activity
19961999
most citedThermal Evolution of Compact Stars

98 citations · 400 across the 14 of their papers we have counts for

collaborators

14 papers

astro-ph1999★ 21 cited

Properties of non-rotating and rapidly rotating protoneutron stars

Klaus Strobel, Christoph Schaab, Manfred K. Weigel

Properties of non-rotating and rapidly rotating protoneutron stars and neutron stars are investigated. Protoneutron stars are hot, lepton rich neutron stars which are formed in Typ…

astro-ph1999★ 21 cited

Quasi Periodic Oscillations in Low Mass X-Ray Binaries and Constraints on the Equation of State of Neutron Star Matter

Christoph Schaab, Manfred K. Weigel

Recently discovered quasi periodic oscillations in the X-ray brightness of low mass X-ray binaries are used to derive constraints on the mass of the neutron star component and the…

astro-ph1999★ 15 cited

Impact of internal heating on the thermal evolution of neutron stars

Christoph Schaab, Armen Sedrakian, Fridolin Weber +1

The impact of various competing heating processes on the thermal evolution of neutron stars is investigated. We show that internal heating leads to significantly enhanced surface t…

astro-ph1998★ 41 cited

Implications of Hyperon Pairing for Cooling of Neutron Stars

Christoph Schaab, Shmuel Balberg, Juergen Schaffner-Bielich

The implications of hyperon pairing for the thermal evolution of neutron stars containing hyperons are investigated. The outcome of cooling simulations are compared for neutron sta…

astro-ph1998

Two Dimensional Cooling Simulations of Rotating Neutron Stars

Ch. Schaab, M. K. Weigel

The effect of rotation on the cooling of neutron stars is investigated. The thermal evolution equations are solved in two dimensions with full account of general relativistic effec…

astro-ph1998★ 8 cited

Neutron superfluidity in strongly magnetic interiors of neutron stars and its effect on thermal evolution

Ch. Schaab, F. Weber, M. K. Weigel

The possibility of a neutron m=2-superfluid in the interior of neutron stars is investigated. This pairing state is energetically favoured in strong magnetic fields ($H\sim 10^{16}…