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Exploring Extra Spatial Dimensions in Black Hole-Neutron Star Binaries

This study investigates the astrophysical search for extra spatial dimensions in black hole-neutron star binary systems. Emphasizing warped extra-dimensional models, we analyze the evolution, mechanics, and enhanced evaporation rates of black holes and neutron stars within the framework of Randall-Sundrum 2's brane-world scenario. We explore the renowned binary pulsar PSR 1913+16 to extract constraints on the existence of additional dimensions, noting significant findings regarding black hole evaporation and orbital dynamics. Insights from this research aim to further our understanding of gravitational physics and the nature of our universe.

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Exploring Extra Spatial Dimensions in Black Hole-Neutron Star Binaries

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  1. Searching forExtra Spatial Dimensions:A Black Hole-Neutron Star Binary System Michael Kavic (Long Island University-Brooklyn) Pheno 2012 May, 8th 2012 Collaborators: John Simonetti, DjordjeMinic, VipinVijayan & UmairSurani (Virginia Tech) The Astrophysical Journal Letters, Volume 737, Issue 2, article id. L28 (2011).

  2. Outline An astrophysical search • Evolution of a black-hole-neutron-star binary: ~10 micron-scale extra dimension • Ingredients • Enhanced black hole evaporation in warped extra dimensional models (RS 2) • Binary black hole-pulsar systems

  3. Infinitely large “warped” extra dimension Randall-Sundrum 2 (1999) x y bulk brane Our brane --- flat, positive cosmological constant (tension), standard model particles/forces confined to the brane The bulk --- AdS: vacuum, negative cosmological constant, gravity only, “warped” (redshift scaling factor confines gravitons near our brane)

  4. Emparan, Fabbri, Kaloper (2002) Emparan, García-Bellido, Kaloper (2003) Enhanced black hole evaporation rate in RS 2 braneworld, due to a greatly enhanced number of emission modes (L is the length scale of warp) Lifetimes for stellar-mass black holes < age of the universe

  5. The “Binary Pulsar”PSR 1913+16 Weisberg and Taylor 2005 ap sin i= 2.3417725(8) s e = 0.6171338(4) P = 0.322997448930 days (7.75 hours) Mpulsar = 1.4414 +/- 0.0002 M* Mcompanion = 1.3867 +/- 0.0002 M* dP/dt= (1.0013 +/- 0.0021) dP/dtGR

  6. Hadjidemetriou (1963, 1967) Binary systems with isotropic mass loss

  7. The Assembled Ingredients A“Binary Pulsar ballpark” P = 7.75 hours BH mass = 3 M* NS mass = 1.4 M* (KIII)

  8. must satisfy Kepler’s third law at any moment, so…

  9. Precision on orbital perioddetermination for PSR 1913+16 +/- 0.0016 ms y-1 0.40 ms y-1 / 0.0016 ms y-1 = 25 sigma Accepting 3 sigma results for a BH-NS binary system, we could set limits to L ~ 3.5 microns

  10. Thank you!!!!

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