A seismic and gravitationally bound double star observed byKepler
نویسندگان
چکیده
منابع مشابه
Formation of a Gravitationally Bound Object after Binary Neutron Star Merging and GRB970228
The stages that follow the merging of two neutron stars are discussed. It is shown that if a rapidly rotating gravitationally bound object is formed after the merging (a spinar or a massive neutron star), then the characteristic time of its evolution is determined by a fundamental value tspin = 3k mpe 2h̄ mec 5/2G1/2 ≈ 10s · k, where the dimensionless value k = 100 ÷ 1000 depends on the exact eq...
متن کاملFormation of a Gravitationally Bound Object after Binary Neutron Star Merging and GRB phenomena
The stages that follow the merging of two neutron stars are discussed. It is shown that if a rapidly rotating gravitationally bound object is formed after the merging (a spinar or a massive neutron star), then the characteristic time of its evolution is determined by a fundamental value tspin = κ m2pe 2h̄ mec 5/2G1/2 ≈ 7 · 10s · κ , where the dimensionless value κ depends on the exact equation o...
متن کاملGravitationally bound monopoles.
We construct monopole solutions in SU(2) Einstein-Yang-Mills-Higgs theory carrying magnetic charge n. For vanishing and small Higgs self-coupling, these multimonopole solutions are gravitationally bound. Their mass per unit charge is lower than the mass of the n = 1 monopole. For large Higgs self-coupling only a repulsive phase exists.
متن کاملDynamical Tomography of Gravitationally Bound Systems
We study the inverse problem of deducing the dynamical characteristics (such as the potential field) of large systems from kinematic observations. We show that, for a class of steady-state systems, the solution is unique even with fragmentary data, dark matter, or selection (bias) functions. Using spherically symmetric models for simulations, we investigate solution convergence and the roles of...
متن کاملLetter to the Editor Formation of a gravitationally bound object after binary neutron star merging and GRB phenomena
The stages that follow the merging of two neutron stars are discussed. It is shown that if a rapidly rotating gravitationally bound object is formed after the merging (a spinar or a massive neutron star), then the characteristic time of its evolution is determined by a fundamental value tspin = 3k mpe 2h̄ mec 5/2G1/2 ≈ 10s · κ , where the dimensionless value κ = 100 ÷ 1000 depends on the exact e...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2015
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/201526610