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3.3 Non-singular Cosmological Solutions Starting and Ending with Pure Dark Energy (de Sitter Universe)3.3.1 A Toy Linear Model: Initial Jump in the Density; 3.3.2 General Non-linear Model: Qualitative Picture. Non-singular Cosmologies Represented by Heteroclynic Phase Trajectories; 3.4 Non-singular Cosmologies: Exact Solutions; 3.4.1 General Exact Solution by the Semi
inverse Method; 3.4.2 Particular Non-singular Cosmologies: Examples of Exact Solutions; References; 4 Friedmann Cosmology with Interaction Between Dark Energy and Multi-Phase Matter
Appendix B Two Classes of Non-linear Interaction Laws Allowing for General Explicit Solutions (the Case of a Single Matter Phase)Appendix C Behavior of Non
singular Cosmological Solutions Obtained by the Semi
Inverse Method in the Beginning and at the End of the Expansion (the Case of a Single Matter Phase); References
inverse Method; 3.4.2 Particular Non-singular Cosmologies: Examples of Exact Solutions; References; 4 Friedmann Cosmology with Interaction Between Dark Energy and Multi-Phase Matter
Appendix B Two Classes of Non-linear Interaction Laws Allowing for General Explicit Solutions (the Case of a Single Matter Phase)Appendix C Behavior of Non
singular Cosmological Solutions Obtained by the Semi
Inverse Method in the Beginning and at the End of the Expansion (the Case of a Single Matter Phase); References