AST1100 Lecture Notes
... both of which can be found in tables of mathematical functions. The final result is called the Stefan-Boltzmann law, F = σT 4 , the flux emitted from a black body is proportional to the temperature to the fourth power. We see that we have two ways of measuring the temperature of a star, by looking ...
... both of which can be found in tables of mathematical functions. The final result is called the Stefan-Boltzmann law, F = σT 4 , the flux emitted from a black body is proportional to the temperature to the fourth power. We see that we have two ways of measuring the temperature of a star, by looking ...
Radiation Effects on Space Electronics
... Jan Kenneth Bekkeng, University of Oslo - Department of Physics ...
... Jan Kenneth Bekkeng, University of Oslo - Department of Physics ...
NON-DESTRUCTIVE TESTING
... The process fails without electricity To interpret the weld radiograph a large amount of experience is required gamma rays is an alternative to x rays because of this disadvantages ...
... The process fails without electricity To interpret the weld radiograph a large amount of experience is required gamma rays is an alternative to x rays because of this disadvantages ...
Kirchhoff law
... Increasing the temperature increases the intensity at all wavelengths Total area under the curve increases as temperature increases, corresponding to increased total emission as the object becomes hotter. Maximum intensity shifts to shorter wavelengths with increasing temperatures Function defined o ...
... Increasing the temperature increases the intensity at all wavelengths Total area under the curve increases as temperature increases, corresponding to increased total emission as the object becomes hotter. Maximum intensity shifts to shorter wavelengths with increasing temperatures Function defined o ...
GCSE Physics criteria sheet
... • payback time State and use the equation: efficiency = useful energy output / total energy output ...
... • payback time State and use the equation: efficiency = useful energy output / total energy output ...
Astronomical units
... Consider a small area dA, exposed to radiation for a time dt. Energy passing through the area is F.dA.dt, where F is the energy flux (units erg s-1 cm-2). Unless the radiation is isotropic (same in all ...
... Consider a small area dA, exposed to radiation for a time dt. Energy passing through the area is F.dA.dt, where F is the energy flux (units erg s-1 cm-2). Unless the radiation is isotropic (same in all ...
Part 1
... photons in some new direction. For a beam directed towards the observer, scattering still has the eect of diminishing the recorded signal, so the two types of process can be treated together for the present purposes. The amount of intensity removed from a beam by extinction in (say) a gas cloud mus ...
... photons in some new direction. For a beam directed towards the observer, scattering still has the eect of diminishing the recorded signal, so the two types of process can be treated together for the present purposes. The amount of intensity removed from a beam by extinction in (say) a gas cloud mus ...
Likely formation of general relativistic radiation pressure supported
... of Led . As if, a leaking and contracting balloon stops contraction as its self gravity fixes the leakage by forcing the molecules to move in (almost) closed circular orbits. Also, simultaneously, the attendant heat and pressure become large enough to resist further contraction. In a very strict sen ...
... of Led . As if, a leaking and contracting balloon stops contraction as its self gravity fixes the leakage by forcing the molecules to move in (almost) closed circular orbits. Also, simultaneously, the attendant heat and pressure become large enough to resist further contraction. In a very strict sen ...
Support worksheet – Option I Questions
... A patient of mass 72 kg is injected with a quantity of technetium 99 whose average activity while in the body is 380 MBq. Technetium 99 decays by gamma emission. The energy of the photons emitted in the decay of technetium is 140 keV. The radioactive material remains in the body for 6 hours. Calcula ...
... A patient of mass 72 kg is injected with a quantity of technetium 99 whose average activity while in the body is 380 MBq. Technetium 99 decays by gamma emission. The energy of the photons emitted in the decay of technetium is 140 keV. The radioactive material remains in the body for 6 hours. Calcula ...
White Dwarfs & Other Ends March 21 − Stars with < 2 M
... • Pressure is not greater at hotter temperature • Baseballs move because they are close together • Quantum mechanics: uncertainty relation • Speed × confinement = Planck’s constant • Pressure is greater if gas is confined to smaller region • In a smaller star, baseballs move faster • Baseballs hit w ...
... • Pressure is not greater at hotter temperature • Baseballs move because they are close together • Quantum mechanics: uncertainty relation • Speed × confinement = Planck’s constant • Pressure is greater if gas is confined to smaller region • In a smaller star, baseballs move faster • Baseballs hit w ...
Properties of Light and Radiation
... Distance traversed in 1 year is called a light-year. Has properties characteristic of both waves and particles. Wave nature: Wavelength × Frequency = c (Speed) λ × ν = c Wavelengths range from γ− rays (λ ∼ 10−13 cm) to radio (λ ∼ 103 cm). Visible light is optical radiation, 3 × 10−5 cm < λ < 7 × 10− ...
... Distance traversed in 1 year is called a light-year. Has properties characteristic of both waves and particles. Wave nature: Wavelength × Frequency = c (Speed) λ × ν = c Wavelengths range from γ− rays (λ ∼ 10−13 cm) to radio (λ ∼ 103 cm). Visible light is optical radiation, 3 × 10−5 cm < λ < 7 × 10− ...
Orbital Instabilities in Triaxial Mass Distributions and
... of stars and planets? [2] What can we say about the basic properties of the birth cluster for our own Sun and its Solar System? ...
... of stars and planets? [2] What can we say about the basic properties of the birth cluster for our own Sun and its Solar System? ...
oct06
... filament temperature is now about 3000K. The bulb is emitting a lot more visible light, all the colors, though not all in equal amounts. The mixture of the colors produces a "warm white" light. It is warm because it is a mixture that contains a lot more red, orange, and yellow than blue, green, and ...
... filament temperature is now about 3000K. The bulb is emitting a lot more visible light, all the colors, though not all in equal amounts. The mixture of the colors produces a "warm white" light. It is warm because it is a mixture that contains a lot more red, orange, and yellow than blue, green, and ...
Radiation pressure
Radiation pressure is the pressure exerted upon any surface exposed to electromagnetic radiation. Radiation pressure implies an interaction between electromagnetic radiation and bodies of various types, including clouds of particles or gases. The interactions can be absorption, reflection, or some of both (the common case). Bodies also emit radiation and thereby experience a resulting pressure.The forces generated by radiation pressure are generally too small to be detected under everyday circumstances; however, they do play a crucial role in some settings, such as astronomy and astrodynamics. For example, had the effects of the sun's radiation pressure on the spacecraft of the Viking program been ignored, the spacecraft would have missed Mars orbit by about 15,000 kilometers.This article addresses the macroscopic aspects of radiation pressure. Detailed quantum mechanical aspects of interactions are addressed in specialized articles on the subject. The details of how photons of various wavelengths interact with atoms can be explored through links in the See also section.