1. 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

2. Phase diagram

3. Neutron stars

4. 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.

5. Spin-one Color superconductivity

6. 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, (1992)]
In strange quark matter the non-leptonic weak process ( ) dominates [Q. D. Wang and T. Lu, Phys. Lett. 148B, 211 (1984)]

7. 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.

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

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

10. Numerical result for CSL phase
Gapless contribution Ratio~0.034

11. 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.

12. 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

13. Acknowledgement
My advisor Dr. Igor Shokovy

14. Thank you