![]() Out of 100, my applications with a male name got 7 responses for interview. I'd send it out with my real name, then a few days later (or few days before) with a female name. So I took my CV and changed the name to a female name. It's MUCH better being a woman So I did an experiment, I work in CS and decided to test what the gender bias is. However, the spectra from lower mass Kerr black holes were almost the same as the spectrum from the Schwarzschild black hole of similar mass.29.6K 1.3K sent 100 applications as a man and a woman. The emission rates of protons were also higher in the Kerr black hole. Many oscillations were present in the high-energy end of the spectrum of Kerr black hole in contrast to the smooth variation observed from the same mass Schwarzschild black hole. There were significant differences between the spectrum from a Schwarzschild and maximally Kerr black hole beginning to emit coloured particles. The decay products of directly emitted particles dominated the spectra at lower energies, but the spectra at higher energies were mostly comprised of directly emitted high energetic particles. As the temperature of the black hole was increased, the flux of protons increased. The spectrum of protons from black holes beginning to emit coloured particles did not resemble the spectra of other secondary particles. The elementary particles with high energies in the secondary spectra were predominantly the high energetic particles directly emitted by the black hole. A significant fraction of particles having energies below the black hole temperature was formed by the decay of unstable particles such as quarks, gluons, muons, tau, W ±, Z 0, and Higgs bosons. The spectra consisted of photons, electrons, three types of neutrinos, and protons. ![]() C code BlackHawk was used to simulate the emission spectra. and Planck mass are considered in the present epoch within the context of the Standard Model. Spectra from black holes of masses between ~10 13 g. Secondary spectra from both Schwarzschild and maximally rotating Kerr black holes are investigated. This work investigates the secondary spectra of particle radiation from black holes formed by the decay of directly emitted elementary particles into stable final products. Hawking radiation is the detectable indicator of black hole evaporations. It is tempting to speculate that this might be the reason why the Universe contains so This shows that gravitational collapse converts the baryons and leptons ![]() Of a black hole cannot decrease, there remains a Generalized Second Law:S 1/4A never decreases whereS is the entropy of matter outside black holes andA is the sum of the surface areas of the event horizons. Although these quantum effects violate the classical law that the area of the event horizon Hole and to its eventual disappearance: any primordial black hole of mass less than about 1015 g would have evaporated by now. This thermal emission leads to a slow decrease in the mass of the black Where κ is the surface gravity of the black hole. \frachk2pk » 10 - 6 ( \fracM\odot M )° K\frac^ \circ K However it is shown that quantum mechanical effectsĬause black holes to create and emit particles as if they were hot bodies with temperature In the classical theory black holes can only absorb and not emit particles. This limit is similar to the limits obtained with ground-based gamma-ray observatories. Using the nondetection of PBH candidates, we derive a 99% confidence limit on the PBH evaporation rate in the vicinity of Earth, PPBH < 7.2 × 10³ pc⁻³ yr⁻¹. None of the unassociated point sources with spectra consistent with PBH evaporation show significant proper motion. In this paper, we develop a new algorithm to detect the proper motion of gamma-ray point sources, and apply it to 318 unassociated point sources at a high galactic latitude in the third Fermi-LAT source catalog. They would appear as potentially moving point sources with gamma-ray emission that become spectrally harder and brighter with time until the PBH completely evaporates. These PBHs have a remaining lifetime of months to years at the start of the Fermi mission. We show that, in cases of individual PBHs, the Fermi-LAT is most sensitive to PBHs with temperatures above approximately 16 GeV and masses 6 ×10¹¹ g, which it can detect out to a distance of about 0.03 pc. Previous searches for PBHs have focused on either short-timescale bursts or the contribution of PBHs to the isotropic gamma-ray emission. Although black holes with these masses cannot be formed as a result of stellar evolution, they may have formed in the early universe and are therefore called primordial black holes (PBHs). ![]() Black holes with masses below approximately 10¹⁵ g are expected to emit gamma-rays with energies above a few tens of MeV, which can be detected by the Fermi Large Area Telescope (LAT).
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