The Ultimate Solar System Quiz

The Sun is a G-type main-sequence star at the center of the Solar System.
Its radius is about 695,000 kilometers, or 109 times that of Earth, and its mass is about 330,000 times that of Earth.
The Sun is mainly composed of hydrogen and helium, with smaller quantities of heavier elements.
The energy from the Sun is the most important source of energy for life on Earth.
The Sun fuses about 600 million tons of hydrogen into helium every second, producing light and heat.
The Sun will eventually become a red giant and then a white dwarf, no longer producing energy by fusion.
The Sun is the brightest object in the Earth's sky, and its energy supports almost all life on Earth.
The Sun's distance from Earth varies, but it takes about 8 minutes and 20 seconds for sunlight to travel from the Sun's horizon to Earth's horizon.
The Sun's rotational period is approximately 25.6 days at the equator and 33.5 days at the poles.
The Sun's original chemical composition was inherited from the interstellar medium out of which it formed.
The Sun is a star that formed 4.6 billion years ago.
It primarily fuses hydrogen into helium in its core, which has a density of up to 150 g/cm3 and a temperature of 15.7 million K.
The fusion rate in the core is in a self-correcting equilibrium.
Energy is transferred from the core to the photosphere through radiation and convection.
The photosphere is the visible surface of the Sun and has a particle density of ~1023 m−3.
The Sun's heavy-element abundances are measured using spectroscopy of the photosphere and meteorites.
The Sun's helium fraction is increasing, and in about 5 billion years, it will cause the Sun to become a red giant.
The radiative zone is the thickest layer of the Sun, and thermal radiation is the primary means of energy transfer.
The convection zone extends from 0.7 solar radii to near the surface and allows convective currents to develop and move the Sun's energy outward.
The Sun's thermal columns form an imprint on the surface, giving it a granular appearance called the solar granulation.

The Sun's atmosphere is composed of the photosphere, chromosphere, transition region, corona, and heliosphere.
The coolest layer of the Sun is the temperature minimum region, which allows for the existence of simple molecules.
The chromosphere, transition region, and corona are much hotter than the surface of the Sun, with the corona being the hottest.
The corona is the extended atmosphere of the Sun, which has a volume much larger than the volume enclosed by the Sun's photosphere.
The heliosphere is the tenuous outermost atmosphere of the Sun, filled with solar wind plasma.
The Sun emits light across the visible spectrum, with a color index near (0.3, 0.3) when viewed from space.
The solar constant is the amount of power that the Sun deposits per unit area that is directly exposed to sunlight.
Ultraviolet light from the Sun has antiseptic properties and can be used to sanitize tools and water, but it is also the main cause of skin cancer.
Energy transport in the Sun is a process that involves photons in thermodynamic equilibrium with matter, and it takes about 30,000,000 years for energy to be transported from the core to the surface.
The Sun has a magnetic field that varies across its surface, with the polar field being 1-2 gauss and the field in sunspots being typically 3,000 gauss.

The Sun's magnetic field causes solar activity, including sunspots, solar flares, and coronal-mass ejections.
The 11-year sunspot cycle is half of a 22-year Babcock-Leighton dynamo cycle.
During the solar cycle's declining phase, sunspots diminish in number and size.
Solar activity can affect Earth's climate and space weather conditions.
The Sun formed about 4.6 billion years ago from the collapse of a giant molecular cloud.
The Sun is currently in its main-sequence stage, during which nuclear fusion reactions fuse hydrogen into helium.
The Sun will spend a total of approximately 10 to 11 billion years as a main-sequence star before the red giant phase.
The Sun is gradually becoming hotter, larger, and more luminous during its time on the main sequence.
The Sun's magnetic field extends well beyond the Sun itself, forming the interplanetary magnetic field.
The interplanetary magnetic field is much stronger than the dipole component of the solar magnetic field due to magnetic fields generated by electrical currents in the plasma surrounding the Sun.