Solar Physics and Energy Generation

A type of neutrino produced in the Sun's proton-proton chain.

Nuclear fusion process in the sun, creating energy and neutrinos

Instruments that detect elusive neutrinos.

Specific neutrino detector used to measure solar neutrino flux.

Neutrinos weakly interact with matter.

The rate of solar neutrinos passing through a given area.

Neutrinos can change types

Theoretical predictions describing the sun's internal workings, including neutrino productions

Subatomic particles produced by nuclear fusion in the Sun's core, carrying away energy from the reactions.

A giant underground detector in Japan designed to study neutrinos, specifically solar neutrinos.

The discrepancy between the number of solar neutrinos predicted by models and those actually detected.

The primary nuclear fusion process in the Sun, where hydrogen nuclei combine to form helium and release energy.

Neutrinos are created in the Sun's core during the proton-proton chain.

The fundamental force responsible for how neutrinos interact with matter, making them difficult to detect.

The number of solar neutrinos passing through a given area in a specific time.

By studying the pp-chain and the neutrinos it produces, we can gain a better understanding of the Sun's inner workings.

Stellar corpses with a mass exceeding the neutron star limit (2-3 solar masses) collapse under their own gravity, forming a black hole.

X-ray binaries containing compact objects too massive to be neutron stars strongly suggest the existence of black holes.

Extremely powerful explosions in distant galaxies, likely caused by supernovae that create black holes.

Two neutron stars in close binaries emit gravitational waves, causing them to merge. This process may be the primary source of heavy elements like gold and platinum.

Binary systems of black holes emit gravitational waves, leading to mergers. These mergers have been directly detected and provide strong evidence for black holes.

The dense, Earth-sized core left behind after a low-mass star runs out of fuel. Supported against gravity by electron degeneracy pressure.

A sudden, dramatic brightening of a white dwarf in a binary system, caused by hydrogen fusion on its surface.

An explosive event that occurs when a white dwarf exceeds the Chandrasekhar Limit (1.4 solar masses), causing it to collapse and explode.

The extremely dense, rapidly spinning remnant of a massive star's core after a supernova. Composed mostly of neutrons and held together by strong nuclear forces.

A rapidly rotating neutron star that emits beams of radiation, detected as regular pulses of energy.

A binary star system where a neutron star accretes matter from its companion, forming a hot, gas-rich accretion disk that emits X-rays.

A region of spacetime where gravity is so strong that nothing, not even light, can escape. Formed from the collapse of massive stars.

The boundary around a black hole beyond which nothing can escape. The 'point of no return.'

The makeup of the Sun, determined by analyzing the absorption lines in its spectrum. This reveals the elements present and their abundance.

The visible surface of the Sun, which we observe at optical wavelengths. It's the region where light escapes the Sun and reaches Earth.

A state of balance in the Sun where the outward pressure from nuclear fusion perfectly counteracts the inward force of gravity, preventing the Sun from collapsing or expanding.

Dark lines in the Sun's spectrum, caused by elements in the Photosphere absorbing specific wavelengths of light.

Pressure in the sun comes from the constant collision of particles (like atoms and ions) due to the high temperature and density of the core.

The entire range of electromagnetic radiation emitted by the Sun. It's like a fingerprint that reveals its composition and temperature.

Nuclear fusion in the Sun's core releases tremendous energy, which exerts an outward pressure, pushing against the inward force of gravity.

The process in the Sun's core where hydrogen atoms fuse to form helium, releasing a tremendous amount of energy. This is the source of the Sun's power.

The Sun's immense gravity pulls its own mass inward, towards the core, creating a strong inward force.

The energy produced by nuclear fusion in the Sun's core, eventually reaching Earth as light and heat.

The force of attraction between any two objects with mass. The bigger the mass, the stronger the gravity.

The Sun's gravity pulls inward, trying to collapse it. This force is balanced by the outward pressure from nuclear fusion.

It ensures a stable Sun, preventing it from collapsing under its own gravity or expanding uncontrollably.

This balance is crucial for the Sun's long-term stability, allowing it to sustain nuclear fusion and provide energy to Earth for billions of years.

The region in the Sun where hot gas rises and cooler gas sinks, transferring energy from the core outwards.

The process where photons emitted in the Sun's core take a long, winding path to escape the Sun due to constant collisions with particles in the dense plasma.

A powerful computer model that allows scientists to visualize and study the complex processes of convection in the Sun's interior.

The visible surface of the Sun, where the light we see originates from.

The process where nuclear fusion reactions in the Sun's core convert hydrogen into helium, releasing immense amounts of energy that power the Sun.

The Convection Zone plays a crucial role in transporting heat and energy from the Sun's core to its surface, eventually reaching Earth.

The Sun's energy originates from the core, where nuclear fusion reactions continuously occur.

The Sun's spectrum shows dark lines (absorption lines) caused by elements in the photosphere absorbing specific wavelengths of light, revealing its composition.

The pressure inside a star increases as you go deeper towards the core, mainly due to the weight of the overlying layers.

The temperature within a star also increases towards the core, due to the heat generated by nuclear fusion reactions.

A unit of mass used to measure the mass of stars and other celestial objects. One solar mass is equal to the mass of our Sun.

Subatomic particles produced by nuclear fusion in the Sun's core, carrying away energy from the reactions.

The Sun maintains a balance between the energy produced by nuclear fusion in its core and the energy radiated into space.

Nuclear fusion in the Sun's core converts hydrogen to helium, releasing tremendous energy that we see as sunlight.

The Sun's stability is maintained by hydrostatic equilibrium and energy balance, ensuring a constant supply of energy for billions of years.

Nuclear fusion is the source of the Sun's energy. It provides the outward pressure that counteracts gravity and keeps the Sun stable.

The Sun's core is incredibly hot and dense, with temperatures reaching millions of degrees, allowing nuclear fusion to occur.

The energy released by nuclear fusion in the Sun's core travels outward, eventually reaching Earth as light and heat.

The Sun has enough hydrogen fuel to sustain nuclear fusion for approximately another 5 billion years.