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Unveiling the Mysteries of Black Holes: From Formation to Evolution

Explore the genesis, characteristics, and phenomena of black holes, from gas cloud contractions to neutron stars and neutron star collapse into black holes. Learn about event horizons, Hawking radiation, holographic principle, and the incredible information paradox. Dive into the fascinating world of black holes and their enigmatic nature.

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Unveiling the Mysteries of Black Holes: From Formation to Evolution

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  1. The genesisandcharacteristicsofblackholes Marion Mikusch Physicsinstitute, universityof Graz

  2. The contractionof a gas cloud • molecules: do not haveenoughEkin • triggers: compressions • Jeans massand Jeans radius:

  3. A collapsesets in… • contraction Epotisreleased • ifheatistransported off collapse • freefalling time:  protostarisborn

  4. Stage ofnucleosynthesis • Different phases: • hydrogen burning • heliumburning • carbon, neon, oxygen, silicateburning • stageofequilibriumuntilfuelisdepleted •  a newthermonuclearprocessstarts • Stars over 8 sm: also heavy elementsarebuilt • iron-nickelcoreisformed  supernova

  5. The unstoppablecollapse • neutronstar: e+pn • untilinternalpressurepreventscontraction • Star over 30 sm: unstoppablecollapse  a black hole isborn

  6. A black hole swallowseverything… • escapevelocityreachesthespeedoflight • Schwarzschild radius:  causalborder • black hole with 10 sm: Rs = 29,5 km • eventhorizon: surfacearoundtheblack hole

  7. Accretiondiscand matter jets • interstellar matter approches in spiral tracks • X-rayemission • rotation  space-time geometryisdistorted • ‘electromagnetictornado‘

  8. thermodynamicaldescription • analogybetweeneventhorizonandentropy • entropy: disorderofmissinginformation in a system • bitofinformation areaoftheeventhorizon • definitionofentropy andtemperature ispossible

  9. Hawking radiation • paradox: finite temperature emissionof thermal radiation?? • Quantum mechanics: uncertaintyprinciple  virtualparticlescanarise in pairs • theydisengagefor a short time andthanannihilate • massoftheblack hole decreases  total evaporation

  10. holographicprinciple • Only 3 observable characteristics: • mass • angular momentum • electriccharge • hugeinformationloss • but a swallowedbitis ‘saved‘ in an areaoftheeventhorizon  like a hologram • 3-dimensional objectmemorizedby a 2-dimensional region

  11. Thankyouforyourattention!

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