the heat coming from the photospher (sun's) is what type of electromagnetic radiation?
477826
heat is not electromagnetic radiation, it's molecular kinetic energy (or thermal energy).  The sun emits Ultraviolet radiation, amongst other emissions in the light spectra, but i don't believe the heat emitted can be attributed to an electromagnetic wave.
419301
The sun is actually made up of hydrogen gas. The "burning" you speak of is the fusion of hydrogen in to helium, which emits extreme amounts of light and energy.
290359
The energy of a photon is given by E = h*f where h is planck's constant and f is the frequency.  Since photons travel at the speed of light, c, the wavelength is just:\nlambda = c / f.\n\nThe spectrum of light goes from red to violet, where red has the lowest frequency (longest wavelength) and violet has the highest frequency (shortest wavelength).  This means that violet light has more energy per photon than red light.\n\nIn radiation heat transfer, a black body is an object that absorbs all incoming radiation and reflects none (stars are nearly black).  Also, a black body emits a spectrum of radiation based on its temperature.  A plot of monochromatic emissive power vs. wavelength shows the relative "concentration" of different wavelengths of radiation in the total output.  This plot has a characteristic shape given by Planck's Law of blackbody radiation, and it has a maximum at:\n\nlambda_max * T = 2898 micrometers * K = constant\n\nwhere T is the temperature in Kelvin\n\nThus lambda_max is inversely proportional to Temperature.  This means, as the temperature of the emitting body increases, the wavelength at which more of the energy is radiated at decreases (the frequency increases).\n\nI wish I could show you the loglog plot of monochromatic emissive power vs wavelength in Mills page 453.  It shows how low temperature bodies emit in the infrared and negligibly in the visible range and as the temperature increases, the maximum moves toward the visible range.  The sun, at 5800 K has a nice plateau maximum in the visible range which explains why being able to see light is so useful for us.  Another cool thing to see in the plot is that the curve is steeper on the low wavelength side than it is on the high wavelength side: this means that as you increase the temperature of an object, it will glow red and then white because anything hot enough to have its maximum in the violet range also has a large emissive power for everything colder than violet, so all colors of light will be present.\n\nSince a hotter body radiates at higher frequencies, in a sense violet light is "hotter" than red light.\n\nTake a look at the book (or another heat transfer engineering text).  I can't explain very well with only text.
1183093
sun bathing is radiation. sun radiation travel through space(no air in space so it is pure radiation energy transfer), travel through air (in there also radiation is dominant ) then get in to your skin\n\nstroform is a good insulater. it has hollo set of chambers. in chambers covection can be done but cells prevent transfer of air further and convection is stoped. in the other hand conduction is prevented due to poor conductivity of material. radiation is not a problem when heat difference is not too much high and because radiation generated from a object is is propotional to absolute heat  of the object. in case of very high temperature allumenium foil is used to limit radiation.
948797
convection, advection and radiation
1176203
One way it actually interacts is by catalysing chemical reactions-various spectrums of light increase atomic bonding between different chemicals and atoms. Of course there is heat, the solar radiation excites atoms and increases their activity, generating heat. Most everything else is optics, like things we say as white reflect almost all the light hitting them and things we see as black absorb the entire spectrum of visible light.
425682
The Core: The Sun's core has a tremendously high temperature and pressure. The temperature is roughly 15 million °C. At this temperature, nuclear fusion occurs, turning four hydrogen nuclei into a single helium nucleus plus a LOT of energy. This "hydrogen burning" releases gamma rays (high-energy photons) and neutrinos (particles with no charge and almost no mass). \n\nThe Radiative Zone (or radiation zone): The next layer out from the core is this zone which emits radiation. This radiation diffuses outwards. The temperature ranges from 15 million °C to one million °C. It may take photons of radiation millions of years to pass through the radiative zone, as they gradually make their way outwards. \n\nThe Convective Zone: In this next layer, photons continue to make their way outwards via convection (towards lower temperature and pressure). The temperature ranges from one million °C to 6,000 °C. \n\nThe Photosphere: This is the lower atmosphere of the Sun and the part that we see (since it emits light at visible wavelengths). This layer is about 300 miles (500km) thick. The temperature is about 5,500 °C. \n\nThe Chromosphere: This reddish layer is an area of rising temperatures. The temperature ranges from 6,000 °C (at lower altitudes) to 50,000 °C (at higher altitudes). This layer is a few thousand miles (or kilometers) thick. It appears red because hydrogen atoms are in an excite state and emit radiation near the red part of the visible spectrum. \n\nThe Chromosphere is visible during solar eclipses (when the moon blocks the Photosphere). \n\nThe Corona: This is the outer layer of the Sun's atmosphere. The corona extends for millions of miles and the temperatures are tremendous, reaching one million °C. \n\nHoles in the corona occur where the Sun's magnetic field loops out into space. These coronal holes may be the source of the solar wind, a stream of energetic particles that permeate the Solar System.
471190
Electromagnetic radiation in the 1 to 1000 m wavelength range.
567446
Due to the fusion process taking place inside the sun it emits radiation. The sunlight has solar energy.\n\nIf u would use some other source of light may be artificial then may be the energy generated would be less
118278
Nothing.  Light is a form of radiation, just as are microwaves, radio waves, ultraviolet rays, x-rays and gamma rays.  However, ultraviolet, x-rays, and gamma rays contain much more energy than do light waves, so they can be damaging to biological tissue.
382985
Light and radio signals are all the same thing, electromagnetic radiation. Radio waves are just very low frequency light and light is just very high frequency radio signals. All objects that are hotter than absolute zero give off some electromagnetic radiation. The really hot objects give off visible light. Cooler ones give off infra red light. Cooler still and you get radio emissions. The Earth's surface gives off radio waves because it is warm. In fact, it gives off so much that it is an interference for communication satellites trying to hear signals from the ground.\n\nModern radio astronomy uses giant antennas to focus radio waves, just like optical telescopes focus visible light. Computers are used to construct images of what the sky would look like if your eyes could see radio waves.
584790
There is no one single uniform temperature in the sun. It depends which layer we are talking about ...\n\nThe Core\nThe innermost layer of the sun is the core. With a temperature of 15 million kelvins (27 million degrees Fahrenheit) \n\nSolar Envelope\nOutside of the core is the radiative envelope, which is surrounded by the convective envelope. The temperature is 4 million kelvins (7 million degrees F). The core contains 40 percent of the sun's mass in 10 percent of the volume, while the solar envelope has 60 percent of the mass in 90 percent of the volume.\n\nPhotosphere\nThe photosphere is the zone from which the sunlight we see is emitted. The photosphere is a comparatively thin layer of low pressure gasses surrounding the envelope. It is only a few hundred kilometers thick, with a temperature of 6000 K. \n\nChromosphere\nIn an eclipse, a red circle around the outside of the sun can sometimes can be seen. This is the chromosphere. Its red coloring is caused by the abundance of hydrogen.\n\nFrom the center of the sun to the chromosphere, the temperature decreases proportionally as the distance from the core increases. The chromosphere's temperature, however, is 7000 K, hotter than that of the photosphere. Temperatures continue to increase through the corona.\n\nSunspots\nSunspots are dark spots on the photosphere, typically with the same diameter as the Earth. They have cooler temperatures than the photosphere. The center of a spot, the umbra, looks dark gray if heavily filtered and is only 4500 K (as compared to the photosphere at 6000K). \n\nThe sun has enormous organized magnetic fields that reach from pole to pole. Loops of the magnetic field oppose convection in the convective envelope and stop the flow of energy to the surface. This results in cool spots at the surface which produce less light than the warmer areas. These cool, dark spots are the sunspots.\n\nCorona\nThe outermost layer of the sun is the corona. Only visible during eclipses, it is a low density cloud of plasma with higher transparency than the inner layers. The white corona is a million times less bright than the inner layers of the sun, but is many times larger.\n\nThe corona is hotter than some of the inner layers. Its average temperature is 1 million K (2 million degrees F) but in some places it can reach 3 million K (5 million degrees F).\n\nTemperatures steadily decrease as we move farther away from the core, but after the photosphere they begin to rise again. There are several theories that explain this, but none have been proven.\n\nSolar Flares\nIn the corona, above sunspots and areas of complex magnetic field patterns, are solar flares. These sparks of energy sometimes reach the size of the Earth and can last for up to several hours. Their temperature has been recorded at 11 million K (20 million degrees F). The extreme heat produces x rays that create light when they hit the gases of the corona.
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light and heat are both electromagnetic waves. Light is in the visible spectrum, and heat is in the infrared spectrum, which is right next to the visible spectrum, but below it. \n\nThink of a coil spring. Look at it from the side. The cols are like waves. Light waves are spaced a certain distance apart. When the spring is stretched, the waves have lower energy and take up more space-- they are longer. These are heat waves and radio waves, compared to visible light.\n\nNow, suppose that the spring is squeezed together rather than stretched apart. This time, the waves are closer together, and have a higher energy. These are ultraviolet waves, or (depending on how high their energy goes) x rays, or even gamma rays.\n\nSo, all the waves are related, it is just how much energy they have that makes them spread out or crowd together. Visible light just happpens to be in the middle, the colors we can see.
532257
A good approximation to the distribution of electromagnetic radiation emitted by the sun is given by the equation for a blackbody with a temperature of 5780 Kelvin:\n\nPower (Watts/meter^2 surface are/meter wavelength) = \n  2*pi*h*c^2/L^5*(exp(h*c/L*k*T)-1)\n\nwhere\n\nh = Planck's constant (6.626 x 10^-34 Joule*sec)\nc = speed of light (2.998 x 10^8 meters/sec)\nL = wavelength (meters)\nk = Boltzmann's constant (1.38 x 10^-23 Joule/Kelvin)\nT = temperature (Kelvin)\n\nThe sun's power output peaks in the visible portion (around a wavelength of 500nm) of the electromagnetic spectrum, but it emits over the entire range of possible wavelengths.\n\nIn reality, the solar spectrum is much more complicated than a simple blackbody curve because of the absorption of specific frequencies by the atoms making up the sun, as well as temperature inhomogeneities and effects due to the sun's magnetic field.
58963
"Solar energy is created deep within the core of the Sun. It is here that the temperature (15,000,000° C; 27,000,000° F) and pressure (340 billion times Earth's air pressure at sea level) is so intense that nuclear reactions take place."\n\n"The Sun's outer visible layer is called the photosphere and has a temperature of 6,000°C (11,000°F). "\n\n"Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F)."
164251
Methane allows solar radiation of short wavelengths in, but not longer wavelength heat.  The increased levels of methane have caused more heat to be trapped within Earth's atmosphere, thus increasing the global temperature.
78735
Light, form of electromagnetic radiation similar to radiant heat, radio waves, and X rays. Light consists of extremely fast oscillations of an electromagnetic field in a particular range of frequencies that can be detected by the human eye. Different colour sensations are produced by light vibrating at different frequencies, ranging from about 4 × 1014 vibrations per second for red light to about 7.5 × 1014 vibrations per second for violet light. The visible spectrum of light is usually defined by its wavelength, ranging from the smallest visible wavelength for violet, about 40 millionths of a centimetre (16 millionths of an inch), to 75 millionths of a centimetre (about 30 millionths of an inch) for red. Higher frequencies, corresponding to shorter wavelengths, comprise ultraviolet radiation, and still higher frequencies are associated with X-rays. Lower frequencies, which are at longer wavelengths, are called infrared radiation, and still lower frequencies are characteristic of radio waves. Most light comes from electrons that vibrate at these high frequencies when heated to a high temperature. The higher the temperature, the greater the frequency of vibration and the bluer the light produced.\nLight is emitted from a source in straight lines and spreads out over a larger and larger area as it travels; the light per unit area diminishes as the square of the distance. When light strikes an object, it is either absorbed or reflected; light reflected from a rough surface is scattered in all directions. Some frequencies are reflected more strongly than others, and this gives objects their characteristic colour. White surfaces scatter light of all wavelengths equally, and black surfaces absorb nearly all light. Image-forming reflection, on the other hand, requires a highly polished surface such as that of a mirror.\n\nDefining the nature of light has always been a fundamental problem in physics. The English mathematician and physicist Sir Isaac Newton described light as an emission of particles, and the Dutch astronomer, mathematician, and physicist Christiaan Huygens developed the theory that light travels by a wave motion.\n\nIt is now believed that these two theories are essentially complementary, and the development of quantum theory has led to the recognition that in some experiments light acts like a series of particles and in other experiments it acts like a wave. In those situations in which it travels in wave motion, the wave vibrates at right angles to the direction of travel; therefore light can be polarized in two mutually perpendicular planes (see Optics).\n\nIII  VELOCITY \n\nThe speed of light was first measured in a laboratory experiment by the French physicist Armand Hippolyte Louis Fizeau, although earlier astronomical observations had yielded approximately the right velocity. By the 1970s the speed of light had been measured very precisely as 299,792,458 m/sec (186,282.397 mi/sec) in a vacuum, and could be used to measure large distances by the time it took for a pulse of light or radio waves to reach a target and return. This is the principle of radar and sonar. Accurate knowledge of the speed and the wavelength of light also permits accurate measurement of length. In fact, in 1983 the metre was redefined as the length of the path travelled by light in a vacuum during a time interval of 1/299,792,458 of a second. The velocity of light in air varies slightly with wavelength, averaging about 3 per cent less than in vacuum; the speed in water is about 25 per cent less, and in glass, 33 per cent less.\n\nLight has an important effect on many chemicals. Sunlight, for example, is used by plants to carry out photosynthesis, and the exposure of certain silver-containing chemicals to light causes them to turn dark in the presence of other chemicals, as is the case in photography.