Solar Nebular Model - Fill in the Blank Flashcards

A set of fill-in-the-blank flashcards covering Kant–Laplace Nebular Theory, the Solar Nebular Disk Model, angular momentum, protostars, protoplanetary disks, planetesimals, accretion, frost line, and the differences between terrestrial and Jovian planet formation.

In the Kant–Laplace Nebular Theory, the collapsing nebula formed a rotating disk; the central part became the __.

Sun

The Sun contains about __% of the Solar System's total angular momentum.

2%

The Solar Nebular Model is also known as the __.

Solar Nebular Disk Model (SNDM)

A major contributor to the Solar Nebular Disk Model (1969) is __.

Victor Safronov

The Solar System is believed to have formed around __ Ga.

4.55

The collapse of the Solar Nebula is triggered by an external event such as a shockwave from a nearby __.

supernova

Conservation of angular momentum causes the cloud's rotation speed to __ as its size decreases.

increase

During the collapse, gravitational potential energy is converted into kinetic energy, heating the gas and forming a __.

protostar

The rest of the material in the flattened disk forms a __, the birthplace of planets.

protoplanetary disk

In the rotating disk, the process of small particles colliding and sticking together to form larger bodies is called __.

accretion

The larger bodies formed by accretion are called __.

planetesimals

Planetesimals initially measured about the size of __ but grew to several kilometers.

centimeters

Some planetesimals coalesced to form even larger bodies called __.

protoplanets

As the radius from the protosun increases, the temperature __.

becomes cooler

In the inner region, only materials like rocks can withstand the heat, giving rise to the small, dense, and rocky planets called __.

Terrestrial Planets

A frost line (snow line) is the distance from the sun where water, ammonia, and methane can __ into a solid ice grain.

freeze

Terrestrial planets are located __ from the Sun.

close to

Jovian planets are composed mostly of hydrogen and __.

helium

Jovian planets are located __ from the Sun.

farther

Jovian planets formed farther from the Sun because volatile materials like __ could condense.

gas and ices

In the early solar system, the frost line marks the boundary between warm inner regions and cooler outer regions where ices and gases can __.

condense

The first step in terrestrial planet formation is the condensation of gases to form __.

rocky particles

The next step is the formation of clumps from rocky particles, a process known as __.

accretion

The growth of clumps into larger bodies is called __.

accretion

Formation of planetesimals from clumps is known as __.

accretion

Growth of planetesimals to a limiting size leads to the formation of __ planets.

terrestrial

The final stage in terrestrial planet formation is the formation of __ planets.

Terrestrial

In Jovian planet formation, condensation of gases forms __ particles.

ice

Ice particles form clumps in a process called __.

accretion

Accretion of clumps leads to the formation of __ planets.

Jovian

The overall sequence of Jovian planet formation ends with the formation of __ planets.

Jovian