Cosmology Quiz on Thermal Bremsstrahlung and GRBs

The distribution of energy among particles in a fixed volume, often described by the Maxwell-Boltzmann distribution.

The wavelength at which a blackbody emits the most energy.

The amount of energy emitted by a blackbody per second, measured in Watts.

As temperature increases, the average energy of emitted photons increases, resulting in shorter wavelengths.

The wavelength of maximum emission shifts towards shorter wavelengths as the temperature of the blackbody increases.

A state of matter where electrons are packed so tightly that quantum mechanics rules apply, preventing them from occupying the same energy level.

The force that resists gravitational collapse in degenerate matter, caused by the pressure of tightly packed electrons.

In normal matter, electrons can move between orbital levels, but in degenerate matter, the Pauli Exclusion Principle forces them into distinct and already filled energy levels.

The process where atoms in matter lose their electrons, creating a dense, highly compressed state.

The ability of a substance to resist changes in volume when under pressure.

The event where a massive star (over 30 solar masses) collapses, forming a black hole and powerful jets of gamma rays.

The collision of two neutron stars, creating a short, intense burst of gamma rays.

Powerful outflows of particles and energy created near a black hole during a long GRB. They are responsible for the emission of gamma rays.

A massive star's explosion, much more powerful than a regular supernova, associated with long GRBs.

A supermassive black hole actively consuming material, producing a powerful spectrum of radiation, including gamma rays.

An X-ray burster is a type of neutron star that experiences sudden bursts of X-rays lasting about a minute.

Hydrogen from a nearby star accumulates on the neutron star's surface and undergoes thermonuclear fusion, leading to a sudden, intense burst of X-rays.

When charged particles interact and change their speed, they emit electromagnetic radiation. The faster they accelerate, the higher the frequency of the radiation.

X-ray pulsars produce radiation from charged particles moving in the magnetic field of a neutron star, while X-ray bursters release energy through thermonuclear explosions on the surface.

The frequency of radiation emitted from thermal bremsstrahlung is directly related to the acceleration of the charged particles. Faster acceleration leads to higher frequency radiation.

Synchrotron Radiation is emitted when a charged particle is forced to move in a curved path by magnetic and electric fields.

Radiation from X-ray pulsars is highly polarized due to the magnetic field, but radiation from X-ray bursters is not polarized due to its origin from a thermal explosion.

X-ray pulsars emit radiation in short bursts (milliseconds), while X-ray bursters have longer bursts (up to a minute).

Synchrotron Radiation results from the acceleration of charged particles in magnetic fields, causing the photons to be emitted in a specific direction along the particle's path.

Both Thermal Bremsstrahlung and Synchrotron Radiation are forms of electromagnetic radiation. They differ in their mechanisms of emission, with Thermal Bremsstrahlung due to particle collisions and Synchrotron Radiation due to magnetic forces.

In the photoelectric effect, a photon's entire energy is transferred to an electron, causing it to be ejected. This transfer is complete, making it precise for measuring the photon's total energy.

The work function refers to the minimum energy required to remove an electron from the surface of a material.

Compton scattering involves a photon interacting with an electron, transferring some of its energy, but not all. The amount of energy lost depends on the scattering angle, making it less accurate for determining the total energy of the photon.

The energy scale of typical photons is in the order of mega-electron volts (MeV), whereas the work function of materials used in detectors is typically in the order of electron volts (eV). This huge difference in energy scales emphasizes that the work function is negligible when compared to photon energies.

The photoelectric effect provides a more accurate measurement of the total energy of a photon compared to Compton scattering because in the photoelectric effect, the photon's entire energy is transferred to the electron, making the measurement precise and consistent.

A type of semiconductor material used in the NIRCam to detect infrared light. It has a narrower energy bandgap compared to materials used in optical CCDs, allowing it to absorb lower energy infrared photons.

The process of converting high-frequency radio waves into lower frequencies, making them easier to manipulate electronically. It is achieved by mixing the signal with a signal from a local oscillator of similar frequency, creating beat frequencies.

A device that focuses incoming radio waves onto a detector. It is typically a large parabolic dish, which reflects the waves to a focal point.

An amplifier that reduces noise in the radio signal received by a radio telescope. This is essential for detecting very faint astronomical signals.

A type of CCD detector designed to capture infrared light. It features on-site amplification of the charge collected at each pixel, enhancing the signal-to-noise ratio.