2 most common scenarios:
1 - early universe was a cloud of gases (mainly hydrogen), so a certain part of the cloud starts to collapse dragging more and more gas by the force of gravity, enough for a gas planet to form, but not too much that a star forms.
2 - After a huge star burns out its fuel, it collapses or explodes in a huge supernova shooting off material containing all chemical elements. A planet might form from these material when they collapse under the force of gravity.
They are called planetesimals. These small bodies collided and merged to form larger bodies like planets and moons during the early stages of the solar system's formation.
Collisions among planetesimals of greatly varying size can lead to a process called accretion, where smaller planetesimals combine to form larger bodies. This can be a critical step in the formation of planets, as larger bodies have stronger gravitational pull and can continue to grow through further collisions. However, collisions with very large planetesimals could disrupt the growing planetesimal or lead to fragmentation, affecting the final size and composition of the resulting planets.
Planets form from a solar nebula through a process called accretion. As the nebula, composed of gas and dust, collapses under gravity, it begins to spin and flatten into a rotating disc. Within this disc, particles collide and stick together, gradually forming larger bodies called planetesimals. Over time, these planetesimals coalesce to create protoplanets, which can further merge to form the planets we see today.
Dust and gas particles in a protoplanetary disk collided and stuck together to form planetesimals, which then collided and accreted to form planets. The process of gravitational attraction and collisions led to the formation of larger bodies within the disk, eventually forming planets.
The protoplanet hypothesis describes the formation of planets from the dust and gas present in the early solar system. It suggests that small planetesimals collided and merged to form larger celestial bodies, eventually leading to the creation of the planets we see today.
Planetesimals.
Planetesimals are small solid objects that form in the protoplanetary disk around a young star, while protoplanets are larger bodies that develop from the accumulation and collision of planetesimals. Planetesimals are the building blocks that come together to form protoplanets, and eventually, planets. So, planetesimals are like the "seeds" that grow into protoplanets.
They are called planetesimals. These small bodies collided and merged to form larger bodies like planets and moons during the early stages of the solar system's formation.
Collisions among planetesimals of greatly varying size can lead to a process called accretion, where smaller planetesimals combine to form larger bodies. This can be a critical step in the formation of planets, as larger bodies have stronger gravitational pull and can continue to grow through further collisions. However, collisions with very large planetesimals could disrupt the growing planetesimal or lead to fragmentation, affecting the final size and composition of the resulting planets.
Rings of gas and dust orbiting stars may condense to form young planets or another term planetesimals. After this, it attracts more matter and increase in size to form planets. This is the basic steps of how planets was formed Dark matter ---->galaxy-------> star--------> planets
Dust clouds in space can gradually clump together due to gravitational attraction between particles, forming planetesimals. These planetesimals then collide and merge to form larger bodies, eventually accumulating enough mass to become planets. This process, known as accretion, is a key step in the formation of individual planets from dust clouds.
Dust and gas particles in a protoplanetary disk collided and stuck together to form planetesimals, which then collided and accreted to form planets. The process of gravitational attraction and collisions led to the formation of larger bodies within the disk, eventually forming planets.
Planetesimals stick together due to gravitational attraction and potentially other forces, such as electrostatic forces or chemical bonds. When two planetesimals collide with enough energy, they can merge and form larger bodies, eventually leading to the formation of planets. The exact mechanisms depend on factors like the size, composition, and relative velocities of the colliding bodies.
The building blocks of planets are called "planetesimals." These are small, solid objects that form from dust and gas in the protoplanetary disk surrounding a young star. Over time, planetesimals collide and coalesce, gradually forming larger bodies that can become planets. This process is part of the overall planetary formation in the early stages of a solar system's development.
By "accretion" of "planetesimals" from the "protoplanetary disk".
Protoplanets are larger bodies in the process of forming into planets, usually by accreting material from a protoplanetary disk. Planetesimals are small celestial bodies that are precursors to planets, often ranging in size from meters to hundreds of kilometers and are believed to be building blocks for planets. Essentially, protoplanets are further along in the planet formation process compared to planetesimals.
Planetesimals formed through the accretion of dust and ice in the protoplanetary disk surrounding a young star. As particles collided and stuck together, they gradually built up larger bodies through a process called gravitational attraction. Over time, these planetesimals combined to form protoplanets, which eventually coalesced into the planets we observe today. This process was influenced by factors such as temperature gradients, orbital dynamics, and the presence of gas and dust in the disk.