The most energetic electromagnetic waves in the universe are gamma-rays from gamma ray bursts (GRBs) from collapsing massive stars, observed by satellites with expected energies of 100 TeV (1 TeV = 1012eV). (a) (10) What is the frequency of these energetic gamma ray photons? 1 eV = 1.60 x 10-19 J. (b) What is the wavelength? 2. An astronaut on the International Space Station (ISS) is experimenting with a solid-state green laser communications system from on-orbit at 435 km altitude to the earth’s surface with a wavelength of 532nm and beam divergence (width) of 10-6 radians or 5.73 x 10-15° << 1°. The indices of refraction in free space and the atmosphere are n0 o 1.00000 ..., and na = 1.000293. Although density in the atmosphere varies continuously from the thinness of the upper atmosphere (near r ® 0) to higher density at the surface, refraction can be modeled as a ‘surface’ mid-atmosphere just like classic Snell’s Law calculations. (a) When the ISS is directly above the laser communications receiver on the ground, what is q2? (Draw a diagram)
The most energetic electromagnetic waves in the universe are gamma-rays from gamma ray bursts (GRBs) from collapsing massive stars, observed by satellites with expected energies of 100 TeV (1 TeV = 1012eV). (a) (10) What is the frequency of these energetic gamma ray photons? 1 eV = 1.60 x 10-19 J. (b) What is the wavelength? 2. An astronaut on the International Space Station (ISS) is experimenting with a solid-state green laser communications system from on-orbit at 435 km altitude to the earth’s surface with a wavelength of 532nm and beam divergence (width) of 10-6 radians or 5.73 x 10-15° << 1°. The indices of refraction in free space and the atmosphere are n0 o 1.00000 ..., and na = 1.000293. Although density in the atmosphere varies continuously from the thinness of the upper atmosphere (near r ® 0) to higher density at the surface, refraction can be modeled as a ‘surface’ mid-atmosphere just like classic Snell’s Law calculations. (a) When the ISS is directly above the laser communications receiver on the ground, what is q2? (Draw a diagram)
The most energetic electromagnetic waves in the universe are gamma-rays from gamma ray bursts (GRBs) from collapsing massive stars, observed by satellites with expected energies of 100 TeV (1 TeV = 1012eV). (a) (10) What is the frequency of these energetic gamma ray photons? 1 eV = 1.60 x 10-19 J. (b) What is the wavelength? 2. An astronaut on the International Space Station (ISS) is experimenting with a solid-state green laser communications system from on-orbit at 435 km altitude to the earth’s surface with a wavelength of 532nm and beam divergence (width) of 10-6 radians or 5.73 x 10-15° << 1°. The indices of refraction in free space and the atmosphere are n0 o 1.00000 ..., and na = 1.000293. Although density in the atmosphere varies continuously from the thinness of the upper atmosphere (near r ® 0) to higher density at the surface, refraction can be modeled as a ‘surface’ mid-atmosphere just like classic Snell’s Law calculations. (a) When the ISS is directly above the laser communications receiver on the ground, what is q2? (Draw a diagram)
The most energetic electromagnetic waves in the universe are gamma-rays from gamma ray bursts (GRBs) from collapsing massive stars, observed by satellites with expected energies of 100 TeV (1 TeV = 1012eV).
(a) (10) What is the frequency of these energetic gamma ray photons? 1 eV = 1.60 x 10-19 J.
(b) What is the wavelength?
2. An astronaut on the International Space Station (ISS) is experimenting with a solid-state green laser communications system from on-orbit at 435 km altitude to the earth’s surface with a wavelength of 532nm and beam divergence (width) of 10-6 radians or 5.73 x 10-15° << 1°. The indices of refraction in free space and the atmosphere are n0 o 1.00000 ..., and na = 1.000293. Although density in the atmosphere varies continuously from the thinness of the upper atmosphere (near r ® 0) to higher density at the surface, refraction can be modeled as a ‘surface’ mid-atmosphere just like classic Snell’s Law calculations.
(a) When the ISS is directly above the laser communications receiver on the ground, what is q2? (Draw a diagram)
Interaction between an electric field and a magnetic field.
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