X-ray binary

* High-mass X-ray binary

* Low-mass X-ray binary

* Be/X-ray binary

* Supergiant X-ray binary

* Symbiotic X-ray binary

* Colliding-wind massive binary

* Eclipsing compact-object binary

* Gravitational-wave-emitting compact binary

* Neutron-star merger system

* Black-hole merger system

* White-dwarf–neutron-star binary

* Stellar remnant in a globular cluster

* Compact-object triple system

Key distinction: a neutron star is a compact stellar remnant; a pulsar is a neutron star observed through its periodic emission; a magnetar is a neutron star with an exceptionally strong magnetic field; and a black hole is a compact object whose gravity prevents light from escaping from within its event horizon.

Kepler’s Laws, the Sun, Stars, Asteroids and SpaceTrain

Faizan Imran’s idea can be developed into a scientific project that models how the Sun, other stars, planets and asteroids move through space. The key is to combine Kepler’s three laws, Newton’s law of gravity, orbital mechanics and computer simulations.

One important distinction: we can calculate and simulate celestial trajectories, but we cannot currently move distant stars around at will. A realistic SpaceTrain project would be a physics-based simulation system, not a machine that physically moves stars.

1. Kepler’s three laws of planetary motion

\[ r=\frac{a(1-e^2)}{1+e\cos\nu} \]

These laws describe orbital motion. For precise simulations involving several stars or planets, Newton's laws of motion and gravity must also be used.

Source for the three laws: NASA's guide to Kepler's Laws.

NASA Science Kepler's Laws

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2. Newton’s law of universal gravitation

Kepler describes orbital patterns; Newton explains the gravitational force responsible for them.

\[ F=\frac{Gm_1m_2}{r^2} \]

• \(F\): gravitational force between two objects.

• \(G\): universal gravitational constant.

• \(m_1,m_2\): masses of the objects.

• \(r\): distance between their centres.

For several stars, the gravitational forces from all the other stars must be calculated together. This is called an N-body simulation.

NASA Science

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3. More suns and stars: from the Sun to giant stars

The following stars are compared by stellar type, not by their actual distance from Earth or their positions in space.

1. Sun

Reference star

A G-type main-sequence star. Its gravity governs the orbits of the planets in our Solar System.

2. Sirius A

A white A-type main-sequence star, more massive and luminous than the Sun. It belongs to a binary system with Sirius B.

3. Pollux

An evolved orange giant. Its larger radius makes it useful for studying how stars change as they age.

4. Arcturus

An orange giant star that demonstrates how a star can expand and evolve beyond the main sequence.

5. Aldebaran

A K-type giant known as the Eye of Taurus. Its expanded outer layers illustrate the changing size of an evolved star.

6. Betelgeuse

A red supergiant with an enormous, changing outer atmosphere. Its future evolution is expected to end in a supernova, although the timing is uncertain.

7. VY Canis Majoris

An extreme red hypergiant with an enormous extended atmosphere. Its exact size is difficult to determine because its outer material is diffuse.

4. The SpaceTrain mathematical model

Your original image contains the state vector:

\[ \mathbf{x}=(\mathbf r,\mathbf v,m,a,e,i,\Omega,\omega,\nu) \]

These variables describe an object's position, velocity, mass and orbital elements. For a simulation, the system would calculate how these values change with time.

Newton's equations for a group of celestial bodies can be written as:

\[ \frac{d^2\mathbf r_i}{dt^2} =\sum_{j\ne i} Gm_j\frac{\mathbf r_j-\mathbf r_i} {|\mathbf r_j-\mathbf r_i|^3} \]

This equation calculates the gravitational acceleration of body \(i\) due to every other body \(j\).

A computer program can then:

1. Load the masses and initial positions of the Sun, stars, planets or asteroids.

2. Calculate their mutual gravitational forces.

3. Update their positions and velocities in small time steps.

4. Plot their trajectories and calculate closest approaches.

5. Detect simulated collisions when bodies overlap, using their adopted physical radii.

Important: orbital elements such as \(a,e,i,\Omega,\omega,\nu\) are most naturally defined for a two-body orbit or an approximate orbit. In a system with many strongly interacting bodies, the full positions and velocities are needed to calculate the evolving motion.

5. What SpaceTrain could realistically do

Possible today

Simulate asteroid trajectories, planetary orbits, binary stars and hypothetical stellar encounters. Estimate collision probabilities under stated assumptions.

Requires careful modelling

Predicting actual stellar collisions requires reliable astronomical observations, three-dimensional velocities, masses and long-term gravitational calculations.

Not possible with current technology

Physically steering distant stars such as Sirius A, Betelgeuse or VY Canis Majoris into collisions.

6. Choose the next stage for Faizan's project

What should SpaceTrain develop first?

Interactive 3D Sun, stars and asteroid simulation

Complete Kepler, Newton and Einstein equations guide

Hypothetical stellar collision predictor

Scientific research proposal for SpaceTrain

Objects to include

Sun, eight planets and asteroids

Sun and all seven named stars

Stars, planets, moons and asteroids

Technical level

Beginner — simple explanations

Advanced — equations, data and calculations

Developer — working software and source code

Develop this SpaceTrain project