Sunlight appears white. however, rainbows, sunburn and the ability to see colors tell a different story. explain what each of these tells us about the suns radiation and what property determines different colors.

A) Sunlight basically consists of a combination of light of different wavelengths. Each of these wavelengths correspond to each of the colors of the rainbow. For example, red light has the longest wavelength. This is followed by orange, then yellow, green, blue and indigo. Violet has the shortest wavelength. These wavelengths (750 nm  to 400 nm) constitute the visible colors. All these light components of different wavelengths combine together to become the color white.

b) When this sunlight passes through droplets of rain, it gets refracted and that is what breaks up the white light into individual colors of the rainbow, just how light passing through a glass prism gets broken down into its individual seven colors.

c) Different objects have the ability to absorb different wavelengths of light. For example, glass absorbs light of all wavelengths except those between 560-520nm, which corresponds to green light. So it reflects the green light and thus, our eyes see  grass as green in color.

d) Light of wavelength below  400 nm (ultraviolet) and above 750nm (Infrared) are not visible. However, they exist in the sun's radiation. Ultraviolet rays are very harmful and responsible for causing sunburn and some types of skin tumors. Infrared light is also harmful and can cause premature wrinkling of skin.

  sequence  is a continuous and distinctive band of  stars  that appears on plots of stellar  color  versus  brightness. these color-magnitude plots are known as  hertzsprung–russell diagramsafter their co-developers,  ejnar hertzsprungand  henry norris russell. stars on this band are known as  main-sequence stars  or  dwarf stars. these are the most numerous true stars in the universe, and include the earth's  sun.after condensation and ignition of a star, it generates  thermal energy  in its dense core region through  nuclear fusion  of  hydrogen  into  helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in  hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of  gravitational collapse  from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the  photosphere. the energy is carried by either  radiation  or  convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the  mass of the sun  (1.5  m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the  proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of  carbon,  nitrogen  and  oxygen  as intermediaries in the  cno cycle  that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4  m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star  evolves  away from the main sequence on the hr diagram, into a  supergiant,  red giant, or directly to a  white dwarf.