![]() ![]() Estimating the current age ofthe universe to be 20 billion years, the time to reach equilibrium fora solar mass black hole is 7.00*10^18 times as long as the universe iscurrently old. Checkit out!įor a solar mass black hole, the time to reach equilibrium is about4.41*10^36 seconds, or 1.40*10^29 years. ![]() The equilibriumpoint at which rate mass loss through Hawking radiation equals rate massgain through background radiation absorption can be determined. At thispoint, the black hole will begin to experience a net mass loss. After enough time has passed, however, the universe willbecome too cold to replace the mass lost to Hawking radiation. This temperatureis definitely hot enough to dominate the net change in mass of a solarmass black hole. Currently,the cosmic background radiation temperature is about 2.7 K. The expanding universe coolsat a rate inversely proportional to the age of the universe. High cosmic backgroundradiation temperatures can easily feed a large black hole enough mass toovercome the virtually insignificant Hawking radiation.ĭoes this mean that black holes will forever gain mass, never radiatingquickly enough to eventually disappear? No. Jennifer Leman, Popular Mechanics, 25 Sep. Recent Examples on the Web The sparse pockets of space that contain little but cosmic background radiation, leftover energy from the formation of the universe, hover in at around 2.7 kelvin. Consequently, a large enough black holein a hot enough universe experiences a net gain in mass. The meaning of COSMIC BACKGROUND RADIATION is background radiation. The cosmic backgroundradiation left from the Big Bang constantly feeds a black hole with energy.Since a black hole is continually absorbing the cosmic background radiation,it is constantly gaining mass. By radiating particles, theblack hole slowly loses mass until it completely dries up and disappearsin a burst of energy.Ī black hole, however, absorbs all incident radiation. For example, a solar mass blackhole has a temperature of about 6*10^-8 K. Since black holes are extremely massive objects,they radiate at very low temperatures. The black hole radiates as a blackbody with a temperature inverselyproportional to mass. Through the quantum process known as Hawking radiation, black holescan actually lose mass by evaporating one member of a particle-antiparticlepair. How long does it take to reach equilibrium between the opposing powers?A LONG time. Eventually, though, the universe will cool enough such that the blackhole radiates faster than the background radiation can replenish the lostmass. This radiation has since been called the cosmic microwave background (CMB). Cosmic background radiation is constantlyfeeding the black hole lots of energy, steadily giving the black hole moremass. Okay, so black holes radiate out into space and lose mass. The Cosmic Background Radiation Factor Mass In vs. ![]()
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