Phenomenology of Magnetic Black Holes with
Description: Phenomenology of Magnetic Black Holes with Electroweak-Symmetric Coronas Mrunal Korwar Physics Department, University of Wisconsin-Madison Email:- mkorwarwisc.edu Phenomenology 2021 Symposium 2007.03703 (JHEP 10 (2020) 210) with Yang Bai,
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slide1. Phenomenology of Magnetic Black Holes with Electroweak-Symmetric Coronas Mrunal Korwar
Physics Department, University of Wisconsin-Madison
Email:- mkorwar@wisc.edu
Phenomenology 2021 Symposium 2007.03703 (JHEPÂ 10Â (2020)Â 210) with Yang Bai, Joshua Berger, and Nicholas Orlofsky
2012.15430 (JHEPÂ 04Â (2021)Â 119) with Yang Bai<br>
slide2. Introduction Open Problems in Fundamental Physics:
1) Nature of Dark Matter and Dark Energy
2) Baryogenesis
3) Naturalness/Hierarchy Problem
…..
n) Exotic Objects or states in the SM or BSM
Observational probes for BHs: 2 Magnetic BH with Electroweak- Symmetric Hair (LIGO collaboration, EHT Collaboration)<br>
slide3. 3 Hairy Black Holes (Lee, Nair, E. Weinberg’ 91 (hep-th:9112008))<br>
slide4. Lagrangian:
Ansatz: Spherically symmetric ansatz in hedgehog gauge (Cho & maison’96 (hep-ph:9601028))
Mass: (Lee & E. Weinberg’94 (hep-th:9406021)) 4 Electroweak Monopoles? Hide Singularity behind event horizon of BH Magnetic BH with Electroweak Hair Divergent.
No Finite Energy Electroweak Monopoles in SM<br>
slide5. Action:
Profile of Electroweak hair: 5 Hairy Magnetic Black Holes Q = 2 (Bai & MK, 2012.15430) masses vanish<br>
slide6. Mass and Radius: 6 Higher charged Hairy Magnetic Black Holes (Maldacena, 2004.06084)<br>
slide7. 2-D massless modes: Landau levels in presence of magnetic fields
Hawking Radiation: (Maldacena, 2004.06084) 7 2-D Hawking Radiation Q = 2 For phenomenological purpose BHs can be taken to be extremal.<br>
slide8. Magnetic BHs get accelerated and extract energy from large coherent magnetic fields present in galaxies 8 Parker Limit Q = 2 (Fletcher et al.
Astro-ph/0310258) ( Turner, Parker, Bogdan’1982) (Bai, Berger, MK, Orlofsky; 2007.03703)<br>
slide9. 9 Limits from Sun and Earth (Bai, Berger, MK, Orlofsky; 2007.03703)<br>
slide10. MACRO: Magnetic monopole search
Mica: Track of monopoles in ancient mica
HSC, MACHO/EROS/OGLE, Kepler(K)
Neutron Star: 10 Final Plot (Bai, Berger, MK, Orlofsky; 2007.03703) Here r is ration of total luminosity going to photon luminosity. With r=1 (proton superconductor) and r=104 (pion superconductor).<br>
slide11. New types of Black Holes (Hairy Magnetic BHs) exist in SM + GR, which have Electroweak Symmetric Vacuum around them where the elementary particles are massless.
This BHs hawking radiate efficiently via a new type of 2-D hawking radiation.
Annihilation of such BHs produce neutrinos and heat which can probed using current observations. Also see (Ghosh, Thalapillil, Ullah 2009.03363) and (Diamond, Kaplan 2103.01850) for other interesting constraints. 11 Summary<br>
Physics Department, University of Wisconsin-Madison
Email:- mkorwar@wisc.edu
Phenomenology 2021 Symposium 2007.03703 (JHEPÂ 10Â (2020)Â 210) with Yang Bai, Joshua Berger, and Nicholas Orlofsky
2012.15430 (JHEPÂ 04Â (2021)Â 119) with Yang Bai<br>
slide2. Introduction Open Problems in Fundamental Physics:
1) Nature of Dark Matter and Dark Energy
2) Baryogenesis
3) Naturalness/Hierarchy Problem
…..
n) Exotic Objects or states in the SM or BSM
Observational probes for BHs: 2 Magnetic BH with Electroweak- Symmetric Hair (LIGO collaboration, EHT Collaboration)<br>
slide3. 3 Hairy Black Holes (Lee, Nair, E. Weinberg’ 91 (hep-th:9112008))<br>
slide4. Lagrangian:
Ansatz: Spherically symmetric ansatz in hedgehog gauge (Cho & maison’96 (hep-ph:9601028))
Mass: (Lee & E. Weinberg’94 (hep-th:9406021)) 4 Electroweak Monopoles? Hide Singularity behind event horizon of BH Magnetic BH with Electroweak Hair Divergent.
No Finite Energy Electroweak Monopoles in SM<br>
slide5. Action:
Profile of Electroweak hair: 5 Hairy Magnetic Black Holes Q = 2 (Bai & MK, 2012.15430) masses vanish<br>
slide6. Mass and Radius: 6 Higher charged Hairy Magnetic Black Holes (Maldacena, 2004.06084)<br>
slide7. 2-D massless modes: Landau levels in presence of magnetic fields
Hawking Radiation: (Maldacena, 2004.06084) 7 2-D Hawking Radiation Q = 2 For phenomenological purpose BHs can be taken to be extremal.<br>
slide8. Magnetic BHs get accelerated and extract energy from large coherent magnetic fields present in galaxies 8 Parker Limit Q = 2 (Fletcher et al.
Astro-ph/0310258) ( Turner, Parker, Bogdan’1982) (Bai, Berger, MK, Orlofsky; 2007.03703)<br>
slide9. 9 Limits from Sun and Earth (Bai, Berger, MK, Orlofsky; 2007.03703)<br>
slide10. MACRO: Magnetic monopole search
Mica: Track of monopoles in ancient mica
HSC, MACHO/EROS/OGLE, Kepler(K)
Neutron Star: 10 Final Plot (Bai, Berger, MK, Orlofsky; 2007.03703) Here r is ration of total luminosity going to photon luminosity. With r=1 (proton superconductor) and r=104 (pion superconductor).<br>
slide11. New types of Black Holes (Hairy Magnetic BHs) exist in SM + GR, which have Electroweak Symmetric Vacuum around them where the elementary particles are massless.
This BHs hawking radiate efficiently via a new type of 2-D hawking radiation.
Annihilation of such BHs produce neutrinos and heat which can probed using current observations. Also see (Ghosh, Thalapillil, Ullah 2009.03363) and (Diamond, Kaplan 2103.01850) for other interesting constraints. 11 Summary<br>