Department of Physics, Arizona State University, Tempe, AZ 85287 The rates of non-leptonic weak processes in spin-one color superconducting quark matter Xinyang Wang Department of Physics, Arizona State University, Tempe, AZ 85287 Mazatlan, Mexico, Nov 10, 2009

Phase diagram www.lsbu.ac.uk/water/phase.html

Neutron stars

Dense matter and Color superconductivity The dominant interaction between quarks is the gluon exchange. At sufficiently high density and low temperature, the quarks are weakly interacting. Attraction between quarks lead to the formation of Cooper pairs.

Spin-one Color superconductivity

Viscosities in stars Bulk and shear viscosities determine the damping of gravitational instabilities in stars [N.Andersson, Astrophys. J. 502, 708(1998)] Viscous properties of stellar matter are determined by weak processes [J. Madsen, Phys. Rev. D 46, 3290 (1992)] In strange quark matter the non-leptonic weak process ( ) dominates [Q. D. Wang and T. Lu, Phys. Lett. 148B, 211 (1984)]

Weak process in dense matter Urca process, e.g., (Stellar cooling) Dominant in non-strange quark matter. Non-lepton process Dominant in strange quark matter.

The rate of the weak processes The rate for d-quark production near equilibrium δμ=μs-μd

Rate of non-leptonic processes in spin-1 color-superconducting matter Annihilate Produce

Numerical result for CSL phase Gapless contribution Ratio~0.034

Summary Cold and dense quark matter is a color superconductor which may be found in neutron stars. Weak processes play an important role in neutron stars. The rate of non-leptonic processes in spin-1 color superconducting matters was calculated. The numerical results for the CSL phase have been presented.

Outlook The numerical result for other spin- one phases. Calculation of the bulk viscosity Study of the interplay between Urca and non-leptonic processes in the bulk viscosity

Acknowledgement My advisor Dr. Igor Shokovy

Thank you