Published July 15, 2011
| Version v1
Journal article
Bulk viscosity coefficients due to phonons and kaons in superfluid color-flavor locked quark matter
Creators
- 1. Department of Astronomy and Astrophysics, Berlin Institute of Technology, Hardenbergstr. 36, D-10623, Berlin (Germany)
- 2. Instituto de Ciencias del Espacio (IEEC/CSIC), Campus Universitat Autonoma de Barcelona, Facultat de Ciencies, Torre C5, E-08193 Bellaterra, Barcelona (Spain)
Description
We evaluate the three bulk viscosity coefficients ζ1, ζ2 and ζ3 in the color-flavor locked superfluid phase due to phonons and kaons, which are the lightest modes in that system. We first show that the computation is rather analogous to the computation of the same coefficients in superfluid 4He, as due to phonons and rotons. For astrophysical applications, we also find the value of the viscosities when there is a periodic disturbance, and the viscosities also depend on the frequency of the disturbance. In a temperature regime that might be of astrophysical relevance, we find that the contributions of both the phonons and kaons should be considered, and that ζ2 is much less that the same coefficient in unpaired quark matter.
Additional details
Identifiers
- DOI
- 10.1103/PhysRevD.84.023004;
- arXiv
- arXiv:1104.5624v2;
Publishing Information
- Journal Title
- Physical Review. D, Particles Fields
- Journal Volume
- 84
- Journal Issue
- 2
- Journal Page Range
- p. 023004-023004.11
- ISSN
- 0556-2821
- CODEN
- PRVDAQ
INIS
- Country of Publication
- United States
- Country of Input or Organization
- International Atomic Energy Agency (IAEA)
- INIS RN
- 43079459
- Subject category
- S72: PHYSICS OF ELEMENTARY PARTICLES AND FIELDS;
- Descriptors DEI
- ASTROPHYSICS; COLOR MODEL; DISTURBANCES; FLAVOR MODEL; HELIUM 4; PHONONS; QUARK MATTER; SUPERFLUIDITY
- Descriptors DEC
- COMPOSITE MODELS; EVEN-EVEN NUCLEI; HELIUM ISOTOPES; ISOTOPES; LIGHT NUCLEI; MATHEMATICAL MODELS; MATTER; NUCLEI; PARTICLE MODELS; PHYSICS; QUARK MODEL; QUASI PARTICLES; STABLE ISOTOPES
Optional Information
- Notes
- (c) 2011 American Institute of Physics