Prashanth Jaikumar California State University Long Beach March 28-29, 2011 ! Collaborators : Brian Niebergal (Scotia Bank), Rachid Ouyed (U.Calgary) 3 rd Mini-Workshop on Neutron Stars and Neutrinos, Arizona State University (Organizers: Cecilia Lunardini and Igor Shovkovy)
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Prashanth Jaikumar California State University Long Beach
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Prashanth Jaikumar
California State University Long Beach
March 28-29, 2011
! Collaborators: Brian Niebergal (Scotia Bank), Rachid Ouyed (U.Calgary)
3rd Mini-Workshop on Neutron Stars and Neutrinos, Arizona State University (Organizers: Cecilia Lunardini and Igor Shovkovy)
Introduction
Part 1: Strange Quark Matter (SQM) • Hypothesis • Strangelets • Neutron Stars vs. Quark Stars
Part 2: Numerical Studies of Combustion • Previous work • Setting up Reactive Diffusive Hydrodynamics • Simulation Results (1D) • Astrophysical implications
Images from http://www.paultan.org
Witten (1984) argued that at high density, bulk SQM can be more stable than nuclear matter
µ(uds) ≈ 0.89µ(ud)
Witten Hypothesis: Quark matter with (u,d,s) may have lower energy/baryon
1. Coulomb energy disfavors very large blobs 2. Surface tension disfavors very small blobs 3. Interactions (α_strong) favor more strange quarks
The estimates are model dependent and fairly simplistic
Berger & Jaffe: PRC 35, 213 (1987)
1. Primordial (Witten): 1st order PT in Early Universe (T ~ 200 MeV) Strangelets formed by freezing of lumps with baryon excess inside
2. Heavy-ion Collisions: Forward rapidity region at RHIC Short lifetime; production rate < 1 in 10^6 collisions for 0.1ns or more (STAR)
3. Binary collision of strange stars (if they exist) can eject strangelets Expected strangelet flux is below current detection limits (1 in 10^14 for A~1000)
April 19, 2011: AMS-02 launched for use at ISS; should find CFL strangelets
Q: Can these 2 classes of stars co-exist?
Answer: Its possible!
Reason 1: Strangelets have some + charge, so repel ordinary nuclei. Quark Star with nuclear crust may exist.
Reason 2: Limits on Strangelet flux from binary SS collisions less than NS-NS collisions (Bauswein, PRL 103, 011101 (2009))